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1. GRANDMA and HXMT Observations of GRB 221009A: The Standard Luminosity Afterglow of a Hyperluminous Gamma-Ray Burst—In Gedenken an David Alexander Kann

Author: D. A. Kann, S. Agayeva, V. Aivazyan, S. Alishov, C. M. Andrade, S. Antier, A. Baransky, P. Bendjoya, Z. Benkhaldoun, S. Beradze, D. Berezin, M. Boër, E. Broens, S. Brunier, M. Bulla, O. Burkhonov, E. Burns, Y. Chen, Y. P. Chen, M. Conti, M. W. Coughlin, W. W. Cui, F. Daigne, B. Delaveau, H. A. R. Devillepoix, T. Dietrich, D. Dornic, F. Dubois, J.-G. Ducoin, E. Durand, P.-A. Duverne, H.-B. Eggenstein, S. Ehgamberdiev, A. Fouad, M. Freeberg, D. Froebrich, M. Y. Ge, S. Gervasoni, V. Godunova, P. Gokuldass, E. Gurbanov, D. W. Han, E. Hasanov, P. Hello, T. Hussenot-Desenonges, R. Inasaridze, A. Iskandar, N. Ismailov, A. Janati, T. Jegou du Laz, S. M. Jia, S. Karpov, A. Kaeouach, R. W. Kiendrebeogo, A. Klotz, R. Kneip, N. Kochiashvili, N. Kunert, A. Lekic, S. Leonini, C. K. Li, W. Li, X. B. Li, J. Y. Liao, L. Logie, F. J. Lu, J. Mao, D. Marchais, R. Ménard, D. Morris, R. Natsvlishvili, V. Nedora, K. Noonan, K. Noysena, N. B. Orange, P. T. H. Pang, H. W. Peng, C. Pellouin, J. Peloton, T. Pradier, O. Pyshna, Y. Rajabov, S. Rau, C. Rinner, J.-P. Rivet, F. D. Romanov, P. Rosi, V. A. Rupchandani, M. Serrau, A. Shokry, A. Simon, K. Smith, O. Sokoliuk, M. Soliman, L. M. Song, A. Takey, Y. Tillayev, L. M. Tinjaca Ramirez, I. Tosta e Melo, D. Turpin, A. de Ugarte Postigo, S. Vanaverbeke, V. Vasylenko, D. Vernet, Z. Vidadi, C. Wang, J. Wang, L. T. Wang, X. F. Wang, S. L. Xiong, Y. P. Xu, W. C. Xue, X. Zeng, S. N. Zhang, H. S. Zhao, and X. F. Zhao
Subjects: Optical astronomy, Optical telescopes, Interstellar dust extinction, Gamma-ray bursters, Astronomy data modeling, Astrophysics, QB460-466
Abstract: Object GRB 221009A is the brightest gamma-ray burst (GRB) detected in more than 50 yr of study. In this paper, we present observations in the X-ray and optical domains obtained by the GRANDMA Collaboration and the Insight Collaboration. We study the optical afterglow with empirical fitting using the GRANDMA+HXMT-LE data sets augmented with data from the literature up to 60 days. We then model numerically using a Bayesian approach, and we find that the GRB afterglow, extinguished by a large dust column, is most likely behind a combination of a large Milky Way dust column and moderate low-metallicity dust in the host galaxy. Using the GRANDMA+HXMT-LE+XRT data set, we find that the simplest model, where the observed afterglow is produced by synchrotron radiation at the forward external shock during the deceleration of a top-hat relativistic jet by a uniform medium, fits the multiwavelength observations only moderately well, with a tension between the observed temporal and spectral evolution. This tension is confirmed when using the augmented data set. We find that the consideration of a jet structure (Gaussian or power law), the inclusion of synchrotron self-Compton emission, or the presence of an underlying supernova do not improve the predictions. Placed in the global context of GRB optical afterglows, we find that the afterglow of GRB 221009A is luminous but not extraordinarily so, highlighting that some aspects of this GRB do not deviate from the global known sample despite its extreme energetics and the peculiar afterglow evolution.
Published: 2023
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2. The 2018 failed outburst of H 1743 – 322: Insight-HXMT, NuSTAR, and NICER views

Author: P J Wang, L D Kong, Y P Chen, S Zhang, S N Zhang, R Soria, L Ji, J L Qu, Y Huang, L Tao, M Y Ge, F J Lu, L Chen, T P Li, Y P Xu, X L Cao, Y Chen, C Z Liu, Q C Bu, C Cai, Z Chang, T X Chen, Y B Chen, W W Cui, Y Y Du, G H Gao, H Gao, Y D Gu, J Guan, C C Guo, D W Han, J Huo, S M Jia, W C Jiang, J Jin, B Li, C K Li, G Li, W Li, X Li, X B Li, X F Li, Z W Li, X H Liang, J Y Liao, B S Liu, H X Liu, H W Liu, X J Liu, X F Lu, Q Luo, T Luo, R C Ma, X Ma, B Meng, Y Nang, J Y Nie, G Ou, X Q Ren, N Sai, L M Song, X Y Song, L Sun, Y Tan, Y L Tuo, C Wang, L J Wang, W S Wang, Y S Wang, X Y Wen, B Y Wu, B B Wu, M Wu, G C Xiao, S Xiao, S L Xiong, R J Yang, S Yang, Yan Ji Yang, Yi Jung Yang, Q B Yi, Q Q Yin, Y You, F Zhang, H M Zhang, J Zhang, P Zhang, W C Zhang, W Zhang, Y F Zhang, Y H Zhang, H S Zhao, X F Zhao, S J Zheng, Y G Zheng, and D K Zhou
Subjects: Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics
Abstract: We studied the 2018 outburst of the black hole transient H 1743 − 322 with a series of Insight-HXMT, NICER, and NuSTAR observations, covering the 1–120 keV band. With our broad-band X-ray spectral modelling, we confirm that the source remained in the low/hard state throughout the month-long outburst, although it became marginally softer at peak flux. We detected Type-C quasi-periodic oscillations (QPOs) and followed the evolution of their properties. The QPO frequency increased from ∼0.1 to ∼0.4 Hz during the rising phase of the outburst and decreased again in the decline. Continuum X-ray flux, power-law photon index, QPO frequency, and QPO root-mean-square amplitude were positively correlated. The QPO amplitude was slightly higher in the soft X-ray band (typical values of 12–16 per cent, compared with 8–10 per cent in the hard band). Our spectral-timing results shed light on the initial rising phase in the low/hard state, which has rarely been monitored with such high cadence, time resolution, and broad-band coverage. Combining spectral and timing properties, we find that ‘failed’ (hard state only) and ‘successful’ outbursts follow the same initial evolutionary track, although the former class of outburst never reaches the threshold for a transition to softer (thermally dominated) accretion regimes.
Published: 2022

3. Physical origin of the non-physical spin evolution of MAXI J1820 + 070

Author: Cunguo Wang, Shaolin Xiong, B. S. Liu, B. B. Wu, H. Gao, J. Y. Liao, H. M. Zhang, R. C. Ma, Y. S. Wang, Y. F. Zhang, Xue-Feng Lu, C. Cai, Lian Tao, Shuinai Zhang, Tong Li, G. H. Gao, S. M. Jia, Tao Luo, M. Wu, X. Y. Song, Bo Li, Wenxiong Li, J. Jin, Xin-Fu Zhao, He-Yang Liu, S. Xiao, Lei Sun, Junqiang Zhang, J. L. Qu, Y. H. Tan, C. K. Li, Y. Nang, Peng Zhang, R. J. Yang, H. W. Liu, N. Sai, Yuan-Yuan Du, Y. G. Zheng, X. X. Li, Z. Chang, Y. B. Chen, Qiu-Yi Luo, Tian-Xiang Chen, Z. W. Li, F. J. Lu, Qingcui Bu, L. M. Song, S. J. Zheng, XiangYang Wen, X. H. Ma, Da-Wei Han, Ya Fang Huang, H. S. Zhao, Yuan You, Qi-Bin Yi, D. K. Zhou, P. J. Wang, W. S. Wang, Ge Ou, Yi Zhang, C. Z. Liu, Sisi Yang, J. Y. Nie, Xin Ren, Liang Zhang, Cheng-Cheng Guo, Ming-Yu Ge, L. Chen, Wan-Chang Zhang, Xiong Li, Yu-Dong Gu, X. J. Liu, Libin Wang, X. L. Cao, Q. Q. Yin, Y. P. Chen, Y. Wang, X. H. Liang, Fuqin Zhang, S. N. Zhang, Y. P. Xu, B. Y. Wu, Xuelong Li, J. Guan, L. D. Kong, Wei Cui, W. C. Zhang, Jia Huo, Gang Li, Wenhan Jiang, Bin Meng, Y. J. Yang, and G. C. Xiao
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Hardness ratio, Astrophysics::High Energy Astrophysical Phenomena, Spin transition, FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Astrophysics, Black hole, Innermost stable circular orbit, Accretion disc, Space and Planetary Science, Coincident, Spectral analysis, 83C57, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: We report on the Insight-HXMT observations of the new black hole X-ray binary MAXI J1820+070 during its 2018 outburst. Detailed spectral analysis via the continuum fitting method shows an evolution of the inferred spin during its high soft sate. Moreover, the hardness ratio, the non-thermal luminosity and the reflection fraction also undergo an evolution, exactly coincident to the period when the inferred spin transition takes place. The unphysical evolution of the spin is attributed to the evolution of the inner disc, which is caused by the collapse of a hot corona due to condensation mechanism or may be related to the deceleration of a jet-like corona. The studies of the inner disc radius and the relation between the disc luminosity and the inner disc radius suggest that, only at a particular epoch, did the inner edge of the disc reach the innermost stable circular orbit and the spin measurement is reliable. We then constrain the spin of MAXI J1820+070 to be a*=0.2^{+0.2}_{-0.3}. Such a slowly spinning black hole possessing a strong jet suggests that its jet activity is driven mainly by the accretion disc rather than by the black hole spin., Comment: 14 pages, 13 figures, 5 tables, accepted for publication in MNRAS
Published: 2021

4. [A case of Pfeiffer syndrome caused by FGFR2 gene variation]

Author: X R, Zhuang and H S, Zhao
Subjects: Male, Child, Preschool, Mutation, Infant, Newborn, Mutation, Missense, Exophthalmos, Humans, Acrocephalosyndactylia, Receptor, Fibroblast Growth Factor, Type 2, Child
Abstract: A 29-month-old male child with FGFR2 heterozygous missense mutation at birth was diagnosed as Pfeiffer syndrome. He was treating for binocular exophthalmos and exposed keratitis in Beijing Tongren Hospital Affiliated to Capital Medical University. The child had skull fusion (clover head), obvious exophthalmos, deformity of fingers and toes, ankylosis of elbow joint or bony fusion, accompanied by neurological complications and growth retardation; FGFR2 (NM_001144916) gene c.679TG (thymineguanine) and p.c227gG(cysteineglycine) heterozygous missense mutations were found in the the child, and his parents did not carry the same mutation. Pfeiffer syndrome type Ⅱ was diagnosed. Permanent adhesion of eyelid margin was performed under general anesthesia, and the postoperative condition was stable.2岁5个月男性患儿出生时在外院发现FGFR2杂合错义突变，诊断为Pfeiffer综合征。现因双眼眼球突出、暴露性角膜炎于首都医科大学附属北京同仁医院就诊。患儿表现为颅骨融合（三叶草样头颅），眼球突出明显，手指及脚趾畸形，肘关节强直或骨性融合，并伴有神经系统并发症及发育迟缓；患儿FGFR2（NM_001144916）基因c.679TG（胸腺嘧啶鸟嘌呤）、p.C227G（半胱氨酸甘氨酸）杂合错义突变，其父母均未携带相同突变。综合临床表现及基因检测诊断为Pfeiffer综合征Ⅱ型。于全身麻醉下行双眼睑缘永久粘连术，术后病情稳定。.
Published: 2022

5. HXMT identification of a non-thermal X-ray burst from SGR J1935+2154 and with FRB 200428

Author: Y. J. Jin, Z. Chang, J. Y. Liao, H. M. Zhang, Y. F. Zhang, X. B. Li, Y. G. Li, Chun-sheng Zhang, Wenhan Jiang, Bo Li, Yu-Xuan Zhu, G. H. Gao, J. Jin, M. Wu, Y. Zhang, Xin-Fu Zhao, Zhi Zhang, Y. H. Tan, Y. X. Zhu, R. C. Shang, C. Cai, B. Lu, Fuqin Zhang, J. K. Deng, S. N. Zhang, W. C. Xue, X. X. Li, Y. G. Zheng, J. F. Zhou, Ming-Yu Ge, X. H. Ma, Wenxiong Li, Tian-Xiang Chen, F. J. Lu, Y. S. Wang, D. K. Zhou, Wei Cui, T. Zhang, Aimei Zhang, Lin Lin, Li-Ming Song, B. S. Liu, Lei Sun, C. Z. Liu, S. J. Zheng, Luhua Jiang, Y. P. Xu, B. B. Wu, X. L. Cao, Tao Luo, XiangYang Wen, Xue-Feng Lu, Bin Meng, S. Xiao, Y. B. Chen, Junqiang Zhang, Tong Li, H. W. Liu, N. Sai, Mao-Shun Li, Yunchao Liu, Sisi Yang, Y. J. Yang, S. M. Jia, Yuan You, L. D. Kong, Songbo Zhang, Cunguo Wang, Qi-Bin Yi, Yu-Dong Gu, Q. Q. Yin, Y. P. Chen, Xuelong Li, J. Guan, X. J. Liu, W. Z. Zhang, Yuan-Yuan Du, Gang Chen, X. H. Liang, G. C. Xiao, R. L. Zhuang, GuoQing Liu, Jia Huo, Y. Nang, Gang Li, Shaolin Xiong, Y. J. Zhang, H. Gao, Qiu-Yi Luo, Z. Zhang, Y. L. Tuo, J. W. Yang, Bing Zhang, B. Y. Wu, Lian Tao, X. Y. Song, H. S. Zhao, G. F. Wang, W. S. Wang, Ge Ou, W. C. Zhang, J. Y. Nie, Yi-Qiao Dong, Cheng-Cheng Guo, C. K. Li, H. Xu, Z. W. Li, Da-Wei Han, Z. L. Zhang, M. X. Fu, Yue Zhang, Ya Fang Huang, J. Z. Wang, L. Chen, Wan-Chang Zhang, Weiguang Cui, Qingcui Bu, Min Gao, and J. L. Qu
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010504 meteorology & atmospheric sciences, X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Magnetar, 01 natural sciences, Coincidence, Radio spectrum, 0103 physical sciences, Thermal, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Event (particle physics), 0105 earth and related environmental sciences, Delay time
Abstract: Fast radio bursts (FRBs) are short pulses observed in radio band from cosmological distances. One class of models invoke soft gamma-ray repeaters (SGRs), or magnetars, as the sources of FRBs. Some radio pulses have been observed from some magnetars, however, no FRB-like events had been detected in association any magnetar burst, including one giant flare. Recently, a pair of FRB-like bursts (FRB 200428 hereafter) separated by milliseconds (ms) were detected from the general direction of the Galactic magnetar SGR J1935+2154. Here we report the detection of a non-thermal X-ray burst in the 1-250 keV energy band with the Insight-HXMT satellite, which we identify as emitted from SGR J1935+2154. The burst showed two hard peaks with a separation of 34 ms, broadly consistent with that of the two bursts in FRB 200428. The delay time between the double radio and X-ray peaks is about 8.57 s, fully consistent with the dispersion delay of FRB 200428. We thus identify the non-thermal X-ray burst is associated with FRB 200428 whose high energy counterpart is the two hard peaks in X-ray. Our results suggest that the non-thermal X-ray burst and FRB 200428 share the same physical origin in an explosive event from SGR J1935+2154., 24 pages, 9 figures, 6 tables; initial submission to a journal on May 9th, 2020. Significant changes include updated localization and detailed spectral evolution of the X-ray burst, and better determination of the two narrow X-ray peaks corresponding to the two radio pulses. Conclusions are strengthened. Nature Astronomy online on Feb. 18, 2021
Published: 2021

6. Peculiar disk behaviors of the black hole candidate MAXI J1348-630 in the hard state observed by Insight-HXMT and Swift

Author: W. Zhang, L. Tao, R. Soria, J. L. Qu, S. N. Zhang, S. S. Weng, L. Zhang, Y. N. Wang, Y. Huang, R. C. Ma, S. Zhang, M. Y. Ge, L. M. Song, X. Ma, Q. C. Bu, C. Cai, X. L. Cao, Z. Chang, L. Chen, T. X. Chen, Y. B. Chen, Y. Chen, Y. P. Chen, W. W. Cui, Y. Y. Du, G. H. Gao, H. Gao, Y. D. Gu, J. Guan, C. C. Guo, D. W. Han, J. Huo, S. M. Jia, W. C. Jiang, J. Jin, L. D. Kong, B. Li, C. K. Li, G. Li, T. P. Li, W. Li, X. Li, X. B. Li, X. F. Li, Z. W. Li, X. H. Liang, J. Y. Liao, B. S. Liu, C. Z. Liu, H. X. Liu, H. W. Liu, X. J. Liu, F. J. Lu, X. F. Lu, Q. Luo, T. Luo, B. Meng, Y. Nang, J. Y. Nie, G. Ou, X. Q. Ren, N. Sai, X. Y. Song, L. Sun, Y. Tan, Y. L. Tuo, C. Wang, L. J. Wang, P. J. Wang, W. S. Wang, Y. S. Wang, X. Y. Wen, B. Y. Wu, B. B. Wu, M. Wu, G. C. Xiao, S. Xiao, S. L. Xiong, R. J. Yang, S. Yang, Y. J. Yang, Y. R. Yang, Q. B. Yi, Q. Q. Yin, Y. Yuan, F. Zhang, H. M. Zhang, P. Zhang, W. C. Zhang, Y. F. Zhang, Y. H. Zhang, H. S. Zhao, X. F. Zhao, S. J. Zheng, Y. G. Zheng, and D. K. Zhou
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present a spectral study of the black hole candidate MAXI J1348-630 during its 2019 outburst, based on monitoring observations with Insight-HXMT and Swift. Throughout the outburst, the spectra are well fitted with power-law plus disk-blackbody components. In the soft-intermediate and soft states, we observed the canonical relation L ~ T_in^4 between disk luminosity L and peak colour temperature T_in, with a constant inner radius R_in (traditionally identified with the innermost stable circular orbit). At other stages of the outburst cycle, the behaviour is more unusual, inconsistent with the canonical outburst evolution of black hole transients. In particular, during the hard rise, the apparent inner radius is smaller than in the soft state (and increasing), and the peak colour temperature is higher (and decreasing). This anomalous behaviour is found even when we model the spectra with self-consistent Comptonization models, which take into account the up-scattering of photons from the disk component into the power-law component. To explain both those anomalous trends at the same time, we suggest that the hardening factor for the inner disk emission was larger than the canonical value of ~1.7 at the beginning of the outburst. A more physical trend of radii and temperature evolution requires a hardening factor evolving from ~3.5 at the beginning of the hard state to ~1.7 in the hard intermediate state. This could be evidence that the inner disk was in the process of condensing from the hot, optically thin medium and had not yet reached a sufficiently high optical depth for its emission spectrum to be described by the standard optically-thick disk solution., 20 pages, 10 figures, 4 tables, accepted by ApJ
Published: 2022

7. Evolution of Accretion Modes between Spectral States Inferred from Spectral and Timing Analysis of Cygnus X-1 with Insight-HXMT observations

Author: M. Z. Feng, L. D. Kong, P. J. Wang, S. N. Zhang, H. X. Liu, Z. X. Yang, Y. Huang, L. Ji, S. M. Jia, X. Ma, W. Yu, H. S. Zhao, J. Y. Nie, Y. L. Tuo, S. Zhang, J. L. Qu, and B. B. Wu
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: We execute a detailed spectral-timing study of Cygnus X-1 in the low/hard, intermediate and high/soft states with the Hard X-ray Modulation Telescope observations. The broad band energy spectra fit well with the "truncated disk model" with the inner boundary of the accretion disk stays within $\sim$10 \textit R$_{\rm g}$ and moves inward as the source softens. Through studying of PDS, rms and Fourier-frequency component resolved spectroscopy, we find that the X-ray variations are generated in two different regions for each state. We discover that the major role that contributes to the X-ray variation is the hot corona rather than the accretion disk. We suggest a scenario with different corona geometry for each state based on the truncated disk geometry in which the corona wraps up the disk to form a sandwich geometry in the low/hard state, and then gradually moves away from the disk in direction that is perpendicular to the disk until forming a jet-like geometry in the high/soft state., 13 pages, 12 figures, and 3 tables, accepted for publication in ApJ
Published: 2022

8. The observation of the South Atlantic Anomaly with the particle monitors onboard Insight-HXMT

Author: Junqiang Zhang, J. Y. Liao, Xiang Li, F. J. Lu, Y. B. Chen, L. M. Song, Y. P. Xu, J. L. Qu, S. N. Zhang, X. L. Cao, C. Z. Liu, Tong Li, and H. S. Zhao
Subjects: 010308 nuclear & particles physics, Astronomy and Astrophysics, Geodesy, 01 natural sciences, Charged particle, Latitude, South Atlantic Anomaly, Secular variation, Earth's magnetic field, Space and Planetary Science, 0103 physical sciences, Particle, Stochastic drift, Longitude, 010303 astronomy & astrophysics, Geology
Abstract: The South Atlantic Anomaly (SAA) is a region of weakened geomagnetic field and in the previous studies, it shows a secular variation with time which is associated with the changing of the magnetic moment. This region also consists of large amounts of energetic charged particles and is danger to space vehicle and astronauts. Thus, it is essential to know the location and movement of the SAA. In this study, three particle monitors onboard Insight-HXMT are used to track the movement and location of the SAA from 2017 June 19 to 2019 June 19. Several particle flux maps are built to show the location of the SAA peak with time. In a grid of map, the particle count is determined by the maximum count rate and the averaged count rate, respectively. We find the results of both methods are consistent very well with each other in deriving the drift rate. The result shows the SAA peak moves westwards with an average drift rate of 0.43 ± 0.01 o /yr in longitude and moves northwards with an average drift rate of 0.17 ± 0.01 o /yr in latitude, and the drift rate is slightly larger than the result from IGRF 12 ( 0.3 o /yr) in longitude, but in latitude, the result of IGRF 12 have no obvious change with time.
Published: 2020

9. Insight-HXMT study of the timing properties of Sco X-1

Author: J. Z. Wang, J. Y. Nie, Y. J. Yang, Xiaobo Li, Weiguang Cui, J. Guan, Qingcui Bu, L. M. Song, Yu-Dong Gu, G. C. Xiao, Luhua Jiang, J. Jin, D. K. Zhou, Y. X. Zhu, X. H. Liang, W. C. Zhang, B. Lu, GuoQing Liu, Ming-Yu Ge, Chun-sheng Zhang, Yi-Qiao Dong, Min Gao, B. B. Wu, Wenhan Jiang, Jia Huo, Y. H. Tan, Cheng-Cheng Guo, J. L. Qu, Gang Li, Y. B. Chen, F. J. Lu, Xin-Fu Zhao, R. C. Shang, J. F. Zhou, Bing Li, XiangYang Wen, Lian Tao, Y. S. Wang, Gang Chen, Wei Cui, B. Y. Wu, Tian-Xiang Chen, T. Zhang, X. Y. Song, X. J. Liu, Tao Luo, Da-Wei Han, Bin Meng, L. Chen, Mao-Shun Li, S. Xiao, Xue-Feng Lu, Tong Li, S. M. Jia, Fuqin Zhang, Z. Zhang, S. N. Zhang, Z. Chang, Yunchao Liu, R. L. Zhuang, Junqiang Zhang, Wan-Chang Zhang, W. S. Wang, Y. Nang, Ge Ou, Yuan-Yuan Du, W. Z. Zhang, Lei Sun, Y. J. Jin, C. Z. Liu, J. K. Deng, L. D. Kong, H. W. Liu, N. Sai, Shaolin Xiong, Cunguo Wang, Y. J. Zhang, X. H. Ma, H. Gao, Sisi Yang, Yupeng Xu, Qiu-Yi Luo, X. F. Li, H. S. Zhao, G. F. Wang, Y. L. Tuo, C. Cai, Wenxiong Li, J. W. Yang, Yu-Xuan Zhu, X. L. Cao, X. X. Li, S. J. Zheng, Yuan You, G. H. Gao, Qi-Bin Yi, M. Wu, Q. Q. Yin, Y. P. Chen, Y. Zhang, Y. G. Li, Aimei Zhang, J. Y. Liao, H. M. Zhang, Y. F. Zhang, Ya Fang Huang, Z. L. Zhang, C. K. Li, Z. W. Li, and M. X. Fu
Subjects: Physics, High energy, 010308 nuclear & particles physics, Phase (waves), Astronomy and Astrophysics, Astrophysics, Horizontal branch, 01 natural sciences, law.invention, Telescope, Root mean square, Space and Planetary Science, law, 0103 physical sciences, Modulation (music), 010303 astronomy & astrophysics, Energy (signal processing), Flare
Abstract: We present a detailed timing study of the brightest persistent X-ray source Sco X-1 using the data collected by the Hard X-ray Modulation Telescope ( I n s i g h t -HXMT) from July 2017 to August 2018. A complete Z-track hardness-intensity diagram (HID) is obtained. The normal branch oscillations (NBOs) at ∼ 6 Hz in the lower part of the normal branch (NB) and the flare branch oscillations (FBOs) at ∼ 16 Hz in the beginning part of the flaring branch (FB) are found in observations with the Low Energy X-ray Telescope (LE) and the Medium Energy X-ray Telescope (ME) of I n s i g h t -HXMT, while the horizontal branch oscillations (HBOs) at ∼ 40 Hz and the kilohertz quasi-periodic oscillations (kHz QPOs) at ∼ 800 Hz are found simultaneously above 20 keV for the first time on the horizontal branch (HB) by the High Energy X-ray Telescope (HE) and ME. We find that for all types of the observed QPOs, the centroid frequencies are independent of energy, while the root mean square (rms) increases with energy; the centroid frequencies of both the HBOs and kHz QPOs increase along the Z-track from the top to the bottom of the HB; and the NBOs show soft phase lags increasing with energy. A continuous QPO transition from the FB to NB in ∼ 200 s are also detected. Our results indicate that the non-thermal emission is the origin of all types of QPOs, the innermost region of the accretion disk is non-thermal in nature, and the corona is nonhomogeneous geometrically.
Published: 2020

10. Insight-HXMT observation on 4U 1608–52: Evolving spectral properties of a bright type-I X-ray burst

Author: S. N. Zhang, W. C. Jiang, W. S. Wang, Ge Ou, Z. Chang, J. F. Zhou, X.Q. Ren, C. Z. Liu, C. L. Zhang, Tian-Xiang Chen, Min Gao, H. S. Zhao, Sisi Yang, G. F. Wang, D. K. Zhou, Yi Zhang, X. J. Liu, J. L. Qu, G. C. Xiao, Jia Huo, Z. L. Zhang, Y. G. Li, M. X. Fu, Ya Fang Huang, Bing Li, F. Zhang, Chun-sheng Zhang, X. F. Li, Aimei Zhang, W. Z. Zhang, J. Z. Wang, Liang Sun, Y. B. Chen, Xue-Feng Lu, F. J. Lu, S. M. Jia, XiangYang Wen, Lian Tao, Yuan You, Junke Zhang, Gang Li, Y. S. Wang, Wei Zhang, B. Y. Wu, Qi-Bin Yi, B. B. Wu, Mao-Shun Li, Yunchao Liu, Y. J. Yang, Tao Luo, Xiaobo Li, L. D. Kong, S. Xiao, Yi-Qiao Dong, X. L. Cao, W. C. Zhang, Q. Luo, Weiguang Cui, X. X. Li, Yuan-Yuan Du, J. Y. Liao, H. M. Zhang, Gang Chen, Qingcui Bu, B. Lu, Y. H. Tan, J. K. Deng, Cheng-Cheng Guo, H. W. Liu, N. Sai, Q. Q. Yin, Y. P. Chen, Y. F. Zhang, C. K. Li, L. M. Song, Yu-Dong Gu, J. Jin, G. H. Gao, Xin-Fu Zhao, S. J. Zheng, Y. X. Zhu, C. Cai, Z. W. Li, Zhi-Xiang Zhang, X. H. Ma, Ming-Yu Ge, M. Wu, Y. Zhang, C. Wang, Wenxiong Li, Andrea Santangelo, Yu-Xuan Zhu, Shaolin Xiong, Luhua Jiang, Y. P. Xu, Y. J. Zhang, H. Gao, X. H. Liang, J. Guan, Ti-Pei Li, Y. L. Tuo, J. W. Yang, GuoQing Liu, Wei Cui, Long Ji, T. Zhang, L. Chen, J. Y. Nie, Da-Wei Han, Bin Meng, and Y. Nang
Subjects: Physics, Thermonuclear fusion, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Spectral properties, X-ray, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radius, Astrophysics, 01 natural sciences, symbols.namesake, Neutron star, Space and Planetary Science, 0103 physical sciences, Eddington luminosity, Reflection (physics), symbols, Spectral analysis, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The evidences for the influence of thermonuclear (type-I) X-ray bursts upon the surrounding environments in neutron star low-mass X-ray binaries (LMXB) were detected previously via spectral and timing analyses. Benefitting from a broad energy coverage of Insight-HXMT, we analyze one photospheric radius expansion (PRE) burst, and find an emission excess at soft X-rays. Our spectral analysis shows that, such an excess is not likely relevant to the disk reflection induced by the burst emission and can be attributed to an enhanced pre-burst/persistent emission. We find that the burst and enhanced persistent emissions sum up to exceed Eddington luminosity by ∼ 40 percentages. We speculate that the enhanced emission is from a region beyond the PRE radius, or through the Comptonization of the corona.
Published: 2019

11. Search for Gamma-Ray Bursts and Gravitational Wave Electromagnetic Counterparts with High Energy X-ray Telescope of \textit{Insight}-HXMT

Author: Yu-Dong Gu, C. K. Li, C. Cai, J. Y. Zhang, Wenxiong Li, Y. Nang, Z. Chang, Yuan-Yuan Du, Z. W. Li, B. Y. Wu, B. B. Wu, Wenhan Jiang, J. Y. Nie, Jia Huo, B. S. Liu, L. D. Kong, F. J. Lu, Y. B. Chen, X. Q. Ren, Yuyang Zhao, Fuqin Zhang, S. N. Zhang, X. X. Li, XiangYang Wen, Lian Tao, Peng Zhang, Gang Li, S. J. Zheng, Bo Li, D. K. Zhou, X. Y. Song, Y. G. Zheng, Y. S. Wang, Tian-Xiang Chen, X. J. Liu, Wei Zhang, Cunguo Wang, Cheng-Cheng Guo, Libin Wang, Yuan You, Qi-Bin Yi, W. C. Zhang, G. H. Gao, Lei Sun, Ya Fang Huang, Y. H. Tan, Wei Cui, M. Wu, Wei Chen, L. Chen, Yi-Yan Yang, Y. H. Zhang, Ming-Yu Ge, H. W. Liu, N. Sai, J. Y. Liao, X. H. Liang, H. M. Zhang, R. C. Ma, Y. P. Xu, Y. F. Zhang, X. B. Li, Xuelong Li, J. Guan, Qingcui Bu, X J Yang, L. M. Song, Tao Luo, S. Xiao, Da-Wei Han, J. L. Qu, Hongfei Liu, X. L. Cao, Q. Q. Yin, Y. P. Chen, J. Jin, Yu-Xuan Zhu, Xin-Fu Zhao, C. Z. Liu, Sisi Yang, R. J. Yang, Qiu-Yi Luo, Y. L. Tuo, Bin Meng, Z. Zhang, Shaolin Xiong, H. Gao, Y. J. Yang, G. C. Xiao, H. S. Zhao, P. J. Wang, W. S. Wang, Ge Ou, X. H. Ma, Xue-Feng Lu, Shuinai Zhang, Tong Li, and S. M. Jia
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Gravitational wave, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, X-ray telescope, Astrophysics, Light curve, Coincidence, law.invention, Telescope, Space and Planetary Science, law, Sensitivity (control systems), Gamma-ray burst, Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract: The High Energy X-ray telescope (HE) on-board the Hard X-ray Modulation Telescope (\textit{Insight}-HXMT) can serve as a wide Field of View (FOV) gamma-ray monitor with high time resolution ($\mu$s) and large effective area (up to thousands cm$^2$). We developed a pipeline to search for Gamma-Ray Bursts (GRBs), using the traditional signal-to-noise ratio (SNR) method for blind search and the coherent search method for targeted search. By taking into account the location and spectrum of the burst and the detector response, the targeted coherent search is more powerful to unveil weak and sub-threshold bursts, especially those in temporal coincidence with Gravitational Wave (GW) events. Based on the original method in literature, we further improved the coherent search to filter out false triggers caused by spikes in light curves, which are commonly seen in gamma-ray instruments (e.g. \textit{Fermi}/GBM, \textit{POLAR}). We show that our improved targeted coherent search method could eliminate almost all false triggers caused by spikes. Based on the first two years of \textit{Insight}-HXMT/HE data, our targeted search recovered 40 GRBs, which were detected by either \textit{Swift}/BAT or \textit{Fermi}/GBM but too weak to be found in our blind search. With this coherent search pipeline, the GRB detection sensitivity of \textit{Insight}-HXMT/HE is increased to about 1.5E-08 erg/cm$^2$ (200 keV$-$3 MeV). We also used this targeted coherent method to search \textit{Insight}-HXMT/HE data for electromagnetic (EM) counterparts of LIGO-Virgo GW events (including O2 and O3a runs). However, we did not find any significant burst associated with GW events., Comment: 12 pages, 14 figures, 5 tables; accepted for publication in MNRAS
Published: 2021

12. Broadband variability study of MAXI J1631-479 in its Hard-Intermediate State observed with Insight-HXMT

Author: B. B. Wu, J. Y. Liao, H. M. Zhang, R. C. Ma, Xue-Feng Lu, Tong Li, S. M. Jia, X. L. Cao, Y. F. Zhang, X. B. Li, Tian-Xiang Chen, C. Cai, Bin Meng, W. C. Zhang, Y. B. Chen, C. Z. Liu, X. H. Liang, Qiu-Yi Luo, Y. Nang, Ya Fang Huang, Wenxiong Li, L. Zhang, L. Sun, Y. J. Yang, Sisi Yang, Andrea Santangelo, G. C. Xiao, Y. P. Xu, Y. L. Tuo, D. K. Zhou, Cheng-Cheng Guo, G. H. Gao, X. J. Liu, M. Wu, C. K. Li, Bo Li, Qingcui Bu, T. M. Belloni, L. M. Song, Libin Wang, Peng Zhang, Tao Luo, S. Xiao, Fuqin Zhang, Y. H. Zhang, Shaolin Xiong, S. N. Zhang, Z. W. Li, X. B. Ma, H. Gao, Y. S. Wang, Q. Q. Yin, Y. P. Chen, Y. H. Tan, J. Jin, Xin-Fu Zhao, L. D. Kong, Lian Tao, G. Li, X. Y. Song, J. Y. Nie, Cunguo Wang, Da-Wei Han, X. X. Li, Xuelong Li, J. Guan, H. W. Liu, N. Sai, Wenhan Jiang, S. J. Zheng, J. L. Qu, Hongfei Liu, Z. Chang, Yuan You, Qi-Bin Yi, J. Y. Zhang, Jia Huo, Wei Cui, F. J. Lu, Yu-Dong Gu, XiangYang Wen, Ming-Yu Ge, H. S. Zhao, Z. S. Li, P. J. Wang, B. Y. Wu, W. Zhang, L. Chen, W. S. Wang, Ge Ou, and Yuan-Yuan Du
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Jet (fluid), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Plasma, Astrophysics, Photon energy, law.invention, Telescope, Acceleration, Space and Planetary Science, Modulation, law, Precession, Astrophysics - High Energy Astrophysical Phenomena, Noise (radio)
Abstract: We report the energy-resolved broadband timing analysis of the black hole X-ray transient MAXI J1631-479 during its 2019 outburst from February 11 to April 9, using data from the Insight-Hard X-ray Modulation Telescope (Insight-HXMT), which caught the source from its hard intermediate state to the soft state. Thanks to the large effective area of Insight-HXMT at high energies, we are able to present the energy dependence of fast variability up to ~100 keV. Type-C quasi-periodic oscillations (QPOs) with frequency varying between 4.9 Hz and 6.5 Hz are observed in the 1-100 keV energy band. While the QPO fractional rms increases with photon energy from 1 keV to ~10 keV and remains more or less constant from ~10 keV to ~100 keV, the rms of the flat-top noise first increases from 1 keV to ~8 keV then drops to less than 0.1% above ~30 keV. We suggest that the disappearance of the broadband variability above 30 keV could be caused by the non-thermal acceleration in the Comptonizing plasma. At the same time, the QPOs could be produced by the precession of either a small-scale jet or a hot inner flow model., To be published in The Astrophysical Journal
Published: 2021

13. QPOs and Orbital elements of X-ray binary 4U 0115+63 during the 2017 outburst observed by Insight-HXMT

Author: Q Lou, Yuan You, Qi-Bin Yi, X. X. Li, S. J. Zheng, Cunguo Wang, J. Jin, H M Zhang, Xin-Fu Zhao, H. S. Zhao, Lei Sun, Wenhan Jiang, G. H. Gao, He-Yang Liu, Y. J. Yang, Xiong Li, Yu-Dong Gu, B. S. Liu, X. H. Ma, Y. P. Xu, Yi Zhang, Y. H. Tan, H. W. Liu, Y Z Ding, N. Sai, M. Wu, G. C. Xiao, W. C. Zhang, Yuan-Yuan Du, Y. G. Zheng, Y. Nang, C. Cai, L. Chen, C. Z. Liu, P. J. Wang, F. J. Lu, J. L. Qu, Bin Meng, Xue-Feng Lu, XiangYang Wen, L. D. Kong, Xuelong Li, J. Guan, S. M. Jia, Wenxiong Li, P Zhang, Fuqin Zhang, S. N. Zhang, Tian-Xiang Chen, Sisi Yang, X. L. Cao, C. K. Li, Y. B. Chen, D. K. Zhou, Y. S. Wang, Libin Wang, J. Y. Liao, Q. Q. Yin, Y. P. Chen, Lian Tao, Ti-Pei Li, R. C. Ma, Y. F. Zhang, Qingcui Bu, Bo Li, B. B. Wu, X. Y. Song, Shuang-Nan Zhang, Junqiang Zhang, W. S. Wang, L. M. Song, Wei Cui, Z. W. Li, Ming-Yu Ge, Wei Wang, Tao Luo, S. Xiao, Xin Ren, Ya Fang Huang, X. J. Liu, Jia Huo, C Zhi, Gang Li, B. Y. Wu, Shaolin Xiong, H. Gao, X. H. Liang, Y. L. Tuo, R. J. Yang, Wei Zhang, Cheng-Cheng Guo, Da-Wei Han, and J. Y. Nie
Subjects: Physics, Orbital elements, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Light curve, 01 natural sciences, Spectral line, Luminosity, Neutron star, Wavelet, Space and Planetary Science, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Energy (signal processing)
Abstract: In this paper, we presented a detailed timing analysis of a prominent outburst of 4U 0115+63 detected by \textit{Insight}-HXMT in 2017 August. The spin period of the neutron star was determined to be $3.61398\pm 0.00002$ s at MJD 57978. We measured the period variability and extract the orbital elements of the binary system. The angle of periastron evolved with a rate of $0.048\pm0.003$ $yr^{-1}$. The light curves are folded to sketch the pulse profiles in different energy ranges. A multi-peak structure in 1-10 keV is clearly illustrated. We introduced wavelet analysis into our data analysis procedures to study QPO signals and perform a detailed wavelet analysis in many different energy ranges. Through the wavelet spectra, we report the discovery of a QPO at the frequency $\sim 10$ mHz. In addition, the X-ray light curves showed multiple QPOs in the period of $\sim 16-32 $ s and $\sim 67- 200 $ s. We found that the $\sim100$ s QPO was significant in most of the observations and energies. There exist positive relations between X-ray luminosity and their Q-factors and S-factors, while the QPO periods have no correlation with X-ray luminosity. In wavelet phase maps, we found that the pulse phase of $\sim 67- 200 $ s QPO drifting frequently while the $\sim 16-32 $ s QPO scarcely drifting. The dissipation of oscillations from high energy to low energy was also observed. These features of QPOs in 4U 0115+63 provide new challenge to our understanding of their physical origins., 14 pages, 9 figures, and 6 tables. This work has been submitted to MNRAS after the referee's report
Published: 2021

14. Insight-HXMT observations of Swift J0243.6+6124: the evolution of RMS pulse fractions at super-Eddington luminosity

Author: Da-Wei Han, Luhua Jiang, Y. P. Xu, C. Cai, X. F. Li, Zhi Zhang, Mao-Shun Li, M. X. Fu, C. K. Li, Wenxiong Li, B. S. Liu, Wenhan Jiang, J. Z. Wang, X. H. Liang, Bing Li, Tao Luo, Y. B. Chen, B. Y. Wu, Weiguang Cui, S. Xiao, Qingcui Bu, Y. S. Wang, Z. W. Li, Chun-sheng Zhang, Yuan-Yuan Du, Xiaobo Li, X. L. Cao, J. Y. Nie, Y. X. Zhu, Ming-Yu Ge, Y. G. Zheng, Yi Jung Yang, J. Y. Liao, Min Gao, H. M. Zhang, Fuqin Zhang, S. N. Zhang, Y. Nang, Y. J. Jin, J. K. Deng, J. Guan, Wei Zhang, Z. Chang, Tian-Xiang Chen, Yi-Qiao Dong, Q. Q. Yin, Y. P. Chen, Cheng-Cheng Guo, Yunchao Liu, J. L. Qu, F. J. Lu, Long Ji, X. H. Ma, GuoQing Liu, Yan Ji Yang, Jia Huo, Gang Chen, W. C. Zhang, Y. F. Zhang, B. Lu, XiangYang Wen, B. B. Wu, Junqiang Zhang, Li-Ming Song, G Ou, Z. L. Zhang, Gang Li, Lian Tao, Y. H. Tan, D. K. Zhou, Xue-Feng Lu, Zhao Zhang, X. Y. Song, Ya Fang Huang, Tong Li, Lei Sun, L. Chen, Yuan You, J. F. Zhou, S. M. Jia, Yu-Xuan Zhu, Ling-Jun Wang, W. Z. Zhang, Qi-Bin Yi, Cunguo Wang, Wei Cui, T. Zhang, L. D. Kong, X. J. Liu, H. W. Liu, X. X. Li, Yu-Dong Gu, N. Sai, S. J. Zheng, Y. G. Li, Aimei Zhang, G. H. Gao, M. Wu, Y. Zhang, R. L. Zhuang, J. Jin, Xin-Fu Zhao, R. C. Shang, C. Z. Liu, Sisi Yang, Shaolin Xiong, Y. J. Zhang, H. Gao, Y. L. Tuo, J. W. Yang, Qiu-Yi Luo, G. C. Xiao, H. S. Zhao, Bin Meng, P. J. Wang, G. F. Wang, and W. S. Wang
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Swift, Physics, Astrophysics::High Energy Astrophysical Phenomena, Phase (waves), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Relative strength, Astrophysics::Cosmology and Extragalactic Astrophysics, Pulse (physics), Luminosity, symbols.namesake, Radiation pressure, Space and Planetary Science, Eddington luminosity, symbols, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, computer, Energy (signal processing), Astrophysics::Galaxy Astrophysics, computer.programming_language
Abstract: Based on Insight-HXMT data, we report on the pulse fraction evolution during the 2017–2018 outburst of the newly discovered first Galactic ultraluminous X-ray (ULX) source Swift J0243.6+6124. The pulse fractions of 19 observation pairs selected in the rising and fading phases with similar luminosity are investigated. The results show a general trend of the pulse fraction increasing with luminosity and energy at supercritical luminosity. However, the relative strength of the pulsation between each pair evolves strongly with luminosity. The pulse fraction in the rising phase is larger at luminosity below 7.71 × 1038 erg s−1, but smaller at above. A transition luminosity is found to be energy independent. Such a phenomenon is first confirmed by Insight-HXMT observations and we speculate that it may have relation with the radiation-pressure-dominated accretion disc.
Published: 2020

15. The Evolution of the Broadband Temporal Features Observed in the Black-hole Transient MAXI J1820+070 with Insight-HXMT

Author: Yanan Wang, Long Ji, S. N. Zhang, Mariano Méndez, J. L. Qu, Pierre Maggi, M. Y. Ge, Erlin Qiao, L. Tao, S. Zhang, Diego Altamirano, L. Zhang, X. Ma, F. J. Lu, T. P. Li, Y. Huang, S. J. Zheng, Y. P. Chen, Z. Chang, Y. L. Tuo, C. Güngör, L. M. Song, Y. P. Xu, X. L. Cao, Y. Chen, C. Z. Liu, Q. C. Bu, C. Cai, G. Chen, L. Chen, T. X. Chen, Y. B. Chen, W. Cui, W. W. Cui, J. K. Deng, Y. W. Dong, Y. Y. Du, M. X. Fu, G. H. Gao, H. Gao, M. Gao, Y. D. Gu, J. Guan, C. C. Guo, D. W. Han, J. Huo, S. M. Jia, L. H. Jiang, W. C. Jiang, J. Jin, Y. J. Jin, L. D. Kong, B. Li, C. K. Li, G. Li, M. S. Li, W. Li, X. Li, X. B. Li, X. F. Li, Y. G. Li, Z. W. Li, X. H. Liang, J. Y. Liao, G. Q. Liu, H. W. Liu, X. J. Liu, Y. N. Liu, B. Lu, X. F. Lu, Q. Luo, T. Luo, B. Meng, Y. Nang, J. Y. Nie, G. Ou, N. Sai, R. C. Shang, X. Y. Song, L. Sun, Y. Tan, G. F. Wang, J. Wang, W. S. Wang, Y. D. Wang, Y. S. Wang, X. Y. Wen, B. B. Wu, B. Y. Wu, M. Wu, G. C. Xiao, S. Xiao, S. L. Xiong, J. W. Yang, S. Yang, Y. J. Yang, Q. B. Yi, Q. Q. Yin, Y. You, A. M. Zhang, C. M. Zhang, F. Zhang, H. M. Zhang, J. Zhang, T. Zhang, W. C. Zhang, W. Zhang, W. Z. Zhang, Y. Zhang, Y. F. Zhang, Y. J. Zhang, Z. Zhang, Z. L. Zhang, H. S. Zhao, X. F. Zhao, D. K. Zhou, J. F. Zhou, R. L. Zhuang, Y. X. Zhu, Y. Zhu, Lingjun Wang, Observatoire astronomique de Strasbourg (ObAS), Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Astronomy
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Range (particle radiation), Jet (fluid), Photon, 010504 meteorology & atmospheric sciences, Hardness ratio, Black holes, Astrophysics::High Energy Astrophysical Phenomena, Time lag, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Low-mass x-ray binary stars, Space and Planetary Science, 0103 physical sciences, Broadband, Transient (oscillation), Electronic band structure, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, Compact objects, 0105 earth and related environmental sciences
Abstract: We study the evolution of the temporal properties of MAXI 1820+070 during the 2018 outburst in its hard state from MJD 58190 to 58289 with Insight-HXMT in a broad energy band 1-150 keV. We find different behaviors of the hardness ratio, the fractional rms and time lag before and after MJD 58257, suggesting a transition occurred at around this point. The observed time lags between the soft photons in the 1-5 keV band and the hard photons in higher energy bands, up to 150 keV, are frequency-dependent: the time lags in the low-frequency range, 2-10 mHz, are both soft and hard lags with a timescale of dozens of seconds but without a clear trend along the outburst; the time lags in the high-frequency range, 1-10 Hz, are only hard lags with a timescale of tens of milliseconds; first increase until around MJD 58257 and decrease after this date. The high-frequency time lags are significantly correlated to the photon index derived from the fit to the quasi-simultaneous NICER spectrum in the 1-10 keV band. This result is qualitatively consistent with a model in which the high-frequency time lags are produced by Comptonization in a jet., Comment: Accepted for publication in ApJ
Published: 2020

16. Role of Endoplasmic Reticulum Stress in Otitis Media

Author: H. S. Zhao, Xiaolin Zhang, Tong Zhao, Bo Li, Juan Che, Jun Chen, Zhaomin Fan, Yanfei Wang, Bo Hua Hu, Maria Hatzoglou, Tihua Zheng, Xiuzhen Liu, and Qingyin Zheng
Subjects: 0301 basic medicine, Programmed cell death, lcsh:QH426-470, endoplasmic reticulum (ER) stress, Caspase 3, Proinflammatory cytokine, 03 medical and health sciences, chemistry.chemical_compound, 0302 clinical medicine, Downregulation and upregulation, Genetics, Genetics (clinical), streptococcal peptidoglycan polysaccharide, Original Research, tauroursodeoxycholic acid, therapy, ATF6, Endoplasmic reticulum, apoptosis, Tauroursodeoxycholic acid, otitis media, Cell biology, lcsh:Genetics, 030104 developmental biology, chemistry, 030220 oncology & carcinogenesis, Unfolded protein response, Molecular Medicine
Abstract: Endoplasmic reticulum (ER) stress occurs in many inflammatory responses. Here, we investigated the role of ER stress and its associated apoptosis in otitis media (OM) to elucidate the mechanisms of OM and the signaling crosstalk between ER stress and other cell damage pathways, including inflammatory cytokines and apoptosis. We examined the expression of inflammatory cytokine- and ER stress-related genes by qRT-PCR, Western blotting, and immunohistochemistry (IHC) in the middle ear of C57BL/6J mice after challenge with peptidoglycan polysaccharide (PGPS), an agent inducing OM. We also evaluated the effect of the suppression of ER stress with tauroursodeoxycholic acid (TUDCA), an ER stress inhibitor. The study revealed the upregulation of ER stress- and apoptosis-related gene expression after the PGPS treatment, specifically ATF6, CHOP, BIP, caspase-12, and caspase-3. TUDCA treatment of PGPS-treated mice decreased OM; reduced the expression of CHOP, BIP, and caspase 3; and significantly decreased the proinflammatory gene expression of tumor necrosis factor-α (TNF-α) and interleukin-6 (IL-6). These results suggest that PGPS triggers ER stress and downstream proinflammatory gene expression in OM and that inhibition of ER stress alleviates OM. We propose that ER stress plays a critical role in inflammation and cell death, leading to the development of OM and points to ER stress inhibition as a potential therapeutic approach for the prevention of OM.
Published: 2020

17. Switches between accretion structures during flares in 4U 1901+03

Author: Z. Chang, Fuqin Zhang, S. N. Zhang, Qiu-Yi Luo, Y. B. Chen, B. B. Wu, Tao Luo, Aimei Zhang, J. Y. Zhang, Ming-Yu Ge, Armin Nabizadeh, Y. G. Li, S. Xiao, Y. L. Tuo, J. W. Yang, L. Chen, Chun-sheng Zhang, Peng Zhang, Yu-Dong Gu, Sergey S. Tsygankov, C. K. Li, Y. J. Jin, J. Y. Nie, M. X. Fu, Yue Zhang, X. J. Liu, Luhua Jiang, Y. P. Xu, Zhao Zhang, G. C. Xiao, Bo Li, H. Xu, Yu-Xuan Zhu, J. Z. Wang, X. H. Liang, W. Z. Zhang, L. Sun, Z. W. Li, G. H. Gao, Yanji Yang, Wan-Chang Zhang, Weiguang Cui, C. Cai, F. J. Lu, Yunchao Liu, Qingcui Bu, X. L. Cao, B. S. Liu, Bin Meng, D. K. Zhou, Y. J. Yang, Shaolin Xiong, Wenxiong Li, Tian-Xiang Chen, Lian Tao, Yi Zhang, Y. J. Zhang, M. Wu, Andrea Santangelo, XiangYang Wen, Suleimanov, H. Gao, Z. Zhang, L. D. Kong, X. Y. Song, Long Ji, W. C. Zhang, Q. B. Yi, B. Y. Wu, Mao-Shun Li, Q. Q. Yin, You-Hong Zhang, H. W. Liu, N. Sai, Da-Wei Han, J. Y. Liao, H. M. Zhang, Zhi Zhang, Ya Fang Huang, Y. F. Zhang, Min Gao, X. B. Li, B. Lu, J. L. Qu, Yi-Qiao Dong, Wenhan Jiang, Cheng-Cheng Guo, Y. S. Wang, Doroshenko, Yuan-Yuan Du, C. Z. Liu, Y X Zhu, Y. P. Chen, Sisi Yang, Y. H. Tan, J. F. Zhou, J. Jin, Xin-Fu Zhao, R. C. Shang, Xuelong Li, J. Guan, GuoQing Liu, Jia Huo, Gang Li, Lorenzo Ducci, Wei Cui, T. Zhang, Li-Ming Song, Xue-Feng Lu, Shuinai Zhang, S. M. Jia, He-Yang Liu, Y. Nang, R. L. Zhuang, J. K. Deng, C. Wang, X. H. Ma, H. S. Zhao, Ti-Pei Li, P. J. Wang, G. F. Wang, W. S. Wang, Ge Ou, Gang Chen, Yuan You, X. X. Li, and S. J. Zheng
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Accretion (astrophysics), Spectral line, Beam pattern, Neutron star, Accretion rate, Pulsar, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Polar cap, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: We report on our analysis of the 2019 outburst of the X-ray accreting pulsar 4U 1901+03 observed with Insight-HXMT and NICER. Both spectra and pulse profiles evolve significantly in the decaying phase of the outburst. Dozens of flares are observed throughout the outburst. They are more frequent and brighter at the outburst peak. We find that the flares, which have a duration from tens to hundreds of seconds, are generally brighter than the persistent emission by a factor of $\sim$ 1.5. The pulse profile shape during the flares can be significantly different than that of the persistent emission. In particular, a phase shift is clearly observed in many cases. We interpret these findings as direct evidence of changes of the pulsed beam pattern, due to transitions between the sub- and super-critical accretion regimes on a short time scale. We also observe that at comparable luminosities the flares' pulse profiles are rather similar to those of the persistent emission. This indicates that the accretion on the polar cap of the neutron star is mainly determined by the luminosity, i.e., the mass accretion rate., 11 pages, 8 figures, accepted for publication in MNRAS
Published: 2020

18. Insight-HXMT firm detection of the highest energy fundamental cyclotron resonance scattering feature in the spectrum of GRO J1008-57

Author: M. Y. Ge, L. Ji, S. N. Zhang, A. Santangelo, C. Z. Liu, V. Doroshenko, R. Staubert, J. L. Qu, S. Zhang, F. J. Lu, L. M. Song, T. P. Li, L. Tao, Y. P. Xu, X. L. Cao, Y. Chen, Q. C. Bu, C. Cai, Z. Chang, G. Chen, L. Chen, T. X. Chen, Y. B. Chen, Y. P. Chen, W. Cui, W. W. Cui, J. K. Deng, Y. W. Dong, Y. Y. Du, M. X. Fu, G. H. Gao, H. Gao, M. Gao, Y. D. Gu, J. Guan, C. C. Guo, D. W. Han, Y. Huang, J. Huo, S. M. Jia, L. H. Jiang, W. C. Jiang, J. Jin, Y. J. Jin, L. D. Kong, B. Li, C. K. Li, G. Li, M. S. Li, W. Li, X. Li, X. B. Li, X. F. Li, Y. G. Li, Z. W. Li, X. H. Liang, J. Y. Liao, B. S. Liu, G. Q. Liu, H. W. Liu, X. J. Liu, Y. N. Liu, B. Lu, X. F. Lu, Q. Luo, T. Luo, X. Ma, B. Meng, Y. Nang, J. Y. Nie, G. Ou, N. Sai, R. C. Shang, X. Y. Song, L. Sun, Y. Tan, Y. L. Tuo, C. Wang, G. F. Wang, J. Wang, L. J. Wang, W. S. Wang, Y. D. Wang, Y. S. Wang, X. Y. Wen, B. B. Wu, B. Y. Wu, M. Wu, G. C. Xiao, S. Xiao, S. L. Xiong, H. Xu, J. W. Yang, S. Yang, Y. J. Yang, Q. B. Yi, Q. Q. Yin, Y. You, A. M. Zhang, C. M. Zhang, F. Zhang, H. M. Zhang, J. Zhang, T. Zhang, W. C. Zhang, W. Zhang, W. Z. Zhang, Y. Zhang, Y. F. Zhang, Y. J. Zhang, Z. Zhang, Z. L. Zhang, H. S. Zhao, X. F. Zhao, S. J. Zheng, Y. G. Zheng, D. K. Zhou, J. F. Zhou, R. L. Zhuang, Y. X. Zhu, and Y. Zhu
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010504 meteorology & atmospheric sciences, Scattering, Astrophysics::High Energy Astrophysical Phenomena, Cyclotron resonance, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Inelastic scattering, 01 natural sciences, Resonance (particle physics), Spectral line, Pulsar, Space and Planetary Science, 0103 physical sciences, Continuum (set theory), Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Line (formation)
Abstract: We report on the observation of the accreting pulsar GRO J1008-57 performed by Insight-HXMT at the peak of the source's 2017 outburst. Pulsations are detected with a spin period of 93.283(1) s. The pulse profile shows double peaks at soft X-rays, and only one peak above 20 keV. The spectrum is well described by the phenomenological models of X-ray pulsars. A cyclotron resonant scattering feature is detected with very high statistical significance at a centroid energy of $E_{\rm cyc}=90.32_{-0.28}^{+0.32}$ keV, for the reference continuum and line models, HIGHECUT and GABS respectively. Detection is very robust with respect to different continuum models. The line energy is significantly higher than what suggested from previous observations, which provided very marginal evidence for the line. This establishes a new record for the centroid energy of a fundamental cyclotron resonant scattering feature observed in accreting pulsars. We also discuss the accretion regime of the source during the Insight-HXMT observation., Comment: 8 pages, 3 figures, accepted for publication in ApJL
Published: 2020
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19. Constraining the transient high-energy activity of FRB180916.J0158+65 with Insight-HXMT followup observations

Author: L. Chen, Yu-Dong Gu, Ya Fang Huang, R. J. Yang, Y. J. Yang, L. Wang, Junqiang Zhang, Wenhan Jiang, Qiu-Yi Luo, X. H. Liang, C. Z. Liu, G. C. Xiao, B. Y. Wu, Y. L. Tuo, Sisi Yang, He-Yang Liu, Wei Cui, W. S. Wang, Xiaobo Li, Wei Zhang, G. H. Gao, Ge Ou, Bing Li, B. B. Wu, Bin Meng, C. Guidorzi, F. Frontera, Yi Zhang, C. Cai, Luciano Nicastro, Lei Sun, Mauro Orlandini, M. Wu, J. Jin, Xin-Fu Zhao, H. S. Zhao, Y. Nang, Cheng-Cheng Guo, Y. P. Xu, Tao Luo, Yuan You, Qingcui Bu, S. Xiao, C. K. Li, Qi-Bin Yi, Shaolin Xiong, P. J. Wang, Wenxiong Li, Y. B. Chen, J. Y. Liao, H. M. Zhang, L. D. Kong, B. S. Liu, X. X. Li, H. Gao, H. W. Liu, N. Sai, Z. W. Li, W. C. Zhang, R. C. Ma, Min Gao, Fuqin Zhang, Y. F. Zhang, S. N. Zhang, D. K. Zhou, C. Wang, J. L. Qu, J. Guan, Lorenzo Amati, Y. G. Zheng, Y. S. Wang, Xin Ren, Tian-Xiang Chen, E. Virgilli, Lian Tao, Z. Chang, Da-Wei Han, Jia Huo, Y. H. Tan, X. Y. Song, X. F. Li, Gang Li, P. Zhang, Ming-Yu Ge, J. Y. Nie, Yuan-Yuan Du, F. J. Lu, XiangYang Wen, X. H. Ma, Li-Ming Song, Xue-Feng Lu, Tong Li, S. M. Jia, X. J. Liu, X. L. Cao, Q. Q. Yin, Y. P. Chen, S. J. Zheng, ITA, and CHN
Subjects: Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Socio-culturale, Context (language use), Astrophysics, Magnetar, 01 natural sciences, law.invention, Telescope, stars: magnetars, law, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Fast radio burst, Detector, Astronomy and Astrophysics, radiation mechanisms: non-thermal, stars: magnetars, radiation mechanisms: non-thermal, Wavelength, Space and Planetary Science, Phase space, Astrophysics - High Energy Astrophysical Phenomena, Energy (signal processing)
Abstract: A link between magnetars and fast radio burst (FRB) sources has finally been established. In this context, one of the open issues is whether/which sources of extra galactic FRBs exhibit X/gamma-ray outbursts and whether it is correlated with radio activity. We aim to constrain possible X/gamma-ray burst activity from one of the nearest extragalactic FRB sources currently known over a broad energy range, by looking for bursts over a range of timescales and energies that are compatible with being powerful flares from extragalactic magnetars. We followed up the as-yet nearest extragalactic FRB source at a mere 149 Mpc distance, the periodic repeater FRB180916.J0158+65, during the active phase on February 4-7, 2020, with the Insight-Hard X-ray Modulation Telescope (HXMT). Taking advantage of the combination of broad band, large effective area, and several independent detectors available, we searched for bursts over a set of timescales from 1 ms to 1.024 s with a sensitive algorithm, that had previously been characterised and optimised. Moreover, through simulations we studied the sensitivity of our technique in the released energy-duration phase space for a set of synthetic flares and assuming different energy spectra. We constrain the possible occurrence of flares in the 1-100 keV energy band to E, 10 pages, 3 figures, accepted by A&A
Published: 2020

20. X-ray reprocessing in accreting pulsar GX 301-2 observed with Insight-HXMT

Author: G. H. Gao, X. X. Li, M. Wu, S. J. Zheng, Y. G. Zheng, Y. Nang, Mauro Orlandini, J. Y. Liao, H. M. Zhang, Y. L. Tuo, Y. J. Yang, R. C. Ma, Y. F. Zhang, X. B. Li, B. S. Liu, Yuan You, X. Q. Ren, Yanji Yang, Armin Nabizadeh, C. Cai, L. Chen, Tian-Xiang Chen, Wenxiong Li, Wan-Chang Zhang, W. S. Wang, Yi Zhang, Ge Ou, Andrea Santangelo, R. J. Yang, Bo Li, Peng Zhang, Qiu-Yi Luo, B. B. Wu, Cunguo Wang, H. S. Zhao, Li-Ming Song, Ming-Yu Ge, C. K. Li, F. J. Lu, Xue-Feng Lu, Y. P. Chen, Shuinai Zhang, Tong Li, Y. H. Tan, P. J. Wang, J. Y. Zhang, Victor Doroshenko, Shaolin Xiong, S. M. Jia, XiangYang Wen, Ling-Jun Wang, H. Gao, Jiren Liu, X. H. Ma, Z. W. Li, Yuan-Yuan Du, C. Z. Liu, D. K. Zhou, Sisi Yang, Ya Fang Huang, J. Jin, Xin-Fu Zhao, G. Li, Tao Luo, S. Xiao, Yu-Dong Gu, X. J. Liu, D. Gavran, X. L. Cao, Q. Q. Yin, Q. B. Yi, B. Y. Wu, V. F. Suleimanov, L. D. Kong, Y. B. Chen, X. H. Liang, L. Sun, Fuqin Zhang, S. N. Zhang, Long Ji, Z. Chang, Y. H. Zhang, Y. P. Xu, Wenhan Jiang, H. W. Liu, N. Sai, Y. S. Wang, W. C. Zhang, Xuelong Li, J. Guan, Lian Tao, Cheng-Cheng Guo, X. Y. Song, Jia Huo, Lorenzo Ducci, J. Y. Nie, Bin Meng, Wei Cui, G. C. Xiao, Qingcui Bu, Da-Wei Han, J. L. Qu, Hongfei Liu, ITA, DEU, and CHN
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Accretion (meteorology), Astrophysics::High Energy Astrophysical Phenomena, X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radiation, 01 natural sciences, Neutron star, Pulsar, Space and Planetary Science, Ionization, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010306 general physics, Absorption (electromagnetic radiation), Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Equivalent width, Astrophysics::Galaxy Astrophysics
Abstract: We investigate the absorption and emission features in observations of GX 301-2 detected with Insight-HXMT/LE in 2017-2019. At different orbital phases, we found prominent Fe Kalpha, Kbeta and Ni Kalpha lines, as well as Compton shoulders and Fe K-shell absorption edges. These features are due to the X-ray reprocessing caused by the interaction between the radiation from the source and surrounding accretion material. According to the ratio of iron lines Kalpha and Kbeta, we infer the accretion material is in a low ionisation state. We find an orbital-dependent local absorption column density, which has a large value and strong variability around the periastron. We explain its variability as a result of inhomogeneities of the accretion environment and/or instabilities of accretion processes. In addition, the variable local column density is correlated with the equivalent width of the iron Kalpha lines throughout the orbit, which suggests that the accretion material near the neutron star is spherically distributed., Comment: 10 pages, 5 figures, 2 tables, accepted for publication in MNRAS
Published: 2020
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21. Discovery of delayed spin-up behavior following two large glitches in the Crab pulsar, and the statistics of such processes

Author: M. Y. Ge, S. N. Zhang, F. J. Lu, T. P. Li, J. P. Yuan, X. P. Zheng, Y. Huang, S. J. Zheng, Y. P. Chen, Z. Chang, Y. L. Tuo, Q. Cheng, C. Güngör, L. M. Song, Y. P. Xu, X. L. Cao, Y. Chen, C. Z. Liu, S. Zhang, J. L. Qu, Q. C. Bu, C. Cai, G. Chen, L. Chen, M. Z. Chen, T. X. Chen, Y. B. Chen, W. Cui, W. W. Cui, J. K. Deng, Y. W. Dong, Y. Y. Du, M. X. Fu, G. H. Gao, H. Gao, M. Gao, Y. D. Gu, J. Guan, C. C. Guo, D. W. Han, L. F. Hao, J. Huo, S. M. Jia, L. H. Jiang, W. C. Jiang, C. J. Jin, J. Jin, Y. J. Jin, L. D. Kong, B. Li, D. Li, C. K. Li, G. Li, M. S. Li, W. Li, X. Li, X. B. Li, X. F. Li, Y. G. Li, Z. W. Li, Z. X. Li, Z. Y. Liu, X. H. Liang, J. Y. Liao, G. Q. Liu, H. W. Liu, X. J. Liu, Y. N. Liu, B. Lu, X. F. Lu, Q. Luo, T. Luo, X. Ma, B. Meng, Y. Nang, J. Y. Nie, G. Ou, N. Sai, R. C. Shang, X. Y. Song, L. Sun, Y. Tan, L. Tao, C. Wang, G. F. Wang, J. Wang, J. B. Wang, M. Wang, N. Wang, W. S. Wang, Y. D. Wang, Y. S. Wang, X. Y. Wen, Z. G. Wen, B. B. Wu, B. Y. Wu, M. Wu, G. C. Xiao, S. Xiao, S. L. Xiong, Y. H. Xu, W. M. Yan, J. W. Yang, S. Yang, Y. J. Yang, Q. B. Yi, Q. Q. Yin, Y. You, Y. L. Yue, A. M. Zhang, C. M. Zhang, D. P. Zhang, F. Zhang, H. M. Zhang, J. Zhang, T. Zhang, W. C. Zhang, W. Zhang, W. Z. Zhang, Y. Zhang, Y. F. Zhang, Y. J. Zhang, Z. Zhang, Z. L. Zhang, H. S. Zhao, X. F. Zhao, W. Zheng, D. K. Zhou, J. F. Zhou, X. Zhou, R. L. Zhuang, Y. X. Zhu, and Y. Zhu
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010504 meteorology & atmospheric sciences, Crab Pulsar, Astrophysics::High Energy Astrophysical Phenomena, Total frequency, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Glitch, Stars, Crab Nebula, Amplitude, Pulsar, Space and Planetary Science, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Spin-up, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences
Abstract: Glitches correspond to sudden jumps of rotation frequency ($\nu$) and its derivative ($\dot{\nu}$) of pulsars, the origin of which remains not well understood yet, partly because the jump processes of most glitches are not well time-resolved. There are three large glitches of the Crab pulsar, detected in 1989, 1996 and 2017, which were found to have delayed spin-up processes before the normal recovery processes. Here we report two additional glitches of the Crab pulsar occurred in 2004 and 2011 for which we discovered delayed spin up processes, and present refined parameters of the largest glitch occurred in 2017. The initial rising time of the glitch is determined as $, Comment: 25 pages, 8 figures
Published: 2020
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22. Isolation and Expression Analysis of PeDWF1 in Phyllostachys edulis

Author: H. S. Zhao, Yihong Yang, H. Y. Sun, H. Xu, S. N. Wang, and Z. M. Gao
Subjects: 0106 biological sciences, 0301 basic medicine, Oryza sativa, Sequence analysis, food and beverages, Plant Science, Biology, biology.organism_classification, 01 natural sciences, 03 medical and health sciences, Open reading frame, 030104 developmental biology, Phyllostachys edulis, Biochemistry, Shoot, Gene expression, Gene, Integral membrane protein, 010606 plant biology & botany
Abstract: Brassinosteroids (BRs) are steroidal hormones that play crucial roles in various processes of plant growth and development. DWF1 encodes a delta(24)-sterol reductase that participates in one of the early stage in the brassinosteroids’ biosynthetic pathway: the conversion of 24-methylenecholesterol to campesterol. Here we report the isolation and expression of one DWF1 homologous gene, PeDWF1, in moso bamboo (Phyllostachys edulis (Carriere) J. Houz.). Sequence analysis revealed that the open reading frame of PeDWF1 was 1686-bp encoding a protein composed of 561 amino acid residues with a calculated molecular weight of 65.1 kD and a theoretic isoelectric point of 8.32. Phylogenetic analysis indicated that PeDWF1 was very close to the cell elongation protein Dwarf1 in rice (Oryza sativa). Furthermore, transient expression of a PeDWF1::GFP fusion protein showed that PeDWF1 was an integral membrane protein most probably associated with the endoplasmic reticulum similar to Dwarf1. Tissue specific expression analysis showed that PeDWF1 was constitutively expressed in moso bamboo with the highest level in shoots and the lowest level in mature leaves. In the early growing stage of shoots, the expression level of PeDWF1 had a rising trend with the increasing height of shoots. These results indicated that PeDWF1 might be involved in the regulation of shoot development by participating in BRs biosynthesis. Moreover, PeDWF1 was heterologously expressed in Escherichia coli and the recombinant protein was about 65 kD, which facilitated further study on the gene function of PeDWF1 in bamboo.
Published: 2018

23. MiR-379-5p improved locomotor function recovery after spinal cord injury in rats by reducing endothelin 1 and inhibiting astrocytes expression

Author: J-C, A, Z-Y, Li, Q-F, Long, D-Y, Wang, H-S, Zhao, S-L, Jia, and W-H, Zhang
Subjects: Rats, Sprague-Dawley, Disease Models, Animal, MicroRNAs, Oxidative Stress, Endothelin-1, Astrocytes, Animals, Pentylenetetrazole, Female, Recovery of Function, Locomotion, Spinal Cord Injuries, Rats
Abstract: The aim of this study was to investigate the effect of microRNA-214-5p (miR-214-5p) on spinal cord injury (SCI) and to explore the mechanism of action in pathophysiological relevance.The model of SCI was successfully established in rats aged 6-8 weeks. The levels of the locomotor function recovery in rats of the miR-379-5p group and SCI group were detected one month later by Basso-Beattie-Bresnahan (BBB) locomotor rating scale. Biochemical indexes were measured by Western blotting and real time-PCR, respectively. In addition, rat astrocytes were cultured to verify the effect of miR-379-5p on activated astrocytes in vitro.Compared with the SCI group, the rats in the miR-379-5p group showed prominent improvement in the locomotor function in vivo. MiR-379-5p attenuated the activation of astrocytes and significantly suppressed the expressions of the nerve growth inhibitors. Furthermore, the down-regulation of endothelin-1 (ET-1) ameliorated the spinal cord ischemia, thereby reducing apoptosis and oxidative stress. Compared with the pentylenetetrazol (PTZ) group, ET-1 and chondroitin sulfate poly-glycoprotein (CSPG) in miR-379-5p group decreased significantly in the astrocytes transfected with miR-214-5p in vitro.MiR-379-5p retarded the neurofilament regeneration block effect by inhibiting endothelin 1 and the expression of the astrocytes after SCI. Furthermore, it might relieve nerve structure destruction, resist oxidative stress, and inhibit apoptosis, eventually promoting functional recovery.
Published: 2019

24. Hot disk of the Swift J0243.6+6124 revealed by Insight-HXMT

Author: J. K. Deng, X. H. Ma, B. B. Wu, Min Gao, Lian Tao, L. Chen, Yi-Yan Yang, X. Y. Song, C. L. Zhang, Xue-Feng Lu, Shuinai Zhang, H. S. Zhao, S. M. Jia, C. Z. Liu, M. X. Fu, Y. Nang, Ya Fang Huang, Tao Luo, Wan-Chang Zhang, Bin Meng, Mao-Shun Li, Sisi Yang, X. X. Li, L. J. Qu, J. Z. Wang, Y. L. Tuo, G. F. Wang, J. W. Yang, W. C. Jiang, Tian-Xiang Chen, Weiguang Cui, Qingcui Bu, Yunchao Liu, Y. J. Jin, L. M. Song, Sergey S. Tsygankov, Y. J. Yang, V. Doroshenko, Ti-Pei Li, F. Zhang, Yuan-Yuan Du, S. J. Zheng, Gang Chen, W. S. Wang, J. Y. Liao, H. M. Zhang, Junke Zhang, Wenxiong Li, Qing-He Zhang, Ge Ou, Da-Wei Han, XiangYang Wen, J. Y. Nie, Y. F. Zhang, Andrea Santangelo, Shaolin Xiong, Bo Lu, J. Jin, Y. J. Zhang, Xuchao Zhao, H. Gao, W. Z. Zhang, Wei Zhang, G. H. Gao, Yi-Qiao Dong, Y. H. Tan, Cheng-Cheng Guo, M. Wu, Y. Zhang, Fangjun Lu, Y. B. Chen, Alexander A. Mushtukov, Z. Zhang, Long Ji, Y. P. Chen, Bing Li, Y. S. Wang, T. Zhang, Chun-sheng Zhang, Xiaobo Li, W. Hu, X. F. Li, X. H. Liang, C. L. Zou, Z. L. Zhang, C. K. Li, G. C. Xiao, H. Xu, Y. X. Zhu, Z. W. Li, Ming-Yu Ge, Z. J. Li, ShaoZhen Liu, L. D. Kong, Yidong Xu, Yu-Dong Gu, S. N. Zhang, Jia Huo, Gang Li, X. L. Cao, J. Zhao, J. Guan, Aimei Zhang, GuoQing Liu, Wei Cui, Yu-Xuan Zhu, X. J. Liu, Liang Sun, Y. G. Li, Luhua Jiang, Z. Chang, Yujuan Liu, H. W. Liu, and N. Sai
Subjects: Swift, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Magnetosphere, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Pulsar, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, computer.programming_language, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Scattering, Spectral properties, Astronomy and Astrophysics, Accretion (astrophysics), Neutron star, Radiation pressure, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, computer
Abstract: We report on analysis of observations of the bright transient X-ray pulsar \src obtained during its 2017-2018 giant outburst with Insight-HXMT, \emph{NuSTAR}, and \textit{Swift} observatories. We focus on the discovery of a sharp state transition of the timing and spectral properties of the source at super-Eddington accretion rates, which we associate with the transition of the accretion disk to a radiation pressure dominated (RPD) state, the first ever directly observed for magnetized neutron star. This transition occurs at slightly higher luminosity compared to already reported transition of the source from sub- to super-critical accretion regime associate with onset of an accretion column. We argue that this scenario can only be realized for comparatively weakly magnetized neutron star, not dissimilar to other ultra-luminous X-ray pulsars (ULPs), which accrete at similar rates. Further evidence for this conclusion is provided by the non-detection of the transition to the propeller state in quiescence which strongly implies compact magnetosphere and thus rules out magnetar-like fields., Submitted to MNRAS
Published: 2019

25. Timing analysis of 2S 1417-624 observed with NICER and Insight-HXMT

Author: Tao Luo, J. Y. Zhang, B. B. Wu, G. H. Gao, Z. L. Zhang, Gang Chen, M. Wu, Y. Zhang, C. K. Li, Wei Zhang, Y. P. Chen, Y. H. Tan, Yi-Qiao Dong, H. Xu, Y. J. Jin, Victor Doroshenko, Shaolin Xiong, Z. W. Li, Cheng-Cheng Guo, F. J. Lu, Ya Fang Huang, Bo Li, Y. J. Zhang, J. Jin, J. K. Deng, H. Gao, L. Chen, Yi-Yan Yang, J. Y. Liao, H. M. Zhang, Tian-Xiang Chen, Yunchao Liu, XiangYang Wen, X. X. Li, Y. F. Zhang, X. B. Li, X. H. Ma, Can Güngör, Li-Ming Song, Xue-Feng Lu, Suo Liu, Xuchao Zhao, W. C. Zhang, Y. S. Wang, J. Zhao, Y. Nang, J. Y. Nie, S. J. Zheng, Mao-Shun Li, Lian Tao, X. H. Liang, L. Sun, Y. G. Li, Qing-He Zhang, Y. L. Tuo, Aimei Zhang, J. W. Yang, C. Z. Liu, S. M. Jia, X. Y. Song, Y. B. Chen, Luhua Jiang, W. Hu, L. J. Qu, H. W. Liu, Sisi Yang, Yu-Xuan Zhu, Z. Zhang, Long Ji, N. Sai, Yuan-Yuan Du, Chun-sheng Zhang, Wenhan Jiang, C. L. Zou, Yupeng Xu, X. J. Liu, X. L. Cao, Z. Chang, C. L. Zhang, Yujuan Liu, Wenxiong Li, B. Lu, S. N. Zhang, Andrea Santangelo, Y. X. Zhu, Ming-Yu Ge, Jia Huo, Gang Li, Lorenzo Ducci, Wei Cui, T. Zhang, W. Z. Zhang, Ti-Pei Li, Xuelong Li, J. Guan, Z. J. Li, L. D. Kong, GuoQing Liu, Bin Meng, Yu-Dong Gu, Y. J. Yang, G. C. Xiao, Fuqin Zhang, W. S. Wang, Ge Ou, Da-Wei Han, Min Gao, H. S. Zhao, M. X. Fu, J. Z. Wang, Weiguang Cui, G. F. Wang, and Qingcui Bu
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Accretion (meteorology), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Theoretical models, FOS: Physical sciences, Static timing analysis, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Radiation, 01 natural sciences, Luminosity, Magnetic field, QC Physics, Pulsar, Space and Planetary Science, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Fermi Gamma-ray Space Telescope
Abstract: We present a study of timing properties of the accreting pulsar 2S 1417-624 observed during its 2018 outburst, based on Swift/BAT, Fermi/GBM, Insight-HXMT and NICER observations. We report a dramatic change of the pulse profiles with luminosity. The morphology of the profile in the range 0.2-10.0keV switches from double to triple peaks at $\sim2.5$ $\rm \times 10^{37}{\it D}_{10}^2\ erg\ s^{-1}$ and from triple to quadruple peaks at $\sim7$ $\rm \times 10^{37}{\it D}_{10}^2\ erg\ s^{-1}$. The profile at high energies (25-100keV) shows significant evolutions as well. We explain this phenomenon according to existing theoretical models. We argue that the first change is related to the transition from the sub to the super-critical accretion regime, while the second to the transition of the accretion disc from the gas-dominated to the radiation pressure-dominated state. Considering the spin-up as well due to the accretion torque, this interpretation allows to estimate the magnetic field self-consistently at $\sim7\times 10^{12}$G., 7 pages, 4 figures, 1 tables, accepted for publication in MNRAS
Published: 2019

26. Non-thermal Electron Energization During the Impulsive Phase of an X9.3 Flare Revealed by Insight-HXMT

Author: C. K. Li, H. S. Zhao, L. M. Song, D. K. Zhou, Yang Su, Shuinai Zhang, Wei Wang, Shuang-Nan Zhang, H. Tian, S. M. Liu, and Peng Zhang
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Electron density, Solar flare, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Magnetic reconnection, Astrophysics, Electron, Radius, Corona, law.invention, Magnetic field, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, law, Astrophysics - High Energy Astrophysical Phenomena, Solar and Stellar Astrophysics (astro-ph.SR), Flare
Abstract: The X9.3 flare SOL20170906T11:55 was observed by the CsI detector aboard the first Chinese X-ray observatory Hard X-ray Modulation telescope (Insight-HXMT). By using wavelets method, we report about 22 s quasiperiodic pulsations(QPPs) during the impulsive phase. And the spectra from 100 keV to 800 keV showed the evolution with the gamma-ray flux, of a power-law photon index from $\sim 1.8$ before the peak, $\sim 2.0$ around the flare peak, to $\sim 1.8$ again. The gyrosynchrotron microwave spectral analysis reveals a $36.6 \pm 0.6 \arcsec$ radius gyrosynchrotron source with mean transverse magnetic field around 608.2 Gauss, and the penetrated $\ge$ 10 keV non-thermal electron density is about $10^{6.7} \mathrm{cm}^{-3}$ at peak time. The magnetic field strength followed the evolution of high-frequency radio flux. Further gyrosynchrotron source modeling analysis implies that there exists a quite steady gyrosynchrotron source, the non-thermal electron density and transverse magnetic field evolution are similar to higher-frequency light curves. The temporally spectral analysis reveals that those non-thermal electrons are accelerated by repeated magnetic reconnection, likely from a lower corona source., Comment: 14 pages, 9 figures, accept for publication by ApJ
Published: 2021

27. The Insight-HXMT mission and its recent progresses

Author: Yupeng Xu, Jing Jin, Lian Tao, Shaolin Xiong, G. F. Wang, X. L. Cao, Shu-Mei Jia, F. J. Lu, Shu Zhang, C. K. Li, J. Y. Liao, Yu-Peng Chen, Li-Ming Song, J. Y. Nie, Xiaobo Li, Tao Li, H. S. Zhao, Y. B. Chen, Shuang-Nan Zhang, ShiJie Zheng, J. L. Qu, C. Z. Liu, J. Guan, Fan Zhang, Huanyu Wang, X. Ma, Yue Huang, Ming-Yu Ge, and Junqiang Zhang
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Computer science, Payload, business.industry, media_common.quotation_subject, FOS: Physical sciences, 01 natural sciences, law.invention, Telescope, Software, Sky, law, Observatory, 0103 physical sciences, Satellite, Ground segment, Astrophysics - High Energy Astrophysical Phenomena, business, Gamma-ray burst, 010303 astronomy & astrophysics, media_common, Remote sensing
Abstract: The Hard X-ray Modulation Telescope HXMT or also dubbed as Insight HXMT is China s first astronomical satellite . It was launched on 15 th June 2017 in JiuQuan, China and is currently in service smoothly. It was designed to perform point ing , scan ning and gamma ray burst (GRB) observations and , based on the Direct Demodulation Method (DDM), the image of the scanned sky region can be reconstructed. Here we introduce the mission and its progresses in aspects of payload, core sciences, ground calibration/facility , ground segment, data archive, software, in orbit performance, calibration, background model, observations and preliminary results ., Comment: published in Proceedings of the SPIE, Volume 10699, id. 106991U 22 pp. (2018)
Published: 2019
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28. Insight-HXMT Observations of a Possible Fast Transition from the Jet- to Wind-dominated State during a Huge Flare of GRS 1915+105

Author: R. J. Yang, Qiu-Yi Luo, L. Chen, H. S. Zhao, Y. L. Tuo, J. Y. Liao, H. M. Zhang, Y. Nang, Lei Sun, C. Z. Liu, Lian Tao, D. K. Zhou, R. C. Ma, Y. F. Zhang, Yuan You, Y. H. Zhang, X. Y. Song, X. H. Ma, Yuan-Yuan Du, Qi-Bin Yi, B. Y. Wu, P. J. Wang, Tao Luo, Bo Liu, B. B. Wu, Xuelong Li, J. Guan, Li-Ming Song, S. Xiao, Bo Li, Shaolin Xiong, X. X. Li, Xue-Feng Lu, H. Gao, G. H. Gao, Tong Li, S. M. Jia, Y. P. Xu, Sisi Yang, S. J. Zheng, F. J. Lu, M. Wu, Jia Huo, XiangYang Wen, Y. H. Tan, Ya Fang Huang, Peng Zhang, Qingcui Bu, Y. G. Zheng, H. W. Liu, Y. J. Yang, X. L. Cao, Gang Li, W. S. Wang, Tian-Xiang Chen, N. Sai, Cunguo Wang, C. K. Li, Ge Ou, W. C. Zhang, S. N. Zhang, Y. B. Chen, Junqiang Zhang, Q. Q. Yin, Z. W. Li, Y. P. Chen, G. C. Xiao, J. Jin, Xin-Fu Zhao, X. J. Liu, Y. S. Wang, Wenhan Jiang, Ling-Jun Wang, C. Cai, Wenxiong Li, Gang Chen, Z. Chang, Da-Wei Han, L. D. Kong, Xiong Li, Yu-Dong Gu, Bin Meng, Min Gao, Ming-Yu Ge, X. H. Liang, J. L. Qu, Hongfei Liu, Fuqin Zhang, Long Ji, X. Q. Ren, Wei Cui, J. Y. Nie, Wei Zhang, and Cheng-Cheng Guo
Subjects: 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, X-ray binary, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Spectral line, Luminosity, law.invention, Astrophysical jet, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Accretion (meteorology), Astronomy and Astrophysics, Radius, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Energy (signal processing), Flare
Abstract: We present the analysis of the brightest flare that was recorded in the \emph{Insight}-HMXT data set, in a broad energy range (2$-$200 keV) from the microquasar GRS~1915+105 during an unusual low-luminosity state. This flare was detected by \emph{Insight}-HXMT among a series of flares during 2 June 2019 UTC 16:37:06 to 20:11:36, with a 2-200 keV luminosity of 3.4$-$7.27$\times10^{38}$ erg s$^{-1}$. Basing on the broad-band spectral analysis, we find that the flare spectrum shows different behaviors during bright and faint epochs. The spectrum of the flare can be fitted with a model dominated by a power-law component. Additional components show up in the bright epoch with a hard tail and in the faint epoch with an absorption line $\sim$ 6.78 keV. The reflection component of the latter is consistent with an inner disk radius $\sim$ 5 times larger than that of the former. These results on the giant flare during the "unusual" low-luminosity state of GRS~1915+105 may suggest that the source experiences a possible fast transition from a jet-dominated state to a wind-dominated state. We speculate that the evolving accretion disk and the large-scale magnetic field may play important roles in this peculiar huge flare.
Published: 2021

29. Two Complete Spectral Transitions of Swift J0243.6+6124 Observed by Insight-HXMT

Author: L. D. Kong, S. Zhang, Y. P. Chen, S. N. Zhang, L. Ji, V. Doroshenko, P. J. Wang, L. Tao, M. Y. Ge, C. Z. Liu, L. M. Song, F. J. Lu, J. L. Qu, T. P. Li, Y. P. Xu, X. L. Cao, Y. Chen, Q. C. Bu, C. Cai, Z. Chang, G. Chen, L. Chen, T. X. Chen, Y. B. Chen, W. Cui, W. W. Cui, J. K. Deng, Y. W. Dong, Y. Y. Du, M. X. Fu, G. H. Gao, H. Gao, M. Gao, Y. D. Gu, J. Guan, C. C. Guo, D. W. Han, Y. Huang, J. Huo, S. M. Jia, L. H. Jiang, W. C. Jiang, J. Jin, Y. J. Jin, B. Li, C. K. Li, G. Li, M. S. Li, W. Li, X. Li, X. B. Li, X. F. Li, Y. G. Li, Z. W. Li, X. H. Liang, J. Y. Liao, B. S. Liu, G. Q. Liu, H. W. Liu, X. J. Liu, Y. N. Liu, B. Lu, X. F. Lu, Q. Luo, T. Luo, X. Ma, B. Meng, Y. Nang, J. Y. Nie, G. Ou, N. Sai, R. C. Shang, X. Y. Song, L. Sun, Y. Tan, Y. L. Tuo, C. Wang, G. F. Wang, J. Wang, L. J. Wang, W. S. Wang, Y. S. Wang, X. Y. Wen, B. B. Wu, B. Y. Wu, M. Wu, G. C. Xiao, S. Xiao, S. L. Xiong, H. Xu, J. W. Yang, S. Yang, Y. J. Yang, Q. B. Yi, Q. Q. Yin, Y. You, A. M. Zhang, C. M. Zhang, F. Zhang, H. M. Zhang, J. Zhang, T. Zhang, W. C. Zhang, W. Zhang, W. Z. Zhang, Y. Zhang, Y. F. Zhang, Y. J. Zhang, Z. Zhang, Z. L. Zhang, H. S. Zhao, X. F. Zhao, S. J. Zheng, Y. G. Zheng, D. K. Zhou, J. F. Zhou, Y. X. Zhu, and R. L. Zhuang
Subjects: Physics, Swift, X-ray astronomy, Space and Planetary Science, X-ray binary, Astronomy and Astrophysics, Astrophysics, computer, Spectral line, Luminosity, computer.programming_language
Published: 2020

30. New weld toe magnification factors for semi-elliptical cracks in plate-to-plate butt-welded joints

Author: H. S. Zhao, S. P. Vipin, and Seng-Tjhen Lie
Subjects: Materials science, business.industry, Mechanical Engineering, Butt welding, Magnification, 020101 civil engineering, 02 engineering and technology, Welding, Structural engineering, Bending, Finite element method, 0201 civil engineering, law.invention, 020303 mechanical engineering & transports, 0203 mechanical engineering, Mechanics of Materials, law, Percentage difference, General Materials Science, business
Abstract: British Standard 7910:2013 includes a single set of equations for estimating the weld toe magnification factor (Mk) of different types of welded joints with a semi-elliptical surface crack. In this study, extensive finite element analyses are performed to determine the Mk of plate-to-plate butt-welded joints subjected to axial and bending loading. The Mk values at the crack deepest points and the crack ends are determined. It is found that the Mk results of butt welds are different with those of single T-butt joints with percentage difference in values being as high as 63.8% and 97.4% for axial and bending loading cases, respectively. Percentage differences of 60.4% and 358.2% for axial and bending loading cases are observed between butt welds and X-joints. New Mk equations for butt welds are proposed using multiple regression analyses.
Published: 2016

31. Research on the Spatial-temporal Differences and Influencing Factors of Anhui Industrial Environmental Efficiency

Author: H. X. Zhuang, Q. Yu, H. S. Zhao, N. Y. Shen, X. Liu, and Z. Yao
Subjects: business.industry, Environmental resource management, Environmental science, business, Environmental efficiency
Abstract: In order to improve the efficiency of industrial environment in Anhui Province and promote the coordinated development of industrial production and environmental protection, industrial waste water discharge, air particulate matter discharge and solid waste discharge are regarded as undesirable outputs. The model measures the industrial environmental efficiency of 16 prefecture-level cities in Anhui Province from 2013 to 2018, and fully considers the differences between regions; then, based on the analysis of the total factor productivity of the industrial environment, the impact of industrial environmental efficiency in each province is found factor. Finally, through the construction of the Malmquist index model, the spatial-temporal change trend of industrial environmental efficiency in Anhui Province was analyzed. Studies have shown that there is a clear difference in the efficiency of the industrial environment in Anhui Province. The change trend of TFP and TEC is basically the same. TEC is the main influencing factor of TFP. All regions should pay attention to technological innovation, adjust the existing industrial production model, coordinate the relationship between industrial development and resource environmental protection, and gradually improve their own industrial environmental efficiency.
Published: 2020

32. Effects of anodic titanium dioxide nanotubes of different diameters on macrophage secretion and expression of cytokines and chemokines

Author: W. L. Lü, Zhenyu Zhang, Ping Gao, H. S. Zhao, Ningli Wang, and C. Y. Li
Subjects: Chemokine, Cell Line, Mice, Gene expression, Cell Adhesion, Animals, Macrophage, Secretion, Cell Proliferation, Titanium, Nanotubes, biology, Chemistry, Macrophages, technology, industry, and agriculture, Original Articles, Cell Biology, General Medicine, Adhesion, In vitro, Secretory protein, Cell culture, Immunology, biology.protein, Biophysics, Cytokines
Abstract: Objectives To investigate effects of TiO2 nanotubes of different diameters on J744A.1 macrophage behaviour, secretion and expression of pro-inflammatory cytokines and chemokines. Materials and methods Macrophage-like J744A.1 cells were cultured on three types of Ti surface: mechanically polished titanium plus 30 and 80 nm TiO2 nanotube surfaces, for 4, 24 and 48 h. Macrophage adhesion and proliferation were assessed using CCK-8 assay. Levels of pro-inflammatory cytokines (TNF-α, IL-1β and IL-6) and chemokines (MCP-1 and MIP-1α) secreted into the supernatant were measured using the Cytometric Bead Arrays kit. TNF-α, MCP-1 and MIP-1α gene expression were quantitatively analysed by real-time PCR. Results These show that TiO2 nanotube surfaces, especially of 80 nm TiO2 nanotube, benefited macrophage adhesion and proliferation, and reduced protein secretion and mRNA expression of TNF-α, MCP-1 and MIP-1α. IL-1β and IL-6 were undetectable on all the surfaces at all times. Conclusions TiO2 nanotube surfaces, especially of 80 nm TiO2 nanotube, reduced inflammatory response in vitro, which might be part of a basis for rapid osseointegration in implants with TiO2 nanotube surfaces in animal studies.
Published: 2014

33. Effect of SiC whiskers on properties of porous silicon carbide ceramic

Author: Huazhe Yang, H. S. Zhao, Z. Q. Li, K. H. Zhang, and X. X. Liu
Subjects: Diffraction, Materials science, Monocrystalline whisker, Mechanical Engineering, Whiskers, Condensed Matter Physics, chemistry.chemical_compound, Flexural strength, chemistry, Mechanics of Materials, Whisker, visual_art, visual_art.visual_art_medium, Silicon carbide, General Materials Science, Ceramic, Composite material, Porosity
Abstract: The porous SiC ceramics reinforced by silicon carbide whisker were produced by mixing SiC whisker with core–shell structure powder precursor. The surface morphology, phase composition, porosity, mechanical and thermal properties of the products were analysed. The morphology images show that small part of the SiC whiskers are inserted in the holes of SiC matrix, and most of the SiC whiskers are well dispersed in the matrix. The X-ray diffraction (XRD) pattern indicates that the crystalline phase of porous SiC ceramics reinforced by SiC whisker is pure β-SiC. The bending strength of porous SiC ceramics is strengthened by SiC whisker through the reinforcement mechanisms of whisker bridging, crack deflection and pulling-out whisker effect. The influence of addition proportion of SiC whisker on the bending strength was studied. Along with increasing SiC whisker additive, the bending strength of the porous ceramics performs an increasing trend. When the percentage of SiC whisker in the SiC ceramics increases to...
Published: 2014

34. In-orbit Demonstration of X-Ray Pulsar Navigation with the Insight-HXMT Satellite

Author: S. J. Zheng, S. N. Zhang, F. J. Lu, W. B. Wang, Y. Gao, T. P. Li, L. M. Song, M. Y. Ge, D. W. Han, Y. Chen, Y. P. Xu, X. L. Cao, C. Z. Liu, S. Zhang, J. L. Qu, Z. Chang, G. Chen, L. Chen, T. X. Chen, Y. B. Chen, Y. P. Chen, W. Cui, W. W. Cui, J. K. Deng, Y. W. Dong, Y. Y. Du, M. X. Fu, G. H. Gao, H. Gao, M. Gao, Y. D. Gu, J. Guan, C. Gungor, C. C. Guo, W. Hu, Y. Huang, J. Huo, J. F. Ji, S. M. Jia, L. H. Jiang, W. C. Jiang, J. Jin, Y. J. Jin, B. Li, C. K. Li, G. Li, M. S. Li, W. Li, X. Li, X. B. Li, X. F. Li, Y. G. Li, Z. J. Li, Z. W. Li, X. H. Liang, J. Y. Liao, G. Q. Liu, H. W. Liu, S. Z. Liu, X. J. Liu, Y. Liu, Y. N. Liu, B. Lu, X. F. Lu, T. Luo, X. Ma, B. Meng, Y. Nang, J. Y. Nie, G Ou, N. Sai, R. C. Shang, L. Sun, Y. Tan, L. Tao, W. Tao, Y. L. Tuo, G. F. Wang, J. Wang, W. S. Wang, Y. S. Wang, X. Y. Wen, B. B. Wu, M. Wu, G. C. Xiao, S. L. Xiong, H. Xu, L. L. Yan, J. W. Yang, S. Yang, Y. J. Yang, A. M. Zhang, C. L. Zhang, C. M. Zhang, F. Zhang, H. M. Zhang, J. Zhang, Q. Zhang, T. Zhang, W. Zhang, W. C. Zhang, W. Z. Zhang, Y. Zhang, Y. F. Zhang, Y. J. Zhang, Z. Zhang, Z. L. Zhang, H. S. Zhao, J. L. Zhao, X. F. Zhao, Y. Zhu, Y. X. Zhu, and C. L. Zou
Subjects: Physics, High energy, Crab Pulsar, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, 01 natural sciences, law.invention, Telescope, Pulsar, Space and Planetary Science, law, 0103 physical sciences, Satellite, Astrophysics::Earth and Planetary Astrophysics, Orbit (control theory), Astrophysics - Instrumentation and Methods for Astrophysics, 010306 general physics, Observation data, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, X-ray pulsar
Abstract: In this work, we report the in-orbit demonstration of X-ray pulsar navigation with Insight-Hard X-ray Modulation Telescope (Insight-HXMT), which was launched on Jun. 15th, 2017. The new pulsar navigation method 'Significance Enhancement of Pulse-profile with Orbit-dynamics' (SEPO) is adopted to determine the orbit with observations of only one pulsar. In this test, the Crab pulsar is chosen and observed by Insight-HXMT from Aug. 31th to Sept. 5th in 2017. Using the 5-day-long observation data, the orbit of Insight-HXMT is determined successfully with the three telescopes onboard - High Energy X-ray Telescope (HE), Medium Energy X-ray Telescope (ME) and Low Energy X-ray Telescope (LE) - respectively. Combining all the data, the position and velocity of the Insight-HXMT are pinpointed to within 10 km (3 sigma) and 10 m/s (3 sigma), respectively., Accepted by the Astrophysical Journal Supplement
Published: 2019

35. Determination of the number of J/psi events with J/psi -> inclusive decays

Author: J. C. Chen, Z. P. Zheng, M. Bertani, A. Zhemchugov, P. L. Wang, B. Zhong, X. L. Luo, Ling Zhao, Q. Ji, Qingming Ma, D. H. Zhang, Feng Liu, Chang Liu, X. K. Zhou, Y. P. Guo, J. K. C. Leung, Z. Y. He, J. F. Hu, Z. A. Liu, G. X. Sun, W. G. Li, J. B. Jiao, Xie-Yan Song, Yang Yang, T. R. Zhang, Chang-Zheng Yuan, N. Wu, Y. P. Chu, Junguang Lu, C. F. Qiao, M. H. Gu, I. Boyko, Y. Zeng, H. L. Ma, M. Shao, Brent J. Liu, M. Destefanis, W. X. Gong, G. Li, Q. Ouyang, Tao Luo, H. S. Zhao, Q. J. Li, H. M. Liu, G. M. Xu, D. P. Jin, F. F. Jing, X. R. Zhou, J. L. Fu, T. Held, H. J. Lu, D. H. Sun, Z. G. Zhao, Y. X. Yang, X. Cai, Cheng Li, Y. T. Liang, X. W. Zhu, Xian Lun Zhu, X. H. Mo, O. Bondarenko, Q. J. Wang, J. P. Liu, G. S. Varner, R. E. Mitchell, M. N. Achasov, J. X. Zuo, B. Wang, Z. Y. Deng, C. D. Fu, S. H. Zhang, Y. Xu, L. Fava, Michael Werner, H. H. Zhang, Jianping Zheng, Lei Zhao, Y. Z. Sun, N. B. Li, Q Zhao, J. P. Dai, Jie Yu, J. S. Huang, Chunyan Zhu, T. C. Zhao, H. Ye, Guo-Ming Chen, A. Calcaterra, Y. J. Sun, W. L. Yuan, J. L. Ping, Yao Wang, J. G. Zhang, Hang Liu, Wei Li, Z. L. Hou, K. J. Zhu, B. D. Schaefer, H. S. Chen, S. S. Sun, Guangyu Zhao, C. L. Ma, Chun S. J. Pun, Yu-Bin Liu, R. Poling, Shaodan Ma, E. Prencipe, S. G. Wang, S. P. Wen, Y. F. Liang, X. L. Li, M. G. Zhao, H. P. Cheng, X. F. Wang, Huihui Liu, Ka-Yuet Liu, J. G. Messchendorp, X. Q. Li, Zhibing Li, M. R. Shepherd, Feng Xue, Cui Li, Qun-Yao Wang, Yi-Fang Zhao, Y. Ban, Q. A. Malik, J. Zhang, F. F. An, Q. J. Xu, D. H. Wei, Y. Q. Wang, Z. P. Mao, Q. L. Xiu, Hua-Bin Li, G. F. Xu, Y. K. Heng, M. Pelizaeus, M. Kavatsyuk, K. Li, L. Y. Dong, Niklaus Berger, C. S. Ji, Fang Liu, Lei Zhou, H. M. Hu, D. J. Ambrose, C. X. Yu, E. H. Thorndike, X. S. Jiang, H. B. Liu, Sai-Juan Chen, M. Ablikim, J. W. Zhang, A. A. Zafar, Z. J. Xiao, X. H. Zhao, X. P. Xu, B. Huang, L. S. Wang, N. Kalantar-Nayestanaki, M. H. Ye, H. Loehner, Xing Lu, T. Yang, Y. H. Guan, J. Zhong, X. H. Liu, L. Zhang, Y. Zhang, B. S. Zou, H. L. Dai, K. Peters, X. L. Ji, C. L. Luo, I. Denysenko, E. Boger, Yuehong Xie, Wei Wu, J. Zhuang, D. M. Li, L. B. Guo, J. F. Sun, S. X. Du, S. P. Yu, Z. A. Zhu, H. Y. Sheng, L. H. Wu, S. J. Zhao, H. H. Liu, B. Y. Zhang, M. Greco, J. Schulze, Talib Hussain, M. X. Luo, J. C. Li, S. Pacetti, C. Motzko, J. M. Bian, Kun Liu, Shisong Fang, S. L. Olsen, B. X. Zhang, J. Fang, B. X. Yu, Y. Ding, U. Wiedner, L. L. Wang, Y. B. Liu, A. Zallo, X. Y. Zhang, S. Qian, Y. H. Zheng, I. B. Nikolaev, G. R. Lu, W. B. Yan, J. F. Chang, L. G. Xia, H. Mao, G. F. Cao, M. L. Chen, Y. S. Zhu, J. F. Qiu, L. L. Jiang, G. Rong, Zhihao Xu, Chuan Liu, J. Q. Zhang, Joong-Won Park, Zhiqiang Liu, Miao He, Y. M. Zhu, R. G. Ping, Q. An, X. T. Liao, G. Chelkov, X. Q. Hao, H. Xu, F. C. Ma, Zhiyong Zhang, S. X. Wu, K. H. Rashid, Yuanbo Chen, X. Liu, P. Weidenkaff, S. B. Liu, Lei Li, Xueyong Shen, Xiujuan Tang, Daniel P Cronin-Hennessy, X. B. Ji, K. Goetzen, Y. J. Mao, Z. P. Zhang, T. Ma, Zujian Wang, X. N. Li, W. M. Ding, Z. Wu, Y. S. Zhang, C. Geng, Zhi-Jun Sun, Haiping Peng, M. Y. Dong, H. L. Tian, C. J. Tang, K. X. Zhao, Hai Liang, Z. H. An, Yulei Han, B. Spruck, Zhe Sun, Y. B. Chen, J. Z. Zhang, K. Wang, F. Feldbauer, M. Qi, J. K. Becker, Kunlun He, N. Yu. Muchnoi, Kai Liu, Y. H. Zhang, Q. W. Lu, Q. G. Wen, J. Z. Bai, Y. T. Gu, C. Q. Feng, Yang Gao, Z. Y. Wang, B. Q. Wang, Y. Ma, C. P. Shen, R. A. Briere, M. Maggiora, Li Yan, Fu-Hu Liu, L. K. Jia, Z. Ning, S. L. Li, R. B. Ferroli, Feng Li, Y. F. Wang, F. A. Harris, J. H. Zou, X. Y. Ma, Chunmei Zhang, C. H. Li, Z. Jiao, Z. G. Wang, H. Y. Zhang, J. Y. Zhang, J. Min, D. Dedovich, Shouguang Jin, Y. P. Huang, Zhiqing Liu, S. Spataro, Y. P. Lu, G. R. Liao, X. R. Li, D. Toth, W. Gradl, A. Q. Guo, W. Lai, Y. H. Yan, Tao Hu, W. Kuehn, T. J. Min, C. Morales Morales, Z. H. Qin, Z. Xue, M. Lu, X. L. Wang, Xingtao Huang, A. Denig, V. Bytev, Y. Qin, G. M. Huang, J. S. Lange, C. X. Liu, Jingwei Zhao, Y. Yuan, S. H. Zhu, P. L. Liu, X. S. Qin, C. Nicholson, M. Ullrich, X. D. Ruan, F. E. Maas, A. Sarantsev, Y. Nefedov, X. D. Sun, H. X. Yang, Xuantong Zhang, M. Wang, and KVI - Center for Advanced Radiation Technology
Subjects: Physics, Systematic error, Nuclear and High Energy Physics, Electron–positron annihilation, Detector, Monte Carlo method, BESIII, Inclusive events, Astronomy and Astrophysics, J/ψ→, Nuclear physics, BESIII detector, Number of J/ψ events, +inclusive+events%22">J/psi -> inclusive events, number of J/psi events, Instrumentation
Abstract: The number of J/psi events collected with the BESIII detector at the BEPC II from June 12 to July 28, 2009 is determined to be (225.3 +/- 2.8) x 10(6) using J/psi -> inclusive events, where the uncertainty is the systematic error and the statistical one is negligible.
Published: 2012

36. Study of $J/ψ\to p\bar{p}$ and $J/ψ\to n\bar{n}$

Author: BESIII Collaboration, M. Ablikim(Institute of High Energy Physics, Beijing, P. R. China), M. N. Achasov(G.I. Budker Institute of Nuclear Physics SB RAS), D. J. Ambrose(University of Rochester, Rochester, New York, USA), F. F. An(Institute of High Energy Physics, Beijing, P. R. China), Q. An(University of Science and Technology of China, Hefei, P. R. China), Z. H. An(Institute of High Energy Physics, Beijing, P. R. China), J. Z. Bai(Institute of High Energy Physics, Beijing, P. R. China), R. B. Ferroli(INFN Laboratori Nazionali di Frascati, Frascati, Italy), Y. Ban(Peking University, Beijing, P. R. China), J. Becker(Bochum Ruhr-University, Bochum, Germany), N. Berger(Institute of High Energy Physics, Beijing, P. R. China), M. B. Bertani(INFN Laboratori Nazionali di Frascati, Frascati, Italy), J. M. Bian(University of Minnesota, Minneapolis, MN, USA), E. Boger(20, a), O. Bondarenko(KVI/University of Groningen, Groningen, The Netherlands), I. Boyko(Joint Institute for Nuclear Research, Dubna, Russia), R. A. Briere(Carnegie Mellon University, Pittsburgh, PA, USA), V. Bytev(Joint Institute for Nuclear Research, Dubna, Russia), X. Cai(Institute of High Energy Physics, Beijing, P. R. China), A. C. Calcaterra(INFN Laboratori Nazionali di Frascati, Frascati, Italy), G. F. Cao(Institute of High Energy Physics, Beijing, P. R. China), J. F. Chang(Institute of High Energy Physics, Beijing, P. R. China), G. Chelkov(20, a), G. Chen(Institute of High Energy Physics, Beijing, P. R. China), H. S. Chen(Institute of High Energy Physics, Beijing, P. R. China), J. C. Chen(Institute of High Energy Physics, Beijing, P. R. China), M. L. Chen(Institute of High Energy Physics, Beijing, P. R. China), S. J. Chen(Nanjing University, Nanjing, P. R. China), Y. Chen(Institute of High Energy Physics, Beijing, P. R. China), Y. B. Chen(Institute of High Energy Physics, Beijing, P. R. China), H. P. Cheng(Huangshan College, Huangshan, P. R. China), Y. P. Chu(Institute of High Energy Physics, Beijing, P. R. China), D. Cronin-Hennessy(University of Minnesota, Minneapolis, MN, USA), H. L. Dai(Institute of High Energy Physics, Beijing, P. R. China), J. P. Dai(Institute of High Energy Physics, Beijing, P. R. China), D. Dedovich(Joint Institute for Nuclear Research, Dubna, Russia), Z. Y. Deng(Institute of High Energy Physics, Beijing, P. R. China), A. Denig(Johannes Gutenberg University of Mainz, Mainz, Germany), I. Denysenko(20, b), M. Destefanis(University of Turin and INFN, Turin, Italy), W. M. Ding(Shandong University, Jinan, P. R. China), Y. Ding(Liaoning University, Shenyang, P. R. China), L. Y. Dong(Institute of High Energy Physics, Beijing, P. R. China), M. Y. Dong(Institute of High Energy Physics, Beijing, P. R. China), S. X. Du(Zhengzhou University, Zhengzhou, P. R. China), J. Fang(Institute of High Energy Physics, Beijing, P. R. China), S. S. Fang(Institute of High Energy Physics, Beijing, P. R. China), L. Fava(44, c), F. Feldbauer(Bochum Ruhr-University, Bochum, Germany), C. Q. Feng(University of Science and Technology of China, Hefei, P. R. China), C. D. Fu(Institute of High Energy Physics, Beijing, P. R. China), J. L. Fu(Nanjing University, Nanjing, P. R. China), Y. Gao(Tsinghua University, Beijing, P. R. China), C. Geng(University of Science and Technology of China, Hefei, P. R. China), K. Goetzen(GSI Helmholtzcentre for Heavy Ion Research GmbH, Darmstadt, Germany), W. X. Gong(Institute of High Energy Physics, Beijing, P. R. China), W. Gradl(Johannes Gutenberg University of Mainz, Mainz, Germany), M. Greco(University of Turin and INFN, Turin, Italy), M. H. Gu(Institute of High Energy Physics, Beijing, P. R. China), Y. T. Gu(GuangXi University, Nanning, P.R.China), Y. H. Guan(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), A. Q. Guo(Nankai University, Tianjin, P. R. China), L. B. Guo(Nanjing Normal University, Nanjing, P. R. China), Y. P. Guo(Nankai University, Tianjin, P. R. China), Y. L. Han(Institute of High Energy Physics, Beijing, P. R. China), X. Q. Hao(Institute of High Energy Physics, Beijing, P. R. China), F. A. Harris(University of Hawaii, Honolulu, Hawaii, USA), K. L. He(Institute of High Energy Physics, Beijing, P. R. China), M. He(Institute of High Energy Physics, Beijing, P. R. China), Z. Y. He(Nankai University, Tianjin, P. R. China), T. Held(Bochum Ruhr-University, Bochum, Germany), Y. K. Heng(Institute of High Energy Physics, Beijing, P. R. China), Z. L. Hou(Institute of High Energy Physics, Beijing, P. R. China), H. M. Hu(Institute of High Energy Physics, Beijing, P. R. China), J. F. Hu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), T. Hu(Institute of High Energy Physics, Beijing, P. R. China), B. Huang(Institute of High Energy Physics, Beijing, P. R. China), G. M. Huang(Huazhong Normal University, Wuhan, P. R. China), J. S. Huang(Henan Normal University, Xinxiang, P. R. China), X. T. Huang(Shandong University, Jinan, P. R. China), Y. P. Huang(Institute of High Energy Physics, Beijing, P. R. China), T. Hussain(University of the Punjab, Lahore, Pakistan), C. S. Ji(University of Science and Technology of China, Hefei, P. R. China), Q. Ji(Institute of High Energy Physics, Beijing, P. R. China), X. B. Ji(Institute of High Energy Physics, Beijing, P. R. China), X. L. Ji(Institute of High Energy Physics, Beijing, P. R. China), L. K. Jia(Institute of High Energy Physics, Beijing, P. R. China), L. L. Jiang(Institute of High Energy Physics, Beijing, P. R. China), X. S. Jiang(Institute of High Energy Physics, Beijing, P. R. China), J. B. Jiao(Shandong University, Jinan, P. R. China), Z. Jiao(Huangshan College, Huangshan, P. R. China), D. P. Jin(Institute of High Energy Physics, Beijing, P. R. China), S. Jin(Institute of High Energy Physics, Beijing, P. R. China), F. F. Jing(Tsinghua University, Beijing, P. R. China), N. Kalantar-Nayestanaki(KVI/University of Groningen, Groningen, The Netherlands), M. Kavatsyuk(KVI/University of Groningen, Groningen, The Netherlands), W. Kuehn(Universitaet Giessen, Giessen, Germany), W. Lai(Institute of High Energy Physics, Beijing, P. R. China), J. S. Lange(Universitaet Giessen, Giessen, Germany), J. K. C. Leung(The University of Hong Kong, Pokfulam, Hong Kong), C. H. Li(Institute of High Energy Physics, Beijing, P. R. China), Cheng Li(University of Science and Technology of China, Hefei, P. R. China), Cui Li(University of Science and Technology of China, Hefei, P. R. China), D. M. Li(Zhengzhou University, Zhengzhou, P. R. China), F. Li(Institute of High Energy Physics, Beijing, P. R. China), G. Li(Institute of High Energy Physics, Beijing, P. R. China), H. B. Li(Institute of High Energy Physics, Beijing, P. R. China), J. C. Li(Institute of High Energy Physics, Beijing, P. R. China), K. Li(Hangzhou Normal University, Hangzhou, P. R. China), Lei Li(Institute of High Energy Physics, Beijing, P. R. China), N. B. Li(Nanjing Normal University, Nanjing, P. R. China), Q. J. Li(Institute of High Energy Physics, Beijing, P. R. China), S. L. Li(Institute of High Energy Physics, Beijing, P. R. China), W. D. Li(Institute of High Energy Physics, Beijing, P. R. China), W. G. Li(Institute of High Energy Physics, Beijing, P. R. China), X. L. Li(Shandong University, Jinan, P. R. China), X. N. Li(Institute of High Energy Physics, Beijing, P. R. China), X. Q. Li(Nankai University, Tianjin, P. R. China), X. R. Li(Seoul National University, Seoul, Korea), Z. B. Li(Sun Yat-Sen University, Guangzhou, P. R. China), H. Liang(University of Science and Technology of China, Hefei, P. R. China), Y. F. Liang(Sichuan University, Chengdu, P. R. China), Y. T. Liang(Universitaet Giessen, Giessen, Germany), G. R. Liao(Tsinghua University, Beijing, P. R. China), X. T. Liao(Institute of High Energy Physics, Beijing, P. R. China), B. J. Liu(Institute of High Energy Physics, Beijing, P. R. China), C. L. Liu(Carnegie Mellon University, Pittsburgh, PA, USA), C. X. Liu(Institute of High Energy Physics, Beijing, P. R. China), C. Y. Liu(Institute of High Energy Physics, Beijing, P. R. China), F. H. Liu(Shanxi University, Taiyuan, P. R. China), Fang Liu(Institute of High Energy Physics, Beijing, P. R. China), Feng Liu(Huazhong Normal University, Wuhan, P. R. China), H. Liu(Shanxi University, Taiyuan, P. R. China), H. B. Liu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), H. H. Liu(Henan University of Science and Technology, Luoyang, P. R. China), H. M. Liu(Institute of High Energy Physics, Beijing, P. R. China), H. W. Liu(Institute of High Energy Physics, Beijing, P. R. China), J. P. Liu(Wuhan University, Wuhan, P. R. China), Kun Liu(Peking University, Beijing, P. R. China), Kai Liu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), K. Y. Liu(Liaoning University, Shenyang, P. R. China), P. L. Liu(Shandong University, Jinan, P. R. China), S. B. Liu(University of Science and Technology of China, Hefei, P. R. China), X. Liu(Institute of High Energy Physics, Beijing, P. R. China), X. H. Liu(Institute of High Energy Physics, Beijing, P. R. China), Y. B. Liu(Nankai University, Tianjin, P. R. China), Y. Liu(Institute of High Energy Physics, Beijing, P. R. China), Z. A. Liu(Institute of High Energy Physics, Beijing, P. R. China), Zhiqiang Liu(Institute of High Energy Physics, Beijing, P. R. China), Zhiqing Liu(Institute of High Energy Physics, Beijing, P. R. China), H. Loehner(KVI/University of Groningen, Groningen, The Netherlands), G. R. Lu(Henan Normal University, Xinxiang, P. R. China), H. J. Lu(Huangshan College, Huangshan, P. R. China), J. G. Lu(Institute of High Energy Physics, Beijing, P. R. China), Q. W. Lu(Shanxi University, Taiyuan, P. R. China), X. R. Lu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), Y. P. Lu(Institute of High Energy Physics, Beijing, P. R. China), C. L. Luo(Nanjing Normal University, Nanjing, P. R. China), M. X. Luo(Zhejiang University, Hangzhou, P. R. China), T. Luo(University of Hawaii, Honolulu, Hawaii, USA), X. L. Luo(Institute of High Energy Physics, Beijing, P. R. China), M. Lv(Institute of High Energy Physics, Beijing, P. R. China), C. L. Ma(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), F. C. Ma(Liaoning University, Shenyang, P. R. China), H. L. Ma(Institute of High Energy Physics, Beijing, P. R. China), Q. M. Ma(Institute of High Energy Physics, Beijing, P. R. China), S. Ma(Institute of High Energy Physics, Beijing, P. R. China), T. Ma(Institute of High Energy Physics, Beijing, P. R. China), X. Y. Ma(Institute of High Energy Physics, Beijing, P. R. China), Y. Ma(Institute of High Energy Physics, Beijing, P. R. China), F. E. Maas(Helmholtz Institute Mainz, Mainz, Germany), M. Maggiora(University of Turin and INFN, Turin, Italy), Q. A. Malik(University of the Punjab, Lahore, Pakistan), H. Mao(Institute of High Energy Physics, Beijing, P. R. China), Y. J. Mao(Peking University, Beijing, P. R. China), Z. P. Mao(Institute of High Energy Physics, Beijing, P. R. China), J. G. Messchendorp(KVI/University of Groningen, Groningen, The Netherlands), J. Min(Institute of High Energy Physics, Beijing, P. R. China), T. J. Min(Institute of High Energy Physics, Beijing, P. R. China), R. E. Mitchell(Indiana University, Bloomington, Indiana, USA), X. H. Mo(Institute of High Energy Physics, Beijing, P. R. China), C. Morales Morales(Helmholtz Institute Mainz, Mainz, Germany), C. Motzko(Bochum Ruhr-University, Bochum, Germany), N. Yu. Muchnoi(G.I. Budker Institute of Nuclear Physics SB RAS), Y. Nefedov(Joint Institute for Nuclear Research, Dubna, Russia), C. Nicholson(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), I. B. Nikolaev(G.I. Budker Institute of Nuclear Physics SB RAS), Z. Ning(Institute of High Energy Physics, Beijing, P. R. China), S. L. Olsen(Seoul National University, Seoul, Korea), Q. Ouyang(Institute of High Energy Physics, Beijing, P. R. China), S. P. Pacetti(18, d), J. W. Park(Seoul National University, Seoul, Korea), M. Pelizaeus(University of Hawaii, Honolulu, Hawaii, USA), K. Peters(GSI Helmholtzcentre for Heavy Ion Research GmbH, Darmstadt, Germany), J. L. Ping(Nanjing Normal University, Nanjing, P. R. China), R. G. Ping(Institute of High Energy Physics, Beijing, P. R. China), R. Poling(University of Minnesota, Minneapolis, MN, USA), E. Prencipe(Johannes Gutenberg University of Mainz, Mainz, Germany), C. S. J. Pun(The University of Hong Kong, Pokfulam, Hong Kong), M. Qi(Nanjing University, Nanjing, P. R. China), S. Qian(Institute of High Energy Physics, Beijing, P. R. China), C. F. Qiao(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), X. S. Qin(Institute of High Energy Physics, Beijing, P. R. China), Y. Qin(Peking University, Beijing, P. R. China), Z. H. Qin(Institute of High Energy Physics, Beijing, P. R. China), J. F. Qiu(Institute of High Energy Physics, Beijing, P. R. China), K. H. Rashid(University of the Punjab, Lahore, Pakistan), G. Rong(Institute of High Energy Physics, Beijing, P. R. China), X. D. Ruan(GuangXi University, Nanning, P.R.China), A. Sarantsev(20, e), J. Schulze(Bochum Ruhr-University, Bochum, Germany), M. Shao(University of Science and Technology of China, Hefei, P. R. China), C. P. Shen(38, f), X. Y. Shen(Institute of High Energy Physics, Beijing, P. R. China), H. Y. Sheng(Institute of High Energy Physics, Beijing, P. R. China), M. R. Shepherd(Indiana University, Bloomington, Indiana, USA), X. Y. Song(Institute of High Energy Physics, Beijing, P. R. China), S. Spataro(University of Turin and INFN, Turin, Italy), B. Spruck(Universitaet Giessen, Giessen, Germany), D. H. Sun(Institute of High Energy Physics, Beijing, P. R. China), G. X. Sun(Institute of High Energy Physics, Beijing, P. R. China), J. F. Sun(Henan Normal University, Xinxiang, P. R. China), S. S. Sun(Institute of High Energy Physics, Beijing, P. R. China), X. D. Sun(Institute of High Energy Physics, Beijing, P. R. China), Y. J. Sun(University of Science and Technology of China, Hefei, P. R. China), Y. Z. Sun(Institute of High Energy Physics, Beijing, P. R. China), Z. J. Sun(Institute of High Energy Physics, Beijing, P. R. China), Z. T. Sun(University of Science and Technology of China, Hefei, P. R. China), C. J. Tang(Sichuan University, Chengdu, P. R. China), X. Tang(Institute of High Energy Physics, Beijing, P. R. China), E. H. Thorndike(University of Rochester, Rochester, New York, USA), H. L. Tian(Institute of High Energy Physics, Beijing, P. R. China), D. Toth(University of Minnesota, Minneapolis, MN, USA), M. U. Ulrich(Universitaet Giessen, Giessen, Germany), G. S. Varner(University of Hawaii, Honolulu, Hawaii, USA), B. Wang(GuangXi University, Nanning, P.R.China), B. Q. Wang(Peking University, Beijing, P. R. China), K. Wang(Institute of High Energy Physics, Beijing, P. R. China), L. L. Wang(China Center of Advanced Science and Technology, Beijing, P. R. China), L. S. Wang(Institute of High Energy Physics, Beijing, P. R. China), M. Wang(Shandong University, Jinan, P. R. China), P. Wang(Institute of High Energy Physics, Beijing, P. R. China), P. L. Wang(Institute of High Energy Physics, Beijing, P. R. China), Q. Wang(Peking University, Beijing, P. R. China), Q. J. Wang(Institute of High Energy Physics, Beijing, P. R. China), S. G. Wang(Peking University, Beijing, P. R. China), X. F. Wang(Henan Normal University, Xinxiang, P. R. China), X. L. Wang(University of Science and Technology of China, Hefei, P. R. China), Y. D. Wang(University of Science and Technology of China, Hefei, P. R. China), Y. F. Wang(Institute of High Energy Physics, Beijing, P. R. China), Y. Q. Wang(Shandong University, Jinan, P. R. China), Z. Wang(Institute of High Energy Physics, Beijing, P. R. China), Z. G. Wang(Institute of High Energy Physics, Beijing, P. R. China), Z. Y. Wang(Institute of High Energy Physics, Beijing, P. R. China), D. H. Wei(Guangxi Normal University, Guilin, P. R. China), P. Weidenkaff(Johannes Gutenberg University of Mainz, Mainz, Germany), Q. G. Wen(University of Science and Technology of China, Hefei, P. R. China), S. P. Wen(Institute of High Energy Physics, Beijing, P. R. China), M. W. Werner(Universitaet Giessen, Giessen, Germany), U. Wiedner(Bochum Ruhr-University, Bochum, Germany), L. H. Wu(Institute of High Energy Physics, Beijing, P. R. China), N. Wu(Institute of High Energy Physics, Beijing, P. R. China), S. X. Wu(University of Science and Technology of China, Hefei, P. R. China), W. Wu(Nankai University, Tianjin, P. R. China), Z. Wu(Institute of High Energy Physics, Beijing, P. R. China), L. G. Xia(Tsinghua University, Beijing, P. R. China), Z. J. Xiao(Nanjing Normal University, Nanjing, P. R. China), Y. G. Xie(Institute of High Energy Physics, Beijing, P. R. China), Q. L. Xiu(Institute of High Energy Physics, Beijing, P. R. China), G. F. Xu(Institute of High Energy Physics, Beijing, P. R. China), G. M. Xu(Peking University, Beijing, P. R. China), H. Xu(Institute of High Energy Physics, Beijing, P. R. China), Q. J. Xu(Hangzhou Normal University, Hangzhou, P. R. China), X. P. Xu(Soochow University, Suzhou, China), Y. Xu(Nankai University, Tianjin, P. R. China), Z. R. Xu(University of Science and Technology of China, Hefei, P. R. China), F. Xue(Huazhong Normal University, Wuhan, P. R. China), Z. Xue(Institute of High Energy Physics, Beijing, P. R. China), L. Yan(University of Science and Technology of China, Hefei, P. R. China), W. B. Yan(University of Science and Technology of China, Hefei, P. R. China), Y. H. Yan(Hunan University, Changsha, P. R. China), H. X. Yang(Institute of High Energy Physics, Beijing, P. R. China), T. Yang(GuangXi University, Nanning, P.R.China), Y. Yang(Huazhong Normal University, Wuhan, P. R. China), Y. X. Yang(Guangxi Normal University, Guilin, P. R. China), H. Ye(Institute of High Energy Physics, Beijing, P. R. China), M. Ye(Institute of High Energy Physics, Beijing, P. R. China), M. H. Ye(China Center of Advanced Science and Technology, Beijing, P. R. China), B. X. Yu(Institute of High Energy Physics, Beijing, P. R. China), C. X. Yu(Nankai University, Tianjin, P. R. China), J. S. Yu(Lanzhou University, Lanzhou, P. R. China), S. P. Yu(Shandong University, Jinan, P. R. China), C. Z. Yuan(Institute of High Energy Physics, Beijing, P. R. China), W. L. Yuan(Nanjing Normal University, Nanjing, P. R. China), Y. Yuan(Institute of High Energy Physics, Beijing, P. R. China), A. A. Zafar(University of the Punjab, Lahore, Pakistan), A. Z. Zallo(INFN Laboratori Nazionali di Frascati, Frascati, Italy), Y. Zeng(Hunan University, Changsha, P. R. China), B. X. Zhang(Institute of High Energy Physics, Beijing, P. R. China), B. Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), C. C. Zhang(Institute of High Energy Physics, Beijing, P. R. China), D. H. Zhang(Institute of High Energy Physics, Beijing, P. R. China), H. H. Zhang(Sun Yat-Sen University, Guangzhou, P. R. China), H. Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. Zhang(Nanjing Normal University, Nanjing, P. R. China), J. G. Zhang(Henan Normal University, Xinxiang, P. R. China), J. Q. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. W. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. Z. Zhang(Institute of High Energy Physics, Beijing, P. R. China), L. Zhang(Nanjing University, Nanjing, P. R. China), S. H. Zhang(Institute of High Energy Physics, Beijing, P. R. China), T. R. Zhang(Nanjing Normal University, Nanjing, P. R. China), X. J. Zhang(Institute of High Energy Physics, Beijing, P. R. China), X. Y. Zhang(Shandong University, Jinan, P. R. China), Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), Y. H. Zhang(Institute of High Energy Physics, Beijing, P. R. China), Y. S. Zhang(GuangXi University, Nanning, P.R.China), Z. P. Zhang(University of Science and Technology of China, Hefei, P. R. China), Z. Y. Zhang(Wuhan University, Wuhan, P. R. China), G. Zhao(Institute of High Energy Physics, Beijing, P. R. China), H. S. Zhao(Institute of High Energy Physics, Beijing, P. R. China), J. W. Zhao(Institute of High Energy Physics, Beijing, P. R. China), K. X. Zhao(Nanjing Normal University, Nanjing, P. R. China), Lei Zhao(University of Science and Technology of China, Hefei, P. R. China), Ling Zhao(Institute of High Energy Physics, Beijing, P. R. China), M. G. Zhao(Nankai University, Tianjin, P. R. China), Q. Zhao(Institute of High Energy Physics, Beijing, P. R. China), S. J. Zhao(Zhengzhou University, Zhengzhou, P. R. China), T. C. Zhao(Institute of High Energy Physics, Beijing, P. R. China), X. H. Zhao(Nanjing University, Nanjing, P. R. China), Y. B. Zhao(Institute of High Energy Physics, Beijing, P. R. China), Z. G. Zhao(University of Science and Technology of China, Hefei, P. R. China), A. Zhemchugov(20, a), B. Zheng(University of South China, Hengyang, P. R. China), J. P. Zheng(Institute of High Energy Physics, Beijing, P. R. China), Y. H. Zheng(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), Z. P. Zheng(Institute of High Energy Physics, Beijing, P. R. China), B. Zhong(Institute of High Energy Physics, Beijing, P. R. China), J. Zhong(Bochum Ruhr-University, Bochum, Germany), L. Zhou(Institute of High Energy Physics, Beijing, P. R. China), X. K. Zhou(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), X. R. Zhou(University of Science and Technology of China, Hefei, P. R. China), C. Zhu(Institute of High Energy Physics, Beijing, P. R. China), K. Zhu(Institute of High Energy Physics, Beijing, P. R. China), K. J. Zhu(Institute of High Energy Physics, Beijing, P. R. China), S. H. Zhu(Institute of High Energy Physics, Beijing, P. R. China), X. L. Zhu(Tsinghua University, Beijing, P. R. China), X. W. Zhu(Institute of High Energy Physics, Beijing, P. R. China), Y. M. Zhu(Nankai University, Tianjin, P. R. China), Y. S. Zhu(Institute of High Energy Physics, Beijing, P. R. China), Z. A. Zhu(Institute of High Energy Physics, Beijing, P. R. China), J. Zhuang(Institute of High Energy Physics, Beijing, P. R. China), B. S. Zou(Institute of High Energy Physics, Beijing, P. R. China), J. H. Zou(Institute of High Energy Physics, Beijing, P. R. China), and J. X. Zuo(Institute of High Energy Physics, Beijing, P. R. China)
Subjects: hep-ex, Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: The decays $J/\psi\to p\bar{p}$ and $J/\psi\to n\bar{n}$ have been investigated with a sample of 225.2 million $J/\psi$ events collected with the BESIII detector at the BEPCII $e^+e^-$ collider. The branching fractions are determined to be $\mathcal{B}(J/\psi\to p\bar{p})=(2.112\pm0.004\pm0.031)\times10^{-3}$ and $\mathcal{B}(J/\psi\to n\bar{n})=(2.07\pm0.01\pm0.17)\times10^{-3}$. Distributions of the angle $\theta$ between the proton or anti-neutron and the beam direction are well described by the form $1+\alpha\cos^2\theta$, and we find $\alpha=0.595\pm0.012\pm0.015$ for $J/\psi\to p\bar{p}$ and $\alpha=0.50\pm0.04\pm0.21$ for $J/\psi\to n\bar{n}$. Our branching-fraction results suggest a large phase angle between the strong and electromagnetic amplitudes describing the $J/\psi\to N\bar{N}$ decay.
Published: 2015

37. Two-photon widths of the $χ_{c0, 2}$ states and helicity analysis for $χ_{c2}\arγγ$}

Author: BESIII Collaboration, M. Ablikim(Institute of High Energy Physics, Beijing, P. R. China), M. N. Achasov(G.I. Budker Institute of Nuclear Physics SB RAS), D. J. Ambrose(University of Rochester, Rochester, New York, USA), F. F. An(Institute of High Energy Physics, Beijing, P. R. China), Q. An(University of Science and Technology of China, Hefei, P. R. China), Z. H. An(Institute of High Energy Physics, Beijing, P. R. China), J. Z. Bai(Institute of High Energy Physics, Beijing, P. R. China), R. B. Ferroli(INFN Laboratori Nazionali di Frascati, Frascati, Italy), Y. Ban(Peking University, Beijing, P. R. China), J. Becker(Bochum Ruhr-University, Bochum, Germany), N. Berger(Institute of High Energy Physics, Beijing, P. R. China), M. B. Bertani(INFN Laboratori Nazionali di Frascati, Frascati, Italy), J. M. Bian(University of Minnesota, Minneapolis, MN, USA), E. Boger(20, a), O. Bondarenko(KVI/University of Groningen, Groningen, The Netherlands), I. Boyko(Joint Institute for Nuclear Research, Dubna, Russia), R. A. Briere(Carnegie Mellon University, Pittsburgh, PA, USA), V. Bytev(Joint Institute for Nuclear Research, Dubna, Russia), X. Cai(Institute of High Energy Physics, Beijing, P. R. China), A. C. Calcaterra(INFN Laboratori Nazionali di Frascati, Frascati, Italy), G. F. Cao(Institute of High Energy Physics, Beijing, P. R. China), J. F. Chang(Institute of High Energy Physics, Beijing, P. R. China), G. Chelkov(20, a), G. Chen(Institute of High Energy Physics, Beijing, P. R. China), H. S. Chen(Institute of High Energy Physics, Beijing, P. R. China), J. C. Chen(Institute of High Energy Physics, Beijing, P. R. China), M. L. Chen(Institute of High Energy Physics, Beijing, P. R. China), S. J. Chen(Nanjing University, Nanjing, P. R. China), Y. Chen(Institute of High Energy Physics, Beijing, P. R. China), Y. B. Chen(Institute of High Energy Physics, Beijing, P. R. China), H. P. Cheng(Huangshan College, Huangshan, P. R. China), Y. P. Chu(Institute of High Energy Physics, Beijing, P. R. China), D. Cronin-Hennessy(University of Minnesota, Minneapolis, MN, USA), H. L. Dai(Institute of High Energy Physics, Beijing, P. R. China), J. P. Dai(Institute of High Energy Physics, Beijing, P. R. China), D. Dedovich(Joint Institute for Nuclear Research, Dubna, Russia), Z. Y. Deng(Institute of High Energy Physics, Beijing, P. R. China), A. Denig(Johannes Gutenberg University of Mainz, Mainz, Germany), I. Denysenko(20, b), M. Destefanis(University of Turin and INFN, Turin, Italy), W. M. Ding(Shandong University, Jinan, P. R. China), Y. Ding(Liaoning University, Shenyang, P. R. China), L. Y. Dong(Institute of High Energy Physics, Beijing, P. R. China), M. Y. Dong(Institute of High Energy Physics, Beijing, P. R. China), S. X. Du(Zhengzhou University, Zhengzhou, P. R. China), J. Fang(Institute of High Energy Physics, Beijing, P. R. China), S. S. Fang(Institute of High Energy Physics, Beijing, P. R. China), L. Fava(44, c), F. Feldbauer(Bochum Ruhr-University, Bochum, Germany), C. Q. Feng(University of Science and Technology of China, Hefei, P. R. China), C. D. Fu(Institute of High Energy Physics, Beijing, P. R. China), J. L. Fu(Nanjing University, Nanjing, P. R. China), Y. Gao(Tsinghua University, Beijing, P. R. China), C. Geng(University of Science and Technology of China, Hefei, P. R. China), K. Goetzen(GSI Helmholtzcentre for Heavy Ion Research GmbH, Darmstadt, Germany), W. X. Gong(Institute of High Energy Physics, Beijing, P. R. China), W. Gradl(Johannes Gutenberg University of Mainz, Mainz, Germany), M. Greco(University of Turin and INFN, Turin, Italy), M. H. Gu(Institute of High Energy Physics, Beijing, P. R. China), Y. T. Gu(GuangXi University, Nanning, P.R.China), Y. H. Guan(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), A. Q. Guo(Nankai University, Tianjin, P. R. China), L. B. Guo(Nanjing Normal University, Nanjing, P. R. China), Y. P. Guo(Nankai University, Tianjin, P. R. China), Y. L. Han(Institute of High Energy Physics, Beijing, P. R. China), X. Q. Hao(Institute of High Energy Physics, Beijing, P. R. China), F. A. Harris(University of Hawaii, Honolulu, Hawaii, USA), K. L. He(Institute of High Energy Physics, Beijing, P. R. China), M. He(Institute of High Energy Physics, Beijing, P. R. China), Z. Y. He(Nankai University, Tianjin, P. R. China), T. Held(Bochum Ruhr-University, Bochum, Germany), Y. K. Heng(Institute of High Energy Physics, Beijing, P. R. China), Z. L. Hou(Institute of High Energy Physics, Beijing, P. R. China), H. M. Hu(Institute of High Energy Physics, Beijing, P. R. China), J. F. Hu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), T. Hu(Institute of High Energy Physics, Beijing, P. R. China), B. Huang(Institute of High Energy Physics, Beijing, P. R. China), G. M. Huang(Huazhong Normal University, Wuhan, P. R. China), J. S. Huang(Henan Normal University, Xinxiang, P. R. China), X. T. Huang(Shandong University, Jinan, P. R. China), Y. P. Huang(Institute of High Energy Physics, Beijing, P. R. China), T. Hussain(University of the Punjab, Lahore, Pakistan), C. S. Ji(University of Science and Technology of China, Hefei, P. R. China), Q. Ji(Institute of High Energy Physics, Beijing, P. R. China), X. B. Ji(Institute of High Energy Physics, Beijing, P. R. China), X. L. Ji(Institute of High Energy Physics, Beijing, P. R. China), L. K. Jia(Institute of High Energy Physics, Beijing, P. R. China), L. L. Jiang(Institute of High Energy Physics, Beijing, P. R. China), X. S. Jiang(Institute of High Energy Physics, Beijing, P. R. China), J. B. Jiao(Shandong University, Jinan, P. R. China), Z. Jiao(Huangshan College, Huangshan, P. R. China), D. P. Jin(Institute of High Energy Physics, Beijing, P. R. China), S. Jin(Institute of High Energy Physics, Beijing, P. R. China), F. F. Jing(Tsinghua University, Beijing, P. R. China), N. Kalantar-Nayestanaki(KVI/University of Groningen, Groningen, The Netherlands), M. Kavatsyuk(KVI/University of Groningen, Groningen, The Netherlands), W. Kuehn(Universitaet Giessen, Giessen, Germany), W. Lai(Institute of High Energy Physics, Beijing, P. R. China), J. S. Lange(Universitaet Giessen, Giessen, Germany), J. K. C. Leung(The University of Hong Kong, Pokfulam, Hong Kong), C. H. Li(Institute of High Energy Physics, Beijing, P. R. China), Cheng Li(University of Science and Technology of China, Hefei, P. R. China), Cui Li(University of Science and Technology of China, Hefei, P. R. China), D. M. Li(Zhengzhou University, Zhengzhou, P. R. China), F. Li(Institute of High Energy Physics, Beijing, P. R. China), G. Li(Institute of High Energy Physics, Beijing, P. R. China), H. B. Li(Institute of High Energy Physics, Beijing, P. R. China), J. C. Li(Institute of High Energy Physics, Beijing, P. R. China), K. Li(Hangzhou Normal University, Hangzhou, P. R. China), Lei Li(Institute of High Energy Physics, Beijing, P. R. China), N. B. Li(Nanjing Normal University, Nanjing, P. R. China), Q. J. Li(Institute of High Energy Physics, Beijing, P. R. China), S. L. Li(Institute of High Energy Physics, Beijing, P. R. China), W. D. Li(Institute of High Energy Physics, Beijing, P. R. China), W. G. Li(Institute of High Energy Physics, Beijing, P. R. China), X. L. Li(Shandong University, Jinan, P. R. China), X. N. Li(Institute of High Energy Physics, Beijing, P. R. China), X. Q. Li(Nankai University, Tianjin, P. R. China), X. R. Li(Seoul National University, Seoul, Korea), Z. B. Li(Sun Yat-Sen University, Guangzhou, P. R. China), H. Liang(University of Science and Technology of China, Hefei, P. R. China), Y. F. Liang(Sichuan University, Chengdu, P. R. China), Y. T. Liang(Universitaet Giessen, Giessen, Germany), G. R. Liao(Tsinghua University, Beijing, P. R. China), X. T. Liao(Institute of High Energy Physics, Beijing, P. R. China), B. J. Liu(Institute of High Energy Physics, Beijing, P. R. China), C. L. Liu(Carnegie Mellon University, Pittsburgh, PA, USA), C. X. Liu(Institute of High Energy Physics, Beijing, P. R. China), C. Y. Liu(Institute of High Energy Physics, Beijing, P. R. China), F. H. Liu(Shanxi University, Taiyuan, P. R. China), Fang Liu(Institute of High Energy Physics, Beijing, P. R. China), Feng Liu(Huazhong Normal University, Wuhan, P. R. China), H. Liu(Shanxi University, Taiyuan, P. R. China), H. B. Liu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), H. H. Liu(Henan University of Science and Technology, Luoyang, P. R. China), H. M. Liu(Institute of High Energy Physics, Beijing, P. R. China), H. W. Liu(Institute of High Energy Physics, Beijing, P. R. China), J. P. Liu(Wuhan University, Wuhan, P. R. China), Kun Liu(Peking University, Beijing, P. R. China), Kai Liu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), K. Y. Liu(Liaoning University, Shenyang, P. R. China), P. L. Liu(Shandong University, Jinan, P. R. China), S. B. Liu(University of Science and Technology of China, Hefei, P. R. China), X. Liu(Institute of High Energy Physics, Beijing, P. R. China), X. H. Liu(Institute of High Energy Physics, Beijing, P. R. China), Y. B. Liu(Nankai University, Tianjin, P. R. China), Y. Liu(Institute of High Energy Physics, Beijing, P. R. China), Z. A. Liu(Institute of High Energy Physics, Beijing, P. R. China), Zhiqiang Liu(Institute of High Energy Physics, Beijing, P. R. China), Zhiqing Liu(Institute of High Energy Physics, Beijing, P. R. China), H. Loehner(KVI/University of Groningen, Groningen, The Netherlands), G. R. Lu(Henan Normal University, Xinxiang, P. R. China), H. J. Lu(Huangshan College, Huangshan, P. R. China), J. G. Lu(Institute of High Energy Physics, Beijing, P. R. China), Q. W. Lu(Shanxi University, Taiyuan, P. R. China), X. R. Lu(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), Y. P. Lu(Institute of High Energy Physics, Beijing, P. R. China), C. L. Luo(Nanjing Normal University, Nanjing, P. R. China), M. X. Luo(Zhejiang University, Hangzhou, P. R. China), T. Luo(University of Hawaii, Honolulu, Hawaii, USA), X. L. Luo(Institute of High Energy Physics, Beijing, P. R. China), M. Lv(Institute of High Energy Physics, Beijing, P. R. China), C. L. Ma(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), F. C. Ma(Liaoning University, Shenyang, P. R. China), H. L. Ma(Institute of High Energy Physics, Beijing, P. R. China), Q. M. Ma(Institute of High Energy Physics, Beijing, P. R. China), S. Ma(Institute of High Energy Physics, Beijing, P. R. China), T. Ma(Institute of High Energy Physics, Beijing, P. R. China), X. Y. Ma(Institute of High Energy Physics, Beijing, P. R. China), Y. Ma(Institute of High Energy Physics, Beijing, P. R. China), F. E. Maas(Helmholtz Institute Mainz, Mainz, Germany), M. Maggiora(University of Turin and INFN, Turin, Italy), Q. A. Malik(University of the Punjab, Lahore, Pakistan), H. Mao(Institute of High Energy Physics, Beijing, P. R. China), Y. J. Mao(Peking University, Beijing, P. R. China), Z. P. Mao(Institute of High Energy Physics, Beijing, P. R. China), J. G. Messchendorp(KVI/University of Groningen, Groningen, The Netherlands), J. Min(Institute of High Energy Physics, Beijing, P. R. China), T. J. Min(Institute of High Energy Physics, Beijing, P. R. China), R. E. Mitchell(Indiana University, Bloomington, Indiana, USA), X. H. Mo(Institute of High Energy Physics, Beijing, P. R. China), C. Morales Morales(Helmholtz Institute Mainz, Mainz, Germany), C. Motzko(Bochum Ruhr-University, Bochum, Germany), N. Yu. Muchnoi(G.I. Budker Institute of Nuclear Physics SB RAS), Y. Nefedov(Joint Institute for Nuclear Research, Dubna, Russia), C. Nicholson(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), I. B. Nikolaev(G.I. Budker Institute of Nuclear Physics SB RAS), Z. Ning(Institute of High Energy Physics, Beijing, P. R. China), S. L. Olsen(Seoul National University, Seoul, Korea), Q. Ouyang(Institute of High Energy Physics, Beijing, P. R. China), S. P. Pacetti(18, d), J. W. Park(Seoul National University, Seoul, Korea), M. Pelizaeus(University of Hawaii, Honolulu, Hawaii, USA), K. Peters(GSI Helmholtzcentre for Heavy Ion Research GmbH, Darmstadt, Germany), J. L. Ping(Nanjing Normal University, Nanjing, P. R. China), R. G. Ping(Institute of High Energy Physics, Beijing, P. R. China), R. Poling(University of Minnesota, Minneapolis, MN, USA), E. Prencipe(Johannes Gutenberg University of Mainz, Mainz, Germany), C. S. J. Pun(The University of Hong Kong, Pokfulam, Hong Kong), M. Qi(Nanjing University, Nanjing, P. R. China), S. Qian(Institute of High Energy Physics, Beijing, P. R. China), C. F. Qiao(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), X. S. Qin(Institute of High Energy Physics, Beijing, P. R. China), Y. Qin(Peking University, Beijing, P. R. China), Z. H. Qin(Institute of High Energy Physics, Beijing, P. R. China), J. F. Qiu(Institute of High Energy Physics, Beijing, P. R. China), K. H. Rashid(University of the Punjab, Lahore, Pakistan), G. Rong(Institute of High Energy Physics, Beijing, P. R. China), X. D. Ruan(GuangXi University, Nanning, P.R.China), A. Sarantsev(20, e), J. Schulze(Bochum Ruhr-University, Bochum, Germany), M. Shao(University of Science and Technology of China, Hefei, P. R. China), C. P. Shen(38, f), X. Y. Shen(Institute of High Energy Physics, Beijing, P. R. China), H. Y. Sheng(Institute of High Energy Physics, Beijing, P. R. China), M. R. Shepherd(Indiana University, Bloomington, Indiana, USA), X. Y. Song(Institute of High Energy Physics, Beijing, P. R. China), S. Spataro(University of Turin and INFN, Turin, Italy), B. Spruck(Universitaet Giessen, Giessen, Germany), D. H. Sun(Institute of High Energy Physics, Beijing, P. R. China), G. X. Sun(Institute of High Energy Physics, Beijing, P. R. China), J. F. Sun(Henan Normal University, Xinxiang, P. R. China), S. S. Sun(Institute of High Energy Physics, Beijing, P. R. China), X. D. Sun(Institute of High Energy Physics, Beijing, P. R. China), Y. J. Sun(University of Science and Technology of China, Hefei, P. R. China), Y. Z. Sun(Institute of High Energy Physics, Beijing, P. R. China), Z. J. Sun(Institute of High Energy Physics, Beijing, P. R. China), Z. T. Sun(University of Science and Technology of China, Hefei, P. R. China), C. J. Tang(Sichuan University, Chengdu, P. R. China), X. Tang(Institute of High Energy Physics, Beijing, P. R. China), E. H. Thorndike(University of Rochester, Rochester, New York, USA), H. L. Tian(Institute of High Energy Physics, Beijing, P. R. China), D. Toth(University of Minnesota, Minneapolis, MN, USA), M. U. Ulrich(Universitaet Giessen, Giessen, Germany), G. S. Varner(University of Hawaii, Honolulu, Hawaii, USA), B. Wang(GuangXi University, Nanning, P.R.China), B. Q. Wang(Peking University, Beijing, P. R. China), K. Wang(Institute of High Energy Physics, Beijing, P. R. China), L. L. Wang(China Center of Advanced Science and Technology, Beijing, P. R. China), L. S. Wang(Institute of High Energy Physics, Beijing, P. R. China), M. Wang(Shandong University, Jinan, P. R. China), P. Wang(Institute of High Energy Physics, Beijing, P. R. China), P. L. Wang(Institute of High Energy Physics, Beijing, P. R. China), Q. Wang(Peking University, Beijing, P. R. China), Q. J. Wang(Institute of High Energy Physics, Beijing, P. R. China), S. G. Wang(Peking University, Beijing, P. R. China), X. F. Wang(Henan Normal University, Xinxiang, P. R. China), X. L. Wang(University of Science and Technology of China, Hefei, P. R. China), Y. D. Wang(University of Science and Technology of China, Hefei, P. R. China), Y. F. Wang(Institute of High Energy Physics, Beijing, P. R. China), Y. Q. Wang(Shandong University, Jinan, P. R. China), Z. Wang(Institute of High Energy Physics, Beijing, P. R. China), Z. G. Wang(Institute of High Energy Physics, Beijing, P. R. China), Z. Y. Wang(Institute of High Energy Physics, Beijing, P. R. China), D. H. Wei(Guangxi Normal University, Guilin, P. R. China), P. Weidenkaff(Johannes Gutenberg University of Mainz, Mainz, Germany), Q. G. Wen(University of Science and Technology of China, Hefei, P. R. China), S. P. Wen(Institute of High Energy Physics, Beijing, P. R. China), M. W. Werner(Universitaet Giessen, Giessen, Germany), U. Wiedner(Bochum Ruhr-University, Bochum, Germany), L. H. Wu(Institute of High Energy Physics, Beijing, P. R. China), N. Wu(Institute of High Energy Physics, Beijing, P. R. China), S. X. Wu(University of Science and Technology of China, Hefei, P. R. China), W. Wu(Nankai University, Tianjin, P. R. China), Z. Wu(Institute of High Energy Physics, Beijing, P. R. China), L. G. Xia(Tsinghua University, Beijing, P. R. China), Z. J. Xiao(Nanjing Normal University, Nanjing, P. R. China), Y. G. Xie(Institute of High Energy Physics, Beijing, P. R. China), Q. L. Xiu(Institute of High Energy Physics, Beijing, P. R. China), G. F. Xu(Institute of High Energy Physics, Beijing, P. R. China), G. M. Xu(Peking University, Beijing, P. R. China), H. Xu(Institute of High Energy Physics, Beijing, P. R. China), Q. J. Xu(Hangzhou Normal University, Hangzhou, P. R. China), X. P. Xu(Soochow University, Suzhou, China), Y. Xu(Nankai University, Tianjin, P. R. China), Z. R. Xu(University of Science and Technology of China, Hefei, P. R. China), F. Xue(Huazhong Normal University, Wuhan, P. R. China), Z. Xue(Institute of High Energy Physics, Beijing, P. R. China), L. Yan(University of Science and Technology of China, Hefei, P. R. China), W. B. Yan(University of Science and Technology of China, Hefei, P. R. China), Y. H. Yan(Hunan University, Changsha, P. R. China), H. X. Yang(Institute of High Energy Physics, Beijing, P. R. China), T. Yang(GuangXi University, Nanning, P.R.China), Y. Yang(Huazhong Normal University, Wuhan, P. R. China), Y. X. Yang(Guangxi Normal University, Guilin, P. R. China), H. Ye(Institute of High Energy Physics, Beijing, P. R. China), M. Ye(Institute of High Energy Physics, Beijing, P. R. China), M. H. Ye(China Center of Advanced Science and Technology, Beijing, P. R. China), B. X. Yu(Institute of High Energy Physics, Beijing, P. R. China), C. X. Yu(Nankai University, Tianjin, P. R. China), J. S. Yu(Lanzhou University, Lanzhou, P. R. China), S. P. Yu(Shandong University, Jinan, P. R. China), C. Z. Yuan(Institute of High Energy Physics, Beijing, P. R. China), W. L. Yuan(Nanjing Normal University, Nanjing, P. R. China), Y. Yuan(Institute of High Energy Physics, Beijing, P. R. China), A. A. Zafar(University of the Punjab, Lahore, Pakistan), A. Z. Zallo(INFN Laboratori Nazionali di Frascati, Frascati, Italy), Y. Zeng(Hunan University, Changsha, P. R. China), B. X. Zhang(Institute of High Energy Physics, Beijing, P. R. China), B. Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), C. C. Zhang(Institute of High Energy Physics, Beijing, P. R. China), D. H. Zhang(Institute of High Energy Physics, Beijing, P. R. China), H. H. Zhang(Sun Yat-Sen University, Guangzhou, P. R. China), H. Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. Zhang(Nanjing Normal University, Nanjing, P. R. China), J. G. Zhang(Henan Normal University, Xinxiang, P. R. China), J. Q. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. W. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), J. Z. Zhang(Institute of High Energy Physics, Beijing, P. R. China), L. Zhang(Nanjing University, Nanjing, P. R. China), S. H. Zhang(Institute of High Energy Physics, Beijing, P. R. China), T. R. Zhang(Nanjing Normal University, Nanjing, P. R. China), X. J. Zhang(Institute of High Energy Physics, Beijing, P. R. China), X. Y. Zhang(Shandong University, Jinan, P. R. China), Y. Zhang(Institute of High Energy Physics, Beijing, P. R. China), Y. H. Zhang(Institute of High Energy Physics, Beijing, P. R. China), Y. S. Zhang(GuangXi University, Nanning, P.R.China), Z. P. Zhang(University of Science and Technology of China, Hefei, P. R. China), Z. Y. Zhang(Wuhan University, Wuhan, P. R. China), G. Zhao(Institute of High Energy Physics, Beijing, P. R. China), H. S. Zhao(Institute of High Energy Physics, Beijing, P. R. China), J. W. Zhao(Institute of High Energy Physics, Beijing, P. R. China), K. X. Zhao(Nanjing Normal University, Nanjing, P. R. China), Lei Zhao(University of Science and Technology of China, Hefei, P. R. China), Ling Zhao(Institute of High Energy Physics, Beijing, P. R. China), M. G. Zhao(Nankai University, Tianjin, P. R. China), Q. Zhao(Institute of High Energy Physics, Beijing, P. R. China), S. J. Zhao(Zhengzhou University, Zhengzhou, P. R. China), T. C. Zhao(Institute of High Energy Physics, Beijing, P. R. China), X. H. Zhao(Nanjing University, Nanjing, P. R. China), Y. B. Zhao(Institute of High Energy Physics, Beijing, P. R. China), Z. G. Zhao(University of Science and Technology of China, Hefei, P. R. China), A. Zhemchugov(20, a), B. Zheng(University of South China, Hengyang, P. R. China), J. P. Zheng(Institute of High Energy Physics, Beijing, P. R. China), Y. H. Zheng(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), Z. P. Zheng(Institute of High Energy Physics, Beijing, P. R. China), B. Zhong(Institute of High Energy Physics, Beijing, P. R. China), J. Zhong(Bochum Ruhr-University, Bochum, Germany), L. Zhou(Institute of High Energy Physics, Beijing, P. R. China), X. K. Zhou(Graduate University of Chinese Academy of Sciences, Beijing, P. R. China), X. R. Zhou(University of Science and Technology of China, Hefei, P. R. China), C. Zhu(Institute of High Energy Physics, Beijing, P. R. China), K. Zhu(Institute of High Energy Physics, Beijing, P. R. China), K. J. Zhu(Institute of High Energy Physics, Beijing, P. R. China), S. H. Zhu(Institute of High Energy Physics, Beijing, P. R. China), X. L. Zhu(Tsinghua University, Beijing, P. R. China), X. W. Zhu(Institute of High Energy Physics, Beijing, P. R. China), Y. M. Zhu(Nankai University, Tianjin, P. R. China), Y. S. Zhu(Institute of High Energy Physics, Beijing, P. R. China), Z. A. Zhu(Institute of High Energy Physics, Beijing, P. R. China), J. Zhuang(Institute of High Energy Physics, Beijing, P. R. China), B. S. Zou(Institute of High Energy Physics, Beijing, P. R. China), J. H. Zou(Institute of High Energy Physics, Beijing, P. R. China), and J. X. Zuo(Institute of High Energy Physics, Beijing, P. R. China)
Subjects: hep-ex, Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Based on a data sample of 106 M $\psi^{\prime}$ events collected with the BESIII detector, the decays $\psi^{\prime}\ar\gamma\chi_{c0, 2}$,$\chi_{c0, 2}\ar\gamma\gamma$ are studied to determine the two-photon widths of the $\chi_{c0, 2}$ states. The two-photon decay branching fractions are determined to be ${\cal B}(\chi_{c0}\ar\gamma\gamma) = (2.24\pm 0.19\pm 0.12\pm 0.08)\times 10^{-4}$ and ${\cal B}(\chi_{c2}\ar\gamma\gamma) = (3.21\pm 0.18\pm 0.17\pm 0.13)\times 10^{-4}$. From these, the two-photon widths are determined to be $\Gamma_{\gamma \gamma}(\chi_{c0}) = (2.33\pm0.20\pm0.13\pm0.17)$ keV, $\Gamma_{\gamma \gamma}(\chi_{c2}) = (0.63\pm0.04\pm0.04\pm0.04)$ keV, and $\cal R$ $=\Gamma_{\gamma \gamma}(\chi_{c2})/\Gamma_{\gamma \gamma}(\chi_{c0})=0.271\pm 0.029\pm 0.013\pm 0.027$, where the uncertainties are statistical, systematic, and those from the PDG ${\cal B}(\psi^{\prime}\ar\gamma\chi_{c0,2})$ and $\Gamma(\chi_{c0,2})$ errors, respectively. The ratio of the two-photon widths for helicity $\lambda=0$ and helicity $\lambda=2$ components in the decay $\chi_{c2}\ar\gamma\gamma$ is measured for the first time to be $f_{0/2} =\Gamma^{\lambda=0}_{\gamma\gamma}(\chi_{c2})/\Gamma^{\lambda=2}_{\gamma\gamma}(\chi_{c2}) = 0.00\pm0.02\pm0.02$.
Published: 2015

38. Hydrothermal deposition of single crystalline germanium nanorods

Author: S. B. Wang, Qian-Feng Zhang, H. Y. Yu, X. L. Xia, Wai Kian Tan, H. S. Zhao, and L. Z. Pei
Subjects: Materials science, Scanning electron microscope, Metals and Alloys, chemistry.chemical_element, Germanium, Nanotechnology, Condensed Matter Physics, Hydrothermal circulation, law.invention, chemistry, Chemical engineering, Transmission electron microscopy, law, Materials Chemistry, Nanorod, Diamond cubic, Physical and Theoretical Chemistry, Electron microscope, High-resolution transmission electron microscopy
Abstract: Single crystalline germanium nanorods have been prepared via a simple hydrothermal deposition process using Ge and GeO2 as the starting materials under the hydrothermal conditions of 400 °C and 7.1 – 8 MPa. Scanning electron microscopy and transmission electron microscopy observations show the diameter of the nanorods ranging from 70 nm to 500 nm and the length greater than 10 μm. X-ray diffraction and high resolution transmission electron microscopy results indicate that the nanorods are mainly composed of single crystalline Ge with cubic diamond structure. The growth process has been proposed as the CuGeO3-assisted growth mechanism.
Published: 2011

39. Insight-HXMT Observations of 4U 1636-536: Corona Cooling Revealed with Single Short Type-I X-Ray Burst

Author: Y. P. Chen, S. Zhang, J. L. Qu, S. N. Zhang, L. Ji, L. D. Kong, X. L. Cao, Z. Chang, G. Chen, L. Chen, T. X. Chen, Y. Chen, Y. B. Chen, W. Cui, W. W. Cui, J. K. Deng, Y. W. Dong, Y. Y. Du, M. X. Fu, G. H. Gao, H. Gao, M. Gao, M. Y. Ge, Y. D. Gu, J. Guan, C. C. Guo, D. W. Han, W. Hu, Y. Huang, J. Huo, S. M. Jia, L. H. Jiang, W. C. Jiang, J. Jin, Y. J. Jin, B. Li, C. K. Li, G. Li, M. S. Li, T. P. Li, W. Li, X. Li, X. B. Li, X. F. Li, Y. G. Li, Z. J. Li, Z. W. Li, X. H. Liang, J. Y. Liao, C. Z. Liu, G. Q. Liu, H. W. Liu, S. Z. Liu, X. J. Liu, Y. Liu, Y. N. Liu, B. Lu, F. J. Lu, X. F. Lu, T. Luo, X. Ma, B. Meng, Y. Nang, J. Y. Nie, G. Ou, N. Sai, L. M. Song, L. Sun, Y. Tan, L. Tao, W. H. Tao, Y. L. Tuo, G. F. Wang, H. Y. Wang, J. Wang, W. S. Wang, Y. S. Wang, X. Y. Wen, B. B. Wu, M. Wu, G. C. Xiao, S. L. Xiong, H. Xu, Y. P. Xu, L. L. Yan, J. W. Yang, S. Yang, Y. J. Yang, A. M. Zhang, C. L. Zhang, C. M. Zhang, F. Zhang, H. M. Zhang, J. Zhang, Q. Zhang, T. Zhang, W. Zhang, W. C. Zhang, W. Z. Zhang, Y. Zhang, Y. F. Zhang, Y. J. Zhang, Z. Zhang, Z. L. Zhang, H. S. Zhao, J. L. Zhao, X. F. Zhao, S. J. Zheng, Y. Zhu, Y. X. Zhu, and C. L. Zou
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Broad bandwidth, Stacking, X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Economic shortage, Astrophysics, 01 natural sciences, Corona, law.invention, Space and Planetary Science, law, 0103 physical sciences, Spectral fitting, Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics, 010303 astronomy & astrophysics, Flare
Abstract: Corona cooling was detected previously from stacking a series of short type-I bursts occurred during the low/had state of atoll outburst. Type-I bursts are hence regarded as sharp probe to our better understanding on the basic property of the corona. The launch of the first Chinese X-ray satellite Insight-HXMT has large detection area at hard X-rays which provide almost unique chance to move further in this research field. We report the first detection of the corona cooling by Insight-HXMT from single short type-I burst showing up during {\bf flare} of 4U 1636-536. This type-I X-ray burst has a duration of $\sim$13 seconds and hard X-ray shortage is detected with significance 6.2~$\sigma$ in 40-70 keV. A cross-correlation analysis between the lightcurves of soft and hard X-ray band, shows that the corona shortage lag the burst emission by 1.6 $\pm$1.2~s. These results are consistent with those derived previously from stacking a large amount of bursts detected by RXTE/PCA within a series of {\bf flares} of 4U 1636-536. Moreover, the broad bandwidth of Insight-HXMT allows as well for the first time to infer the burst influence upon the continuum spectrum via performing the spectral fitting of the burst, which ends up with the finding that hard X-ray shortage appears at around 40 keV in the continuum spectrum. These results suggest that the evolution of the corona along with the outburst{\bf /flare} of NS XRB may be traced via looking into a series of embedded type-I bursts by using Insight-HXMT., Comment: published in 2018, ApJL,864, L30
Published: 2018

40. SYNTHESIS OF TUBULAR <font>Ge</font> NANOSTRUCTURES

Author: H. S. Zhao, H. Y. Yu, J. L. Hu, and L. Z. Pei
Subjects: Nanostructure, Materials science, chemistry.chemical_element, Bioengineering, Germanium, Nanotechnology, Condensed Matter Physics, Hydrothermal circulation, Computer Science Applications, chemistry, Chemical engineering, Transmission electron microscopy, Hydrothermal synthesis, General Materials Science, Lamellar structure, Crystallite, Electrical and Electronic Engineering, High-resolution transmission electron microscopy, Biotechnology
Abstract: Hollow germanium tubular nanostructures have been obtained by a hydrothermal process at a temperature of 400°C and pressure of 7 MPa with quick cooling to room temperature. Transmission electron microscopy (TEM) and high-resolution transmission electron microscopy (HRTEM) show that the germanium tubular nanostructures are polycrystalline and have open-end structures at the tips. The diameter of germanium tubular nanostructures is about 40–70 nm and the inner pore size is about 10 nm in average. We propose the rolling mechanism for the formation of tubular nanostructures from lamellar nanostructures to explain the possible formation process of germanium tubular nanostructures.
Published: 2010

41. Hydrothermal Deposition of Silicon Nanochains

Author: H. Y. Yu, Wai Kian Tan, L. Z. Pei, and H. S. Zhao
Subjects: Morphology (linguistics), Materials science, Silicon, Scanning electron microscope, chemistry.chemical_element, Bioengineering, Nanotechnology, Surfaces and Interfaces, engineering.material, Condensed Matter Physics, Silicon monoxide, Surfaces, Coatings and Films, chemistry.chemical_compound, Polycrystalline silicon, chemistry, Chemical engineering, Mechanics of Materials, Transmission electron microscopy, engineering, Hydrothermal deposition, High-resolution transmission electron microscopy, Biotechnology
Abstract: Si nanochains have been prepared via a simple hydrothermal deposition route using silicon monoxide as the starting material at 300°C. Scanning electron microscopy (SEM), transmission electron microscopy (TEM), energy dispersive spectrum (EDS) and high-resolution transmission electron microscopy (HRTEM) are used to observe the structure and morphology of the products. The obtained Si nanochains are composed of knots and necks with polycrystalline silicon cubic structure. The surface of the Si nanochains is covered with amorphous silica outer layers. The growth mechanism of the Si nanochains is discussed. [DOI: 10.1380/ejssnt.2008.171]
Published: 2008

42. Separation of polysaccharide from wolfberry fruit and determination by infrared spectroscopy based on nonlinear modeling

Author: Z.-T. Xu H.-S. Zhao and H. Zhang
Subjects: chemistry.chemical_classification, Nonlinear system, Chromatography, chemistry, Analytical chemistry, Infrared spectroscopy, Polysaccharide
Published: 2015

43. PTCH Mutations in Sporadic and Gorlin-syndrome-related Odontogenic Keratocysts

Author: H. S. Zhao, L. S. Sun, Xiaomei Gu, and Tie-Jun Li
Subjects: Adult, Male, Patched Receptors, 0301 basic medicine, China, Pathology, medicine.medical_specialty, Adolescent, Ptch gene, DNA Mutational Analysis, Receptors, Cell Surface, Nevoid basal-cell carcinoma syndrome, medicine.disease_cause, Pathogenesis, 03 medical and health sciences, 0302 clinical medicine, Asian People, medicine, Humans, General Dentistry, Mutation, Polymorphism, Genetic, business.industry, Basal Cell Nevus Syndrome, 030206 dentistry, Middle Aged, medicine.disease, Odontogenic, Patched-1 Receptor, stomatognathic diseases, 030104 developmental biology, Odontogenic Cysts, Keratins, Female, business
Abstract: Odontogenic keratocysts are relatively common lesions that may occur in isolation or in association with nevoid basal cell carcinoma syndrome (or Gorlin syndrome). The PTCH gene has been reported to be associated with Gorlin syndrome. We investigated 10 cases of non-syndromic keratocysts and two other cases associated with Gorlin syndrome, looking for PTCH mutations. Four novel and 1 known PTCH mutations were identified in five individual patients. Of the 5 mutations identified, 2 were germ-line mutations (2619C>A; 1338_1339insGCG) in 2 cysts associated with Gorlin syndrome, and 3 were somatic mutations (3124_3129dupGTGTGC; 1361_1364delGTCT; 3913G>T) in 3 non-syndromic cysts. This report describes PTCH mutations in both non-syndromic and Gorlin-syndrome-related odontogenic keratocysts in Chinese patients, and suggests that defects of PTCH are associated with the pathogenesis of syndromic as well as a subset of non-syndromic keratocysts.
Published: 2006

44. Composite films of BaTiO3and PVDF

Author: Weiying Zhong, Peng Zhang, H. S. Zhao, C. S. Fang, and Xia Li
Subjects: Dc field, Materials science, Field (physics), Electric field, Composite number, Figure of merit, Composite material, Condensed Matter Physics, Electronic, Optical and Magnetic Materials, Pyroelectricity
Abstract: BaTiO3+PVDF composite films were prepared with and without DC electric field during the film-forming process. The figure of merit p/e of the films with 10kV/cm field reaches 1.5 × 10−7C/m2K, whereas that of the films without electric field is only 1.2 × 10−8C/m2K. Experiments show that the application of a strong DC field during the film-forming process may rotate the grains so that the c-axes are parallel to the field. The ordered distribution of the grains will enhance the pyroelectricity and improve the aging characteristics of the composite films.
Published: 1997

45. Dielectric properties of Ba1-xSrxTiO3prepared by sag method

Author: Peicong Zhang, X. H. Wang, Weiying Zhong, Luyuan Zhang, H. S. Zhao, D. R. Chen, and J. W. Feng
Subjects: Phase transition, Materials science, Condensed matter physics, Impurity, visual_art, visual_art.visual_art_medium, Dielectric permittivity, Curie temperature, Ceramic, Curie constant, Dielectric, Condensed Matter Physics, Electronic, Optical and Magnetic Materials
Abstract: Ba1-x,SrxTiO3(x=0, 0.3, 0.5 and 0.7) were synthesized by the SAG method. XRD revealed a cubic structure at room temperature. From the temperature dependence of the dielectric permittivity, the Curie temperature was measured. Although it decreases linearly with increasing x, it is obviously lower than that of the ceramics made by traditional method. The lowering of Curie temperature and disappearance of the trigonal-orthorhombic and orthorhombic-tetragonal phase transitions might be caused by the impurity Fe3+ and the excess of Ba at the grain surface
Published: 1997

46. Study of polar glass-ceramics containing crystalline SrTiO3

Author: H. S. Zhao, Weiying Zhong, Xia Li, Luyuan Zhang, Peicong Zhang, W. M. Xie, and Z. Y. Ding
Subjects: Structural phase, Materials science, business.industry, Dielectric, Atmospheric temperature range, Condensed Matter Physics, Electronic, Optical and Magnetic Materials, Pyroelectricity, Optics, visual_art, visual_art.visual_art_medium, Polar, Ceramic, Crystallite, Composite material, business
Abstract: A polar glass-ceramic with crystallites Sr2TiSi2O8 and SrTiO3 is prepared. The dielectric and pyroelectric properties are studied in the temperature range from 10 to 300K. The pyroelectric coefficient is negative above 40K and becomes positive below this temperature. The sign-change of pyroelectric coefficient is ascribed to the structural phase transition of SrTiO3.
Published: 1997

47. Observation of Two NewN*Resonances in the Decayψ(3686)→pp¯π0

Author: S. J. Zhao, Zheng Wang, J. S. Lange, S. G. Wang, Jingwei Zhao, C. X. Yu, L. L. Wang, X. Y. Zhang, X. S. Jiang, H. B. Liu, B. S. Zou, J. F. Sun, Xingtao Huang, A. Denig, V. Bytev, Y. X. Yang, Y. Yuan, X. H. Mo, Q. J. Wang, J. P. Liu, Jianping Zheng, W. Gradl, M. L. Chen, J. L. Fu, H. Mao, Y. Qin, H. H. Zhang, Y. Z. Sun, T. C. Zhao, J. L. Ping, W. L. Yuan, P. Weidenkaff, S. H. Zhu, S. H. Zhang, Zhenyu Zhang, W. Lai, X. L. Ji, Zhiqiang Liu, Miao He, Q. An, P. L. Liu, M. Lv, J. G. Zhang, R. G. Ping, C. L. Ma, Daniel P Cronin-Hennessy, C. S. Ji, R. Poling, W. Kühn, P. Wang, T. Yang, S. X. Wu, I. Denysenko, E. Boger, S. Pacetti, B. X. Yu, Jianhao Zhang, Xiujuan Tang, Jie Yu, Guo-Ming Chen, Tao Hu, Lei Zhao, X. Q. Hao, Y. H. Yan, Wu Li, Jin Wang, Z. L. Hou, G. Rong, Xing Lu, J. Zhong, T. J. Min, Y. M. Zhu, X. R. Zhou, J. S. Huang, Z. J. Xiao, Z. H. An, B. Spruck, K. H. Rashid, L. Y. Dong, Niklaus Berger, E. Prencipe, S. P. Wen, Y. F. Liang, X. Liu, Z. H. Qin, M. Shao, Z. T. Sun, C. Morales Morales, R. E. Mitchell, Y. P. Guo, J. K. C. Leung, F. Feldbauer, X. S. Qin, Chang-Zheng Yuan, C. Nicholson, M. Y. Dong, X. L. Li, G. X. Sun, J. B. Jiao, Y. P. Chu, Junguang Lu, C. F. Qiao, Z. G. Zhao, M. R. Shepherd, Feng Xue, Cui Li, Y. T. Liang, J. Fang, B. Zheng, S. Spataro, M. Ullrich, M. Pelizaeus, X. D. Ruan, J. F. Chang, G. F. Cao, Y. J. Sun, D. H. Sun, Hua-Bin Li, M. Qi, Wei Li, X. L. Wang, J. K. Becker, Xu Zhang, Hao Liu, S. S. Sun, F. F. An, J. P. Dai, Y. H. Guan, X. H. Liu, J. C. Chen, Xie-Yan Song, J. Zhang, Ling Zhao, Guangyu Zhao, Hai Liang, Z. Y. He, Z. Xue, M. Kavatsyuk, Y. P. Lu, Kun Liu, Fang Liu, C. L. Luo, Lei Zhou, G. R. Liao, A. Zhemchugov, Yang Yang, Yulei Han, Li-Feng Wang, Y. K. Heng, D. Toth, Chunyan Zhu, Sai-Juan Chen, D. H. Zhang, Yang Gao, Shisong Fang, Yuehong Xie, Wei Wu, K. Peters, Kunlun He, Q. Ouyang, Q. J. Li, J. F. Hu, Z. P. Mao, G. M. Xu, Kai Liu, Z. A. Liu, G. S. Varner, M. Bertani, Z. Ning, H. Y. Zhang, Haiwen Liu, X. H. Zhao, B. Zhong, Yong’an Liu, S. P. Yu, Shaodan Ma, X. T. Liao, A. Zallo, L. G. Xia, Qingming Ma, Kai Zhu, R. A. Briere, Feng Liu, Chang Liu, Y. S. Zhu, J. F. Qiu, H. Xu, X. P. Xu, F. C. Ma, G. M. Huang, J. Min, Chun S. J. Pun, D. Dedovich, T. R. Zhang, M. H. Gu, O. Bondarenko, D. J. Ambrose, J. Z. Bai, Y. T. Gu, M. G. Zhao, Y. J. Mao, D. M. Li, Shouguang Jin, Qian Wang, Y. P. Huang, G. Li, Y. D. Wang, X. N. Li, X. F. Wang, Zhen Wang, M. Ye, Huihui Liu, C. Motzko, C. Geng, L. Fava, Tao Luo, Xian Lun Zhu, S. L. Olsen, Li Yan, Talib Hussain, J. G. Messchendorp, G. R. Lu, C. D. Fu, A. Calcaterra, Q. L. Xiu, Jiangchao Li, Yi-Fang Zhao, Fu-Hu Liu, L. Zhang, H. S. Chen, Zong-Ping Zheng, H. Loehner, Joong-Won Park, Y. H. Zheng, W. B. Yan, H. L. Dai, J. Zhuang, S. X. Du, L. L. Jiang, Jun-Yi Zhang, G. F. Xu, L. H. Wu, M. X. Luo, G. Chelkov, B. X. Zhang, I. B. Nikolaev, Xueyong Shen, Zujian Wang, Y. S. Zhang, Xiaobo Zhu, Zhi-Jun Sun, Zhihao Xu, Chuan Liu, J. Schulze, J. M. Bian, N. Yu. Muchnoi, F. F. Jing, Y. H. Zhang, Q. W. Lu, K. Li, B. Huang, N. Kalantar-Nayestanaki, Y. Ding, E. H. Thorndike, Q. G. Wen, S. Qian, M. Maggiora, Bingxin Zhang, M. N. Achasov, J. X. Zuo, H. Y. Sheng, M. Greco, S. B. Liu, U. Wiedner, Lei Li, L. K. Jia, Z. P. Zhang, YongJu Chen, T. Ma, Jianguo Zhang, M. H. Ye, Yun-Zhi Zhang, H. P. Cheng, Y. Q. Wang, Z. A. Zhu, M. Ablikim, A. A. Zafar, X. B. Ji, K. Goetzen, Q. Ji, W. M. Ding, N. Wu, Feng Li, D. P. Jin, Y. F. Wang, F. A. Harris, B. Wang, Z. Y. Deng, Michael Werner, X. Y. Ma, Hang Liu, Chunmei Zhang, Q. J. Xu, D. H. Wei, C. H. Li, X. Q. Li, H. M. Hu, Hailong Ma, L. B. Guo, Z. Wu, Y. B. Chen, J. Z. Zhang, Y. B. Liu, K. Y. Liu, H. L. Tian, C. J. Tang, K. X. Zhao, K. Wang, P. L. Wang, X. L. Luo, C. Q. Feng, X. K. Zhou, B. Q. Wang, Y. Ma, H. S. Zhao, C. P. Shen, T. Held, H. J. Lu, Cunming Liu, I. Boyko, Y. Xu, N. B. Li, Y. Zeng, Q Zhao, H. Ye, Brent J. Liu, M. Destefanis, W. X. Gong, Zhibing Li, Y. Ban, Q. A. Malik, Zhiqing Liu, F. E. Maas, Cheng Li, A. Sarantsev, Y. Nefedov, X. D. Sun, H. X. Yang, K. J. Zhu, M. Wang, X. R. Li, A. Q. Guo, Z. Jiao, S. L. Li, R. B. Ferroli, J. H. Zou, and X. Cai
Subjects: Baryon, Nuclear physics, Physics, Branching fraction, Electron–positron annihilation, Partial wave analysis, Analytical chemistry, General Physics and Astronomy, Resonance, Bar (unit)
Abstract: Based on 106 x 10(6)psi(3686) events collected with the BESIII detector at the BEPCII facility, a partial wave analysis of psi(3686) -> p (p) over bar pi(0) is performed. The branching fraction of this channel has been determined to be B psi(3686) -> p (p) over bar pi(0) = (1.65 +/- 0.03 +/- 0.15) x 10(-4). In this decay, 7 N* intermediate resonances are observed. Among these, two new resonances, N(2300) and N(2570) are significant, one 1/2(+) resonance with a mass of 2300(-30-0)(+40+109) MeV/c(2) and width of 340(-30-58)(+30+110) MeV/c(2), and one 5/2(-) resonance with a mass of 2570(-10-10)(+19+34) MeV/c(2) and width of 250(-24-21)(+14+69) MeV/c(.)(2) For the remaining 5 N* intermediate resonances [N(1440), N(1520), N(1535), N(1650) and N(1720)], the analysis yields mass and width values that are consistent with those from established resonances. DOI: 10.1103/PhysRevLett.110.022001
Published: 2013

48. Observation of a Charged Charmoniumlike Structure in e^{+}e^{-}→π^{+}π^{-}J/ψ at sqrt[s]=4.26 GeV

Author: M, Ablikim, M N, Achasov, X C, Ai, O, Albayrak, D J, Ambrose, F F, An, Q, An, J Z, Bai, R, Baldini Ferroli, Y, Ban, J, Becker, J V, Bennett, M, Bertani, J M, Bian, E, Boger, O, Bondarenko, I, Boyko, R A, Briere, V, Bytev, H, Cai, X, Cai, O, Cakir, A, Calcaterra, G F, Cao, S A, Cetin, J F, Chang, G, Chelkov, G, Chen, H S, Chen, J C, Chen, M L, Chen, S J, Chen, X, Chen, Y B, Chen, H P, Cheng, Y P, Chu, D, Cronin-Hennessy, H L, Dai, J P, Dai, D, Dedovich, Z Y, Deng, A, Denig, I, Denysenko, M, Destefanis, W M, Ding, Y, Ding, L Y, Dong, M Y, Dong, S X, Du, J, Fang, S S, Fang, L, Fava, C Q, Feng, P, Friedel, C D, Fu, J L, Fu, O, Fuks, Q, Gao, Y, Gao, C, Geng, K, Goetzen, W X, Gong, W, Gradl, M, Greco, M H, Gu, Y T, Gu, Y H, Guan, A Q, Guo, L B, Guo, T, Guo, Y P, Guo, Y L, Han, F A, Harris, K L, He, M, He, Z Y, He, T, Held, Y K, Heng, Z L, Hou, C, Hu, H M, Hu, J F, Hu, T, Hu, G M, Huang, G S, Huang, J S, Huang, L, Huang, X T, Huang, Y, Huang, Y P, Huang, T, Hussain, C S, Ji, Q, Ji, Q P, Ji, X B, Ji, X L, Ji, L L, Jiang, X S, Jiang, J B, Jiao, Z, Jiao, D P, Jin, S, Jin, F F, Jing, N, Kalantar-Nayestanaki, M, Kavatsyuk, B, Kopf, M, Kornicer, W, Kühn, W, Lai, J S, Lange, M, Lara, P, Larin, M, Leyhe, C H, Li, Cheng, Li, Cui, Li, D M, Li, F, Li, G, Li, H B, Li, J C, Li, K, Li, Lei, Li, Q J, Li, S L, Li, W D, Li, W G, Li, X L, Li, X N, Li, X Q, Li, X R, Li, Z B, Li, H, Liang, Y F, Liang, Y T, Liang, G R, Liao, X T, Liao, D, Lin, B J, Liu, C L, Liu, C X, Liu, F H, Liu, Fang, Liu, Feng, Liu, H, Liu, H B, Liu, H H, Liu, H M, Liu, H W, Liu, J P, Liu, K, Liu, K Y, Liu, Kai, Liu, P L, Liu, Q, Liu, S B, Liu, X, Liu, Y B, Liu, Z A, Liu, Zhiqiang, Liu, Zhiqing, Liu, H, Loehner, X C, Lou, G R, Lu, H J, Lu, J G, Lu, Q W, Lu, X R, Lu, Y P, Lu, C L, Luo, M X, Luo, T, Luo, X L, Luo, M, Lv, C L, Ma, F C, Ma, H L, Ma, Q M, Ma, S, Ma, T, Ma, X Y, Ma, F E, Maas, M, Maggiora, Q A, Malik, Y J, Mao, Z P, Mao, J G, Messchendorp, J, Min, T J, Min, R E, Mitchell, X H, Mo, Y J, Mo, H, Moeini, C, Morales Morales, K, Moriya, N Yu, Muchnoi, H, Muramatsu, Y, Nefedov, C, Nicholson, I B, Nikolaev, Z, Ning, S L, Olsen, Q, Ouyang, S, Pacetti, J W, Park, M, Pelizaeus, H P, Peng, K, Peters, J L, Ping, R G, Ping, R, Poling, E, Prencipe, M, Qi, S, Qian, C F, Qiao, L Q, Qin, X S, Qin, Y, Qin, Z H, Qin, J F, Qiu, K H, Rashid, G, Rong, X D, Ruan, A, Sarantsev, B D, Schaefer, M, Shao, C P, Shen, X Y, Shen, H Y, Sheng, M R, Shepherd, W M, Song, X Y, Song, S, Spataro, B, Spruck, D H, Sun, G X, Sun, J F, Sun, S S, Sun, Y J, Sun, Y Z, Sun, Z J, Sun, Z T, Sun, C J, Tang, X, Tang, I, Tapan, E H, Thorndike, D, Toth, M, Ullrich, I, Uman, G S, Varner, B Q, Wang, D, Wang, D Y, Wang, K, Wang, L L, Wang, L S, Wang, M, Wang, P, Wang, P L, Wang, Q J, Wang, S G, Wang, X F, Wang, X L, Wang, Y D, Wang, Y F, Wang, Y Q, Wang, Z, Wang, Z G, Wang, Z Y, Wang, D H, Wei, J B, Wei, P, Weidenkaff, Q G, Wen, S P, Wen, M, Werner, U, Wiedner, L H, Wu, N, Wu, S X, Wu, W, Wu, Z, Wu, L G, Xia, Y X, Xia, Z J, Xiao, Y G, Xie, Q L, Xiu, G F, Xu, G M, Xu, Q J, Xu, Q N, Xu, X P, Xu, Z R, Xu, F, Xue, Z, Xue, L, Yan, W B, Yan, Y H, Yan, H X, Yang, Y, Yang, Y X, Yang, H, Ye, M, Ye, M H, Ye, B X, Yu, C X, Yu, H W, Yu, J S, Yu, S P, Yu, C Z, Yuan, Y, Yuan, A A, Zafar, A, Zallo, S L, Zang, Y, Zeng, B X, Zhang, B Y, Zhang, C, Zhang, C C, Zhang, D H, Zhang, H H, Zhang, H Y, Zhang, J Q, Zhang, J W, Zhang, J Y, Zhang, J Z, Zhang, LiLi, Zhang, R, Zhang, S H, Zhang, X J, Zhang, X Y, Zhang, Y, Zhang, Y H, Zhang, Z P, Zhang, Z Y, Zhang, Zhenghao, Zhang, G, Zhao, H S, Zhao, J W, Zhao, K X, Zhao, Lei, Zhao, Ling, Zhao, M G, Zhao, Q, Zhao, S J, Zhao, T C, Zhao, X H, Zhao, Y B, Zhao, Z G, Zhao, A, Zhemchugov, B, Zheng, J P, Zheng, Y H, Zheng, B, Zhong, L, Zhou, X, Zhou, X K, Zhou, X R, Zhou, C, Zhu, K, Zhu, K J, Zhu, S H, Zhu, X L, Zhu, Y C, Zhu, Y M, Zhu, Y S, Zhu, Z A, Zhu, J, Zhuang, B S, Zou, and J H, Zou
Abstract: We study the process ee+ e- → π+ π- J/ψ at a center-of-mass energy of 4.260 GeV using a 525 pb(-1) data sample collected with the BESIII detector operating at the Beijing Electron Positron Collider. The Born cross section is measured to be (62.9±1.9±3.7) pb, consistent with the production of the Y(4260). We observe a structure at around 3.9 GeV/c2 in the π(±)J/ψ mass spectrum, which we refer to as the Z(c)(3900). If interpreted as a new particle, it is unusual in that it carries an electric charge and couples to charmonium. A fit to the π(±)J/ψ invariant mass spectrum, neglecting interference, results in a mass of (3899.0±3.6±4.9) MeV/c2 and a width of (46±10±20) MeV. Its production ratio is measured to be R = (σ(e+ e- → π(±)Z(c)(3900)(∓) → π+ π- J/ψ)/σ(e+ e- → π+ π- J/ψ)) = (21.5±3.3±7.5)%. In all measurements the first errors are statistical and the second are systematic.
Published: 2013

49. Study ofJ/ψ→pp¯andJ/ψ→nn¯

Author: Zhenyu Zhang, W. Lai, Z. Ning, Tao Hu, S. L. Li, R. B. Ferroli, X. S. Qin, C. Nicholson, S. S. Sun, M. H. Ye, P. L. Wang, F. F. Jing, Xing Lu, J. H. Zou, J. Zhong, C. Morales Morales, X. L. Luo, M. N. Achasov, J. X. Zuo, M. Ullrich, X. B. Ji, K. Goetzen, X. D. Ruan, A. Sarantsev, Z. P. Mao, X. K. Zhou, X. H. Zhao, H. H. Zhang, W. M. Ding, Y. Nefedov, X. D. Sun, J. C. Chen, X. L. Ji, S. P. Yu, H. X. Yang, Yao Wang, K. J. Zhu, Xuantong Zhang, Ling Zhao, Lei Zhao, Z. Y. He, Yang Yang, Z. A. Liu, A. Zhemchugov, M. Wang, Z. Jiao, Talib Hussain, Y. S. Zhang, J. S. Huang, Z. G. Wang, H. Y. Zhang, M. Pelizaeus, Zhiqing Liu, J. S. Lange, H. S. Zhao, R. E. Mitchell, D. H. Zhang, S. J. Zhao, X. R. Zhou, J. L. Fu, Jingwei Zhao, J. F. Hu, J. P. Dai, Chang-Zheng Yuan, G. M. Xu, X. Cai, S. P. Wen, Y. F. Liang, L. Y. Dong, Chun S. J. Pun, Niklaus Berger, Y. Ban, Q. A. Malik, Cheng Li, T. Held, L. L. Wang, Chunyan Zhu, A. Q. Guo, C. L. Luo, T. C. Zhao, J. L. Ping, J. Y. Zhang, X. Y. Zhang, R. Poling, H. J. Lu, Z. J. Xiao, Fang Liu, Lei Zhou, Shaodan Ma, M. G. Zhao, J. Min, L. Zhang, X. L. Li, M. L. Chen, D. Dedovich, Xingtao Huang, A. Denig, X. F. Wang, Huihui Liu, Y. Yuan, D. H. Sun, Zhiqiang Liu, Miao He, Yi-Fang Zhao, X. P. Xu, S. H. Zhu, Shouguang Jin, F. E. Maas, Q. An, Y. P. Huang, R. G. Ping, Z. A. Zhu, Y. T. Liang, B. Zheng, D. M. Li, X. R. Li, Yu-Bin Liu, B. Y. Zhang, V. Bytev, X. Q. Hao, J. G. Messchendorp, P. L. Liu, B. Huang, L. S. Wang, N. Kalantar-Nayestanaki, X. H. Mo, Tao Luo, H. Y. Sheng, H. M. Hu, Y. Qin, Q. J. Wang, J. P. Liu, S. X. Wu, H. H. Liu, M. Greco, S. Spataro, K. H. Rashid, S. G. Wang, Feng Liu, Y. H. Zheng, I. B. Nikolaev, Y. J. Sun, Jianping Zheng, X. Liu, Xian Lun Zhu, Wei Li, X. L. Wang, U. Wiedner, Q. L. Xiu, J. Zhang, C. D. Fu, W. L. Yuan, Guangyu Zhao, M. Lv, J. G. Zhang, M. Kavatsyuk, Sai-Juan Chen, D. P. Jin, A. Calcaterra, C. X. Yu, J. Q. Zhang, G. X. Sun, W. G. Li, C. L. Ma, Xiujuan Tang, L. B. Guo, H. S. Chen, Kai Liu, J. C. Li, Kun Liu, J. F. Sun, K. Peters, Y. P. Lu, Shisong Fang, G. R. Liao, Qun-Yao Wang, C. S. Ji, E. Prencipe, G. M. Huang, G. F. Xu, Q. Ji, T. Yang, X. T. Liao, D. Toth, A. Zallo, I. Denysenko, E. Boger, H. Xu, F. C. Ma, C. X. Liu, Y. K. Heng, J. W. Zhang, Q. J. Li, H. M. Liu, Hang Liu, N. Wu, L. G. Xia, Y. S. Zhu, J. F. Qiu, G. S. Varner, F. F. An, S. Pacetti, Y. H. Guan, Y. J. Mao, B. Wang, Z. Y. Deng, Michael Werner, X. H. Liu, Z. P. Zheng, M. Bertani, M. R. Shepherd, Feng Xue, Cui Li, B. X. Yu, X. N. Li, Y. B. Liu, Y. H. Yan, Q. J. Xu, H. Loehner, D. H. Wei, Y. Xu, N. B. Li, B. Zhong, W. Kuehn, J. Zhuang, L. H. Wu, M. X. Luo, T. J. Min, Qingming Ma, S. H. Zhang, Q Zhao, B. X. Zhang, H. Ye, Chang Liu, Jie Yu, D. J. Ambrose, Zhihao Xu, Chuan Liu, T. R. Zhang, M. H. Gu, Zhibing Li, Z. H. Qin, Guo-Ming Chen, C. Motzko, S. L. Olsen, G. Li, Z. L. Hou, G. R. Lu, J. Fang, J. F. Chang, M. Qi, G. F. Cao, Xiang Li, C. Geng, Z. Xue, J. K. Becker, G. Rong, Y. P. Guo, J. K. C. Leung, J. B. Jiao, Y. P. Chu, Junguang Lu, C. F. Qiao, G. Chelkov, Xiaobo Zhu, Yang Gao, N. Yu. Muchnoi, Y. H. Zhang, Q. W. Lu, Q. G. Wen, Y. M. Zhu, Z. Y. Wang, M. Maggiora, K. Li, E. H. Thorndike, Yuanbo Chen, X. S. Jiang, S. B. Liu, Lei Li, Z. P. Zhang, T. Ma, H. B. Liu, Hua-Bin Li, B. S. Zou, Y. Zhang, Yuehong Xie, Wei Wu, H. Mao, H. L. Ma, M. Shao, M. Y. Dong, Z. G. Zhao, Y. X. Yang, Hai Liang, P. Weidenkaff, Yulei Han, Kunlun He, Daniel P Cronin-Hennessy, Y. Z. Sun, W. B. Yan, L. L. Jiang, Z. H. An, B. Spruck, Xueyong Shen, F. Feldbauer, Zujian Wang, Zhi-Jun Sun, J. Z. Bai, Y. T. Gu, Li Yan, Fu-Hu Liu, Y. F. Wang, F. A. Harris, Zhe Sun, Y. B. Chen, X. Y. Ma, J. Z. Zhang, Chunmei Zhang, K. Wang, C. Q. Feng, C. H. Li, B. Q. Wang, Y. Ma, C. P. Shen, H. P. Cheng, Y. Q. Wang, Z. Wu, M. Ablikim, A. A. Zafar, K. Y. Liu, H. L. Tian, C. J. Tang, K. X. Zhao, H. L. Dai, S. X. Du, I. Boyko, J. Schulze, Y. Zeng, J. M. Bian, Y. Ding, R. A. Briere, S. Qian, L. K. Jia, Xie-Yan Song, Q. Ouyang, Feng Li, O. Bondarenko, L. Fava, Brent J. Liu, M. Destefanis, W. X. Gong, Joong-Won Park, and W. Gradl
Subjects: Baryon, Physics, Nuclear and High Energy Physics, QCD sum rules, Proton, Electron–positron annihilation, Phase angle, Analytical chemistry, High Energy Physics::Experiment, Astrophysics::Earth and Planetary Astrophysics, Nucleon, Antineutron, Bar (unit)
Abstract: The decays J/psi -> p (p) over bar and J/psi -> n (n) over bar have been investigated with a sample of 225.2 x 10(6) J/psi events collected with the BESIII detector at the BEPCII e(+)e(-) collider. The branching fractions are determined to be B(J/psi -> p (p) over bar) = (2.112 +/- 0.004 +/- 0.031 x 10(-3) and B(J/psi -> n (n) over bar) =(2.07 +/- 0.01 +/- 0.17) x 10(-3). Distributions of the angle theta between the proton or antineutron and the beam direction are well described by the form 1 + alpha cos(2)theta, and we find alpha = 0.595 +/- 0.012 +/- 0.015 for J/psi -> p (p) over bar and alpha = 0.50 +/- 0.04 +/- 0.21 for J/psi -> n (n) over bar. Our branching- fraction results suggest a large phase angle between the strong and electromagnetic amplitudes describing the J/psi -> N (N) over bar decay.
Published: 2012

50. First Observation of theM1Transitionψ(3686)→γηc(2S)

Author: C. Q. Feng, L. Zhang, Z. Jiao, Z. A. Zhu, B. Q. Wang, M. Bertani, Y. Ma, C. P. Shen, B. Zhong, J. Q. Zhang, Zhe Sun, X. S. Qin, C. Nicholson, Qingming Ma, Zhiqing Liu, Y. B. Chen, Feng Liu, Chang Liu, J. Z. Zhang, M. Ullrich, X. D. Ruan, H. H. Liu, T. R. Zhang, K. Wang, Kun Liu, Shisong Fang, F. F. An, Y. H. Guan, X. H. Liu, X. H. Mo, M. H. Gu, L. Yu, X. R. Li, Q. J. Wang, J. P. Liu, Y. P. Guo, J. K. C. Leung, G. Li, A. Q. Guo, Jianping Zheng, W. L. Yuan, Ling Zhao, H. Loehner, J. B. Jiao, M. Lv, J. G. Zhang, X. T. Liao, Y. P. Chu, Junguang Lu, C. F. Qiao, J. Z. Bai, Y. T. Gu, J. C. Chen, Lei Zhao, Z. Y. He, G. Chelkov, Yang Yang, C. L. Ma, H. Xu, F. C. Ma, I. Boyko, Y. Zeng, J. Zhuang, L. H. Wu, M. X. Luo, Y. H. Yan, Z. Ning, X. L. Wang, X. S. Jiang, J. S. Huang, C. Geng, A. Zhemchugov, R. A. Briere, D. H. Zhang, H. B. Liu, S. L. Li, R. B. Ferroli, C. S. Ji, T. Yang, L. Y. Dong, L. K. Jia, I. Denysenko, E. Boger, B. X. Zhang, Y. J. Mao, Niklaus Berger, S. Pacetti, Zhiqiang Liu, Miao He, Q. An, B. X. Yu, D. P. Jin, W. Kuehn, J. F. Hu, X. L. Li, S. X. Wu, B. S. Zou, T. J. Min, Xiujuan Tang, X. N. Li, Brent J. Liu, M. Destefanis, Feng Li, G. M. Xu, H. M. Hu, H. Mao, Haiping Peng, X. Cai, Y. T. Liang, Zhihao Xu, Chuan Liu, Zong-Ping Zheng, Z. H. Qin, J. H. Zou, Xie-Yan Song, W. X. Gong, G. M. Huang, D. J. Ambrose, Chang-Zheng Yuan, P. Weidenkaff, J. Zhang, M. Kavatsyuk, A. Sarantsev, Tao Luo, B. Wang, Z. Y. Deng, Daniel P Cronin-Hennessy, Xingtao Huang, A. Denig, Q. Ouyang, Sai-Juan Chen, K. Li, Michael Werner, E. H. Thorndike, Chun S. J. Pun, V. Bytev, Li Yan, H. L. Ma, C. Motzko, S. L. Olsen, Y. Qin, M. Shao, Xian Lun Zhu, C. D. Fu, N. Yu. Muchnoi, Y. Nefedov, D. H. Sun, Hang Liu, J. S. Lange, L. B. Guo, M. G. Zhao, T. C. Zhao, J. L. Ping, X. D. Sun, R. Poling, G. R. Lu, X. F. Wang, Huihui Liu, Fu-Hu Liu, Y. H. Zhang, Q. W. Lu, H. X. Yang, K. J. Zhu, Jingwei Zhao, A. Calcaterra, X. W. Zhu, O. Bondarenko, Yu-Bin Liu, H. H. Zhang, Jiangchao Li, Z. G. Zhao, Yuanbo Chen, Q. J. Xu, J. G. Messchendorp, S. B. Liu, Joong-Won Park, Q. G. Wen, Xuantong Zhang, C. X. Liu, L. Fava, Y. X. Yang, S. H. Zhang, H. L. Dai, Jie Yu, D. H. Wei, Yao Wang, Y. Yuan, Q. L. Xiu, E. Prencipe, Z. Y. Wang, M. Maggiora, Lei Li, G. X. Sun, W. G. Li, M. Wang, S. X. Du, Guo-Ming Chen, Z. L. Hou, Y. B. Liu, Z. P. Zhang, B. D. Schaefer, Y. Ban, S. G. Wang, J. Schulze, M. Y. Dong, X. L. Ji, S. P. Yu, S. P. Wen, Y. F. Liang, Y. Z. Sun, Q. A. Malik, S. H. Zhu, J. M. Bian, Z. H. An, B. Spruck, Z. Xue, T. Ma, Q. Ji, C. X. Yu, Y. Ding, Haosheng Chen, Talib Hussain, P. L. Wang, G. F. Xu, S. Qian, J. F. Sun, M. R. Shepherd, F. Feldbauer, Hai Liang, P. L. Liu, Feng Xue, Cui Li, Hua-Bin Li, M. Qi, J. K. Becker, Y. Xu, N. B. Li, Q. J. Li, Q Zhao, H. M. Liu, M. Pelizaeus, H. Ye, G. S. Varner, Y. Zhang, Yulei Han, Yuehong Xie, Xing Lu, Wei Wu, F. E. Maas, J. Zhong, H. P. Cheng, X. Q. Li, Kunlun He, Kai Liu, Yang Gao, Ka-Yuet Liu, N. Wu, Y. Q. Wang, Zhibing Li, M. Ablikim, C. L. Luo, A. A. Zafar, W. B. Yan, L. L. Jiang, X. L. Luo, Fang Liu, Lei Zhou, X. K. Zhou, Xueyong Shen, Zujian Wang, Y. S. Zhang, H. S. Zhao, Zhi-Jun Sun, X. P. Xu, T. Held, H. J. Lu, D. M. Li, B. Y. Zhang, Y. H. Zheng, I. B. Nikolaev, F. F. Jing, M. N. Achasov, J. X. Zuo, Z. G. Wang, H. Y. Zhang, Guangyu Zhao, R. E. Mitchell, J. Y. Zhang, J. P. Dai, J. Min, Chunyan Zhu, D. Dedovich, Shaodan Ma, Shouguang Jin, Yi-Fang Zhao, Y. P. Huang, W. Gradl, W. Lai, Y. K. Heng, J. W. Zhang, X. Q. Hao, Tao Hu, B. Huang, Zhiyong Zhang, L. S. Wang, N. Kalantar-Nayestanaki, M. H. Ye, K. H. Rashid, X. Liu, C. Morales Morales, H. Y. Sheng, S. Spataro, M. Greco, U. Wiedner, Y. P. Lu, G. R. Liao, D. Toth, S. J. Zhao, L. L. Wang, X. Y. Zhang, M. L. Chen, R. G. Ping, S. S. Sun, X. B. Ji, K. Goetzen, Z. P. Mao, X. H. Zhao, W. M. Ding, J. Fang, J. F. Chang, G. F. Cao, G. Rong, Z. A. Liu, Y. M. Zhu, X. R. Zhou, J. L. Fu, Cheng Li, Z. J. Xiao, B. Zheng, Y. J. Sun, Wei Li, Qun-Yao Wang, K. Peters, A. Zallo, L. G. Xia, Y. S. Zhu, J. F. Qiu, Z. Wu, H. L. Tian, C. J. Tang, K. X. Zhao, Y. F. Wang, F. A. Harris, X. Y. Ma, Chunmei Zhang, and C. H. Li
Subjects: Physics, Branching fraction, Electron–positron annihilation, Excited state, Analytical chemistry, General Physics and Astronomy
Abstract: Using a sample of 106×10(6) ψ(3686) events collected with the BESIII detector at the BEPCII storage ring, we have made the first measurement of the M1 transition between the radially excited charmonium S-wave spin-triplet and the radially excited S-wave spin-singlet states: ψ(3686)→γη(c)(2S). Analyses of the processes ψ(3686)→γη(c)(2S) with η(c)(2S)→K(S)(0)K(±)π(∓) and K(+)K(-)π(0) give an η(c)(2S) signal with a statistical significance of greater than 10 standard deviations under a wide range of assumptions about the signal and background properties. The data are used to obtain measurements of the η(c)(2S) mass (M(η(c)(2S))=3637.6±2.9(stat)±1.6(syst) MeV/c(2)), width (Γ(η(c)(2S))=16.9±6.4(stat)±4.8(syst) MeV), and the product branching-fraction (B(ψ(3686)→γη(c)(2S))×B(η(c)(2S)→KKπ)=(1.30±0.20(stat)±0.30(syst))×10(-5)). Combining our result with a BABAR measurement of B(η(c)(2S)→KKπ), we find the branching fraction of the M1 transition to be B(ψ(3686)→γη(c)(2S))=(6.8±1.1(stat)±4.5(syst))×10(-4).
Published: 2012

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