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1,676 results on '"CHEN, J.-L."'

1. Hadronic cross section measurements with the DAMPE space mission using 20GeV-10TeV cosmic-ray protons and $^4$He

Author

Alemanno, F., An, Q., Azzarello, P., Barbato, F. C. T., Bernardini, P., Bi, X. J., Cagnoli, I., Cai, M. S., Casilli, E., Catanzani, E., Chang, J., Chen, D. Y., Chen, J. L., Chen, Z. F., Coppin, P., Cui, M. Y., Cui, T. S., Cui, Y. X., Dai, H. T., De Benedittis, A., De Mitri, I., de Palma, F., Di Giovanni, A., Ding, Q., Dong, T. K., Dong, Z. X., Donvito, G., Droz, D., Duan, J. L., Duan, K. K., Fan, R. R., Fan, Y. Z., Fang, F., Fang, K., Feng, C. Q., Feng, L., Frieden, J. M., Fusco, P., Gao, M., Gargano, F., Gong, K., Gong, Y. Z., Guo, D. Y., Guo, J. H., Han, S. X., Hu, Y. M., Huang, G. S., Huang, X. Y., Huang, Y. Y., Ionica, M., Jiang, L. Y., Jiang, Y. Z., Jiang, W., Kong, J., Kotenko, A., Kyratzis, D., Lei, S. J., Li, W. H., Li, W. L., Li, X., Li, X. Q., Liang, Y. M., Liu, C. M., Liu, H., Liu, J., Liu, S. B., Liu, Y., Loparco, F., Luo, C. N., Ma, M., Ma, P. X., Ma, T., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Niu, X. Y., Pan, X., Parenti, A., Peng, W. X., Peng, X. Y., Perrina, C., Putti-Garcia, E., Qiao, R., Rao, J. N., Ruina, A., Sarkar, R., Savina, P., Serpolla, A., Shangguan, Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Silveri, L., Song, J. X., Stolpovskiy, M., Su, H., Su, M., Sun, H. R., Sun, Z. Y., Surdo, A., Teng, X. J., Tykhonov, A., Wang, J. Z., Wang, L. G., Wang, S., Wang, S. X., Wang, X. L., Wang, Y., Wang, Y. F., Wang, Y. Z., Wang, Z. M., Wei, D. M., Wei, J. J., Wei, Y. F., Wu, D., Wu, J., Wu, S. S., Wu, X., Xia, Z. Q., Xu, H. T., Xu, J., Xu, Z. H., Xu, Z. L., Xu, E. H., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, P., Yang, Y. Q., Yao, H. J., Yu, Y. H., Yuan, G. W., Yuan, Q., Yue, C., Zang, J. J., Zhang, S. X., Zhang, W. Z., Zhang, Yan, Zhang, Yi, Zhang, Y. J., Zhang, Y. L., Zhang, Y. P., Zhang, Y. Q., Zhang, Z., Zhang, Z. Y., Zhao, C., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., and Zhu, Y.

Subjects
High Energy Physics - Experiment
Abstract

Precise direct cosmic-ray (CR) measurements provide an important probe to study the energetic particle sources in our Galaxy, and the interstellar environment through which these particles propagate. Uncertainties on hadronic models, ion-nucleon cross sections in particular, are currently the limiting factor towards obtaining more accurate CR ion flux measurements with calorimetric space-based experiments. We present an energy-dependent measurement of the inelastic cross section of protons and helium-4 nuclei (alpha particles) on a Bi$_4$Ge$_3$O$_{12}$ target, using 88 months of data collected by the DAMPE space mission. The kinetic energy range per nucleon of the measurement points ranges from 18 GeV to 9 TeV for protons, and from 5 GeV/n to 3 TeV/n for helium-4 nuclei. Our results lead to a significant improvement of the CR flux normalisation. In the case of helium-4, these results correspond to the first cross section measurements on a heavy target material at energies above 10 GeV/n., Comment: 17 pages, submitted to PRD

Published
2024

2. Interstellar Nitrogen Isotope Ratios: Measurements on tracers of C$^{14}$N and C$^{15}$N

Author

Chen, J. L., Zhang, J. S., Henkel, C., Yan, Y. T., Yu, H. Z., Wang, Y. X., Zou, Y. P., Zhao, J. Y., and Wang, X. Y.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The nitrogen isotope ratio 14N/15N is a powerful tool to trace Galactic stellar nucleosynthesis and constraining Galactic chemical evolution. Previous observations have found lower 14N/15N ratios in the Galactic center and higher values in the Galactic disk. This is consistent with the inside-out formation scenario of our Milky Way. However, previous studies mostly utilized double isotope ratios also including 12C/13C, which introduces additional uncertainties. Here we therefore present observations of C14N and its rare isotopologue, C15N, toward a sample of star forming regions, measured by the IRAM 30 m and/or the ARO 12 m telescope at $\lambda$ ~3 mm wavelength. For those 35 sources detected in both isotopologues, physical parameters are determined. Furthermore we have obtained nitrogen isotope ratios using the strongest hyperfine components of CN and C15N. For those sources showing small deviations from Local Thermodynamical Equilibrium and/or self-absorption, the weakest hyperfine component, likely free of the latter effect, was used to obtain reliable 14N/15N values. Our measured 14N/15N isotope ratios from C14N and C15N measurements are compatible with those from our earlier measurements of NH3 and 15NH3 (Paper I), i.e., increasing ratios to a Galacticentric distance of ~9 kpc. The unweighted second order polynomial fit yields $\frac{{\rm C^{14}N}}{{\rm C^{15}N}} = (-4.85 \pm 1.89)\;{\rm kpc^{-2}} \times R_{\rm GC}^{2} + (82.11 \pm 31.93) \;{\rm kpc^{-1}} \times R_{\rm GC} - (28.12 \pm 126.62)$. Toward the outer galaxy, the isotope ratio tends to decrease, supporting an earlier finding by H13CN/HC15N. Galactic chemical evolution models are consistent with our measurements of the 14N/15N isotope ratio, i.e. a rising trend from the Galactic center region to approximately 9 kpc, followed by a decreasing trend with increasing $R_{\rm GC}$ toward the outer Galaxy., Comment: 34 pages, 9 figures, 6 tables

Published
2024

3. Robustness of Interferometric Power to Sudden Death

Author

Zhu, D., Zhang, F. L., and Chen, J. L.

Subjects
Quantum Physics
Abstract

We study the dissipative dynamics of interferometric power as a discordlike measure in Markovian environments, such as dephasing, depolarizing, and generalized amplitude damping. Moreover, we compare the dynamics of interferometric power and entanglement by choosing proper initial conditions. Our study shows that in all cases where the sudden death of entanglement appears, interferometric power decays asymptotically. Therefore, quantum metrology based on interferometric power is more robust than entanglement., Comment: 8 pages, 10 figures. Comments welcome!

Published
2024

4. Sudden change of interferometric power for X shape states

Author

Zhu, D., Zhang, F. L., and Chen, J. L.

Subjects
Quantum Physics
Abstract

Quantum interferometric power (IP) is a discordlike measure. We study the dynamics of IP for two-qubit X shape states under different noisy environments. Our study shows that IP exhibits sudden change, and one side quantum channel is enough for the occurrence of a sudden change of IP. In particular, we show that the initial state having no sudden change of quantum discord exhibits a sudden change of IP under the dynamics of amplitude noise, but the converse is not true. Besides, we also investigate the dynamics of IP under two different kinds of composite noises. Our results also confirm that sudden change of IP occurs under such composite noises., Comment: 11 pages, 8 figures. Comments welcome!

Published
2024

6. A Systematic Observational Study on Galactic Interstellar Ratio 18O/17O. II. C18O and C17O J=2-1 Data Analysis

Author

Zou, Y. P., Zhang, J. S., Henkel, C., Romano, D., Liu, W., Zheng, Y. H., Yan, Y. T., Chen, J. L., Wang, Y. X., and Zhao, J. Y.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

To investigate the relative amount of ejecta from high-mass versus intermediate-mass stars and to trace the chemical evolution of the Galaxy, we have performed with the IRAM 30m and the SMT 10m telescopes a systematic study of Galactic interstellar 18O/17O ratios toward a sample of 421 molecular clouds, covering a galactocentric distance range of 1-22 kpc. The results presented in this paper are based on the J=2-1 transition and encompass 364 sources showing both C18O and C17O detections. The previously suggested 18O/17O gradient is confirmed. For the 41 sources detected with both facilities, good agreement is obtained. A correlation of 18O/17O ratios with heliocentric distance is not found, indicating that beam dilution and linear beam sizes are not relevant. For the subsample of IRAM 30 m high-mass star-forming regions with accurate parallax distances, an unweighted fit gives 18O/17O = (0.12+-0.02)R_GC+(2.38+-0.13) with a correlation coefficient of R = 0.67. While the slope is consistent with our J=1-0 measurement, ratios are systematically lower. This should be caused by larger optical depths of C18O 2-1 lines, w.r.t the corresponding 1-0 transitions, which is supported by RADEX calculations and the fact that C18O/C17O is positively correlated with 13CO/C18O. After considering optical depth effects with C18O J=2-1 reaching typically an optical depth of 0.5, corrected 18O/17O ratios from the J=1-0 and J=2-1 lines become consistent. A good numerical fit to the data is provided by the MWG-12 model, including both rotating stars and novae., Comment: 17 pages, 11 figures, published in ApJS

Published
2023
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7. Measurement of the cosmic p+He energy spectrum from 50 GeV to 0.5 PeV with the DAMPE space mission

Author

DAMPE Collaboration, Alemanno, F., Altomare, C., An, Q., Azzarello, P., Barbato, F. C. T., Bernardini, P., Bi, X. J., Cagnoli, I., Cai, M. S., Casilli, E., Catanzani, E., Chang, J., Chen, D. Y., Chen, J. L., Chen, Z. F., Coppin, P., Cui, M. Y., Cui, T. S., Cui, Y. X., Dai, H. T., De Benedittis, A., De Mitri, I., de Palma, F., Deliyergiyev, M., Di Giovanni, A., Di Santo, M., Ding, Q., Dong, T. K., Dong, Z. X., Donvito, G., Droz, D., Duan, J. L., Duan, K. K., Fan, R. R., Fan, Y. Z., Fang, F., Fang, K., Feng, C. Q., Feng, L., Alonso, M. Fernandez, Frieden, J. M., Fusco, P., Gao, M., Gargano, F., Gong, K., Gong, Y. Z., Guo, D. Y., Guo, J. H., Han, S. X., Hu, Y. M., Huang, G. S., Huang, X. Y., Huang, Y. Y., Ionica, M., Jiang, L. Y., Jiang, Y. Z., Jiang, W., Kong, J., Kotenko, A., Kyratzis, D., Lei, S. J., Li, W. H., Li, W. L., Li, X., Li, X. Q., Liang, Y. M., Liu, C. M., Liu, H., Liu, J., Liu, S. B., Liu, Y., Loparco, F., Luo, C. N., Ma, M., Ma, P. X., Ma, T., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Salinas, M. Muñoz, Niu, X. Y., Pan, X., Parenti, A., Peng, W. X., Peng, X. Y., Perrina, C., Putti-Garcia, E., Qiao, R., Rao, J. N., Ruina, A., Shangguan, Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Silveri, L., Song, J. X., Stolpovskiy, M., Su, H., Su, M., Sun, H. R., Sun, Z. Y., Surdo, A., Teng, X. J., Tykhonov, A., Wang, J. Z., Wang, L. G., Wang, S., Wang, S. X., Wang, X. L., Wang, Y., Wang, Y. F., Wang, Y. Z., Wang, Z. M., Wei, D. M., Wei, J. J., Wei, Y. F., Wu, D., Wu, J., Wu, L. B., Wu, S. S., Wu, X., Xia, Z. Q., Xu, H. T., Xu, J., Xu, Z. H., Xu, Z. L., Xu, E. H., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, P., Yang, Y. Q., Yao, H. J., Yu, Y. H., Yuan, G. W., Yuan, Q., Yue, C., Zang, J. J., Zhang, S. X., Zhang, W. Z., Zhang, Yan, Zhang, Yi, Zhang, Y. J., Zhang, Y. L., Zhang, Y. P., Zhang, Y. Q., Zhang, Z., Zhang, Z. Y., Zhao, C., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., and Zhu, Y.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract

Recent observations of the light component of the cosmic-ray spectrum have revealed unexpected features that motivate further and more precise measurements up to the highest energies. The Dark Matter Particle Explorer is a satellite-based cosmic-ray experiment that has been operational since December 2015, continuously collecting data on high-energy cosmic particles with very good statistics, energy resolution, and particle identification capabilities. In this work, the latest measurements of the energy spectrum of proton+helium in the energy range from 46 GeV to 464 TeV are presented. Among the most distinctive features of the spectrum, a spectral hardening at 600 GeV has been observed, along with a softening at 29 TeV measured with a 6.6{\sigma} significance. Moreover, the detector features and the analysis approach allowed for the extension of the spectral measurement up to the sub-PeV region. Even if with small statistical significance due to the low number of events, data suggest a new spectral hardening at about 150 TeV., Comment: Published on PRD

Published
2023
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8. A Possible Chemical Clock in High-mass Star-forming Regions: N(HC3N)/N(N2H+)?

Author

Wang, Y. X., Zhang, J. S., Yu, H. Z., Wang, Y., Yan, Y. T., Chen, J. L., Zhao, J. Y., and Zou, Y. P.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We conducted observations of multiple HC3N (J = 10-9, 12-11, and 16-15) lines and the N2H+ (J = 1-0) line toward a large sample of 61 ultracompact (UC) H II regions, through the Institutde Radioastronomie Millmetrique 30 m and the Arizona Radio Observatory 12 m telescopes. The N2H+ J = 1-0 line is detected in 60 sources and HC3N is detected in 59 sources, including 40 sources with three lines, 9 sources with two lines, and 10 sources with one line. Using the rotational diagram, the rotational temperature and column density of HC3N were estimated toward sources with at least two HC3N lines. For 10 sources with only one HC3N line, their parameters were estimated, taking one average value of Trot. For N2H+, we estimated the optical depth of the N2H+ J = 1-0 line, based on the line intensity ratio of its hyperfine structure lines. Then the excitation temperature and column density were calculated. When combining our results in UC H II regions and previous observation results on high-mass starless cores and high-mass protostellar cores, the N(HC3N)/N(N2H+) ratio clearly increases from the region stage. This means that the abundance ratio changes with the evolution of high-mass star-forming regions (HMSFRs). Moreover, positive correlations between the ratio and other evolutionary indicators (dust temperature, bolometric luminosity, and luminosity-to-mass ratio) are found. Thus we propose the ratio of N(HC3N)/N(N2H+) as a reliable chemical clock of HMSFRs., Comment: 40 pages, 8 figures and 8 tables

Published
2023
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9. Individual pulse emission from the diffuse drifter PSR J1401$-$6357 using the ultrawideband receiver on the Parkes radio telescope

Author

Chen, J. L., Wen, Z. G., Duan, X. F., He, D. L., Wang, N., Wang, H. G., Yuen, R., Yuan, J. P., Yan, W. M., Wang, Z., Lv, C. B., Wang, H., and Cui, S. R.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

In this study, we report on a detailed single pulse analysis of the radio emission from the pulsar J1401$-$6357 (B1358$-$63) based on data observed with the ultrawideband low-frequency receiver on the Parkes radio telescope. In addition to a weak leading component, the integrated pulse profile features a single-humped structure with a slight asymmetry. The frequency evolution of the pulse profile is studied. Well-defined nulls, with an estimated nulling fraction greater than 2\%, are present across the whole frequency band. No emission is detected with significance above 3$\sigma$ in the average pulse profile integrated over all null pulses. Using fluctuation spectral analysis, we reveal the existence of temporal-dependent subpulse drifting in this pulsar for the first time. A clear double-peaked feature is present at exactly the alias border across the whole frequency band, which suggests that the apparent drift sense changes during the observation. Our observations provide further confirmation that the phenomena of pulse nulling and subpulse drifting are independent of observing frequency, which suggest that they invoke changes on the global magnetospheric scale., Comment: 10 pages, 13 figures

Published
2022
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10. Search for relativistic fractionally charged particles in space

Author

DAMPE Collaboration, Alemanno, F., Altomare, C., An, Q., Azzarello, P., Barbato, F. C. T., Bernardini, P., Bi, X. J., Cai, M. S., Casilli, E., Catanzani, E., Chang, J., Chen, D. Y., Chen, J. L., Chen, Z. F., Cui, M. Y., Cui, T. S., Cui, Y. X., Dai, H. T., De-Benedittis, A., De Mitri, I., de Palma, F., Deliyergiyev, M., Di Giovanni, A., Di Santo, M., Ding, Q., Dong, T. K., Dong, Z. X., Donvito, G., Droz, D., Duan, J. L., Duan, K. K., D'Urso, D., Fan, R. R., Fan, Y. Z., Fang, F., Fang, K., Feng, C. Q., Feng, L., Alonso, M. F., Frieden, J. M., Fusco, P., Gao, M., Gargano, F., Gong, K., Gong, Y. Z., Guo, D. Y., Guo, J. H., Han, S. X., Hu, Y. M., Huang, G. S., Huang, X. Y., Huang, Y. Y., Ionica, M., Jiang, L. Y., Jiang, W., Kong, J., Kotenko, A., Kyratzis, D., Lei, S. J., Li, W. L., Li, W. H., Li, X., Li, X. Q., Liang, Y. M., Liu, C. M., Liu, H., Liu, J., Liu, S. B., Liu, Y., Loparco, F., Luo, C. N., Ma, M., Ma, P. X., Ma, T., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Salinas, M. M., Niu, X. Y., Pan, X., Parenti, A., Peng, W. X., Peng, X. Y., Perrina, C., Qiao, R., Rao, J. N., Ruina, A., Shangguan, Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Silveri, L., Song, J. X., Stolpovskiy, M., Su, H., Su, M., Sun, H. R., Sun, Z. Y., Surdo, A., Teng, X. J., Tykhonov, A., Wang, J. Z., Wang, L. G., Wang, S., Wang, S. X., Wang, X. L., Wang, Y., Wang, Y. F., Wang, Y. Z., Wei, D. M., Wei, J. J., Wei, Y. F., Wu, D., Wu, J., Wu, L. B., Wu, S. S., Wu, X., Xia, Z. Q., Xu, E. H., Xu, H. T., Xu, J., Xu, Z. H., Xu, Z. L., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, P., Yang, Y. Q., Yao, H. J., Yu, Y. H., Yuan, G. W., Yuan, Q., Yue, C., Zang, J. J., Zhang, S. X., Zhang, W. Z., Zhang, Yan, Zhang, Yi., Zhang, Y. J., Zhang, Y. L., Zhang, Y. P., Zhang, Y. Q., Zhang, Z., Zhang, Z. Y., Zhao, C., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., and Zhu, Y.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment, High Energy Physics - Phenomenology, Physics - Space Physics
Abstract

More than a century after the performance of the oil drop experiment, the possible existence of fractionally charged particles FCP still remains unsettled. The search for FCPs is crucial for some extensions of the Standard Model in particle physics. Most of the previously conducted searches for FCPs in cosmic rays were based on experiments underground or at high altitudes. However, there have been few searches for FCPs in cosmic rays carried out in orbit other than AMS-01 flown by a space shuttle and BESS by a balloon at the top of the atmosphere. In this study, we conduct an FCP search in space based on on-orbit data obtained using the DArk Matter Particle Explorer (DAMPE) satellite over a period of five years. Unlike underground experiments, which require an FCP energy of the order of hundreds of GeV, our FCP search starts at only a few GeV. An upper limit of $6.2\times 10^{-10}~~\mathrm{cm^{-2}sr^{-1} s^{-1}}$ is obtained for the flux. Our results demonstrate that DAMPE exhibits higher sensitivity than experiments of similar types by three orders of magnitude that more stringently restricts the conditions for the existence of FCP in primary cosmic rays., Comment: 19 pages, 6 figures, accepted by PRD

Published
2022
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11. Interstellar Nitrogen Isotope Ratios: New NH3 Data from the Galactic Center out to the Perseus Arm

Author

Chen, J. L., Zhang, J. S., Henkel, C., Yan, Y. T., Yu, H. Z., Qiu, J. J., Tang, X. D., Wang, J., Liu, W., Wang, Y. X., Zheng, Y. H., Zhao, J. Y., and Zou, Y. P.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Our aim is to measure the interstellar 14N/15N ratio across the Galaxy, to establish a standard data set on interstellar ammonia isotope ratios, and to provide new constraints on the Galactic chemical evolution. The (J, K ) = (1, 1), (2, 2), and (3, 3) lines of 14NH3 and 15NH3 were observed with the Shanghai Tianma 65 m radio telescope (TMRT) and the Effelsberg 100 m telescope toward a large sample of 210 sources. One hundred fourty-one of these sources were detected by the TMRT in 14NH3. Eight of them were also detected in 15NH3. For 10 of the 36 sources with strong NH3 emission, the Effelsberg 100 m telescope successfully detected their 15NH3(1, 1) lines, including 3 sources (G081.7522, W51D, and Orion-KL) with detections by the TMRT telescope. Thus, a total of 15 sources are detected in both the 14NH3 and 15NH3 lines. Line and physical parameters for these 15 sources are derived, including optical depths, rotation and kinetic temperatures, and total column densities. 14N/15N isotope ratios were determined from the 14NH3/15NH3 abundance ratios. The isotope ratios obtained from both telescopes agree for a given source within the uncertainties, and no dependence on heliocentric distance and kinetic temperature is seen. 14N/15N ratios tend to increase with galactocentric distance, confirming a radial nitrogen isotope gradient. This is consistent with results from recent Galactic chemical model calculations, including the impact of superasymptotic giant branch stars and novae.

Published
2022
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12. The discovery of a rotating radio transient J1918$-$0449 with intriguing emission properties with the five hundred meter aperture spherical radio telescope

Author

Chen, J. L., Wen, Z. G., Yuan, J. P., Wang, N., Li, D., Wang, H. G., Yan, W. M., Yuen, R., Wang, P., Wang, Z., Zhu, W. W., Niu, J. R., Miao, C. C., Xue, M. Y., and Gong, B. P.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

In this study, we report on a detailed single pulse analysis of the radio emission from a rotating radio transient (RRAT) J1918$-$0449 which is the first RRAT discovered with the five hundred meter aperture spherical radio telescope (FAST). The sensitive observations were carried out on 30 April 2021 using the FAST with a central frequency of 1250 MHz and a short time resolution of 49.152 $\mu$s, which forms a reliable basis to probe single pulse emission properties in detail. The source was successively observed for around 2 hours. A total of 83 dispersed bursts with significance above 6$\sigma$ are detected over 1.8 hours. The source's DM and rotational period are determined to be 116.1$\pm$0.4 \pcm \ and 2479.21$\pm$0.03 ms, respectively. The share of registered pulses from the total number of observed period is 3.12\%. No underlying emission is detected in the averaged off pulse profile. For bursts with fluence larger than 10 Jy ms, the pulse energy follows a power-law distribution with an index of $-3.1\pm0.4$, suggesting the existence of bright pulse emission. We find that the distribution of time between subsequent pulses is consistent with a stationary Poisson process and find no evidence of clustering over the 1.8 h observations, giving a mean burst rate of one burst every 66 s. Close inspection of the detected bright pulses reveals that 21 pulses exhibit well-defined quasi-periodicities. The subpulse drifting is present in non-successive rotations with periodicity of $2.51\pm0.06$ periods. Finally, possible physical mechanisms are discussed., Comment: 11 pages, 11 figures

Published
2022
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13. Cyanopolyyne line survey towards high-mass star-forming regions with TMRT

Author

Wang, Y. X., Zhang, J. S., Yan, Y. T., Qiu, J. J., Chen, J. L., Zhao, J. Y., Zou, Y. P., Wu, X. C., He, X. L., Gong, Y. B., and Cai, J. H.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We carried out a cyanopolyyne line survey towards a large sample of HMSFRs using the Shanghai Tian Ma 65m Radio Telescope (TMRT). Our sample consisted of 123 targets taken from the TMRT C band line survey. It included three kinds of sources, namely those with detection of the 6.7 GHz CH3OH maser alone, with detection of the radio recombination line (RRL) alone, and with detection of both (hereafter referred to as Maser-only, RRL-only, and Maser-RRL sources, respectively). We detected HC3N in 38 sources, HC5N in 11 sources, and HC7N in G24.790+0.084, with the highest detection rate being found for Maser-RRL sources and a very low detection rate found for RRL-only sources. Their column densities were derived using the rotational temperature measured from the NH3 lines. And we constructed and fitted the far-infrared (FIR) spectral energy distributions. Based on these, we derive their dust temperatures, H2 column densities, and abundances of cyanopolyynes relative to H2. The detection rate, the column density, and the relative abundance of HC3N increase from Maser-only to Maser-RRL sources and decrease from Maser-RRL to RRL-only sources. This trend is consistent with the proposed evolutionary trend of HC3N under the assumption that our Maser-only, Maser-RRL, and RRL-only sources correspond to massive young stellar objects, ultra-compact HII regions, and normal classical HII regions, respectively. Furthermore, a statistical analysis of the integrated line intensity and column density of HC3N and shock-tracing molecules (SiO, H2CO) enabled us to find positive correlations between them. This suggests that HC3N may be another tracer of shocks, and should therefore be the subject of further observations and corresponding chemical simulations. Our results indirectly support the idea that the neutral--neutral reaction between C2H2 and CN is the dominant formation pathway of HC3N., Comment: 23 pages, 5 figures, 4 tables, Accepted to A&A

Published
2022
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14. Decayless longitudinal oscillations of a solar filament maintained by quasi-periodic jets

Author

Ni, Y. W., Guo, J. H., Zhang, Q. M., Chen, J. L., Fang, C., and Chen, P. F.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Context: As a ubiquitous phenomenon, large-amplitude longitudinal filament oscillations usually decay in 1--4 periods. Recently, we observed a decayless case of such oscillations in the corona. Aims: We try to understand the physical process that maintains the decayless oscillation of the filament. Methods: Multi-wavelength imaging observations and magnetograms are collected to study the dynamics of the filament oscillation and its associated phenomena. To explain the decayless oscillations, we also perform one-dimensional hydrodynamic numerical simulations using the MPI-AMRVAC code. Results: In observations, the filament oscillates decaylessly with a period of $36.4 \pm 0.3$ min for almost 4 hours before eruption. During oscillations, four quasi-periodic jets emanate from a magnetic cancellation site near the filament. The time interval between neighboring jets is $\sim 68.9 \pm 1.0$ min. Numerical simulations constrained by the observations reproduced the decayless longitudinal oscillations. However, it is surprising to find that the period of the decayless oscillations is not consistent with the pendulum model. Conclusions: We propose that the decayless longitudinal oscillations of the filament are maintained by quasi-periodic jets, which is verified by the hydrodynamic simulations. More importantly, it is found that, when driven by quasi-periodic jets, the period of the filament longitudinal oscillations depends also on the driving period of the jets, not simply the pendulum period. With a parameter survey in simulations, we derived a formula, by which one can derive the pendulum oscillation period using the observed period of decayless filament oscillations and the driving periods of jets., Comment: 11 pages, 10 figures, accepted for publication in Section 9. The Sun and the Heliosphere of Astronomy and Astrophysics, comments are welcome

Published
2022
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15. Transverse Coronal-Loop Oscillations Induced by the Non-radial Eruption of a Magnetic Flux Rope

Author

Zhang, Q. M., Chen, J. L., Li, S. T., Lu, L., and Li, D.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

We investigate the transverse coronal-loop oscillations induced by the eruption of a prominence-carrying flux rope on 7 December 2012. The flux rope originating from NOAA Active Region (AR) 11621 was observed in EUV wavelengths by the SDO/AIA and in H$\alpha$ line center by the ground-based telescope at the BBSO. The early evolution of the flux rope is divided into two steps: a slow rise phase at a speed of $\approx$230\,km\,s$^{-1}$ and a fast rise phase at a speed of $\approx$706\,km\,s$^{-1}$. The eruption generates a C5.8 flare and the onset of the fast rise is consistent with the HXR peak time of the flare. The embedded prominence has a lower speed of $\approx$452\,km\,s$^{-1}$. During the early eruption of the flux rope, the nearby coronal loops are disturbed and experience independent kink-mode oscillations in the horizontal and vertical directions. The oscillation in the horizontal direction has an initial amplitude of $\approx$3.1\,Mm, a period of $\approx$294\,seconds, and a damping time of $\approx$645\,seconds. It is most striking in 171\,{\AA} and lasts for three to four cycles. The oscillations in the vertical directions are observed mainly in 171, 193, and 211\,{\AA}. The initial amplitudes lie in the range of 3.4\,--\,5.2\,Mm, with an average value of 4.5\,Mm. The periods are between 407\,seconds and 441\,seconds, with an average value of 423\,seconds. The oscillations are damping and last for nearly four cycles. The damping times lie in the range of 570\,--\,1012\,seconds, with an average value of 741\,seconds. Assuming a semi-circular shape of the vertically oscillating loops, we calculate the loop lengths according to their heights. Using the observed periods, we carry out coronal seismology and estimate the internal Alfv\'{e}n speeds (988\,--\,1145\,km\,s$^{-1}$) and the magnetic-field strengths (12\,--\,43\,G) of the oscillating loops., Comment: 22 pages, 12 figures, accepted for publication in Solar Physics

Published
2022
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16. Discovery of ammonia (9,6) masers in two high-mass star-forming regions

Author

Yan, Y. T., Henkel, C., Menten, K. M., Gong, Y., Ott, J., Wilson, T. L., Wootten, A., Brunthaler, A., Zhang, J. S., Chen, J. L., and Yang, K.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

Molecular maser lines are signposts of high-mass star formation, probing excitation and kinematics of very compact regions in the close environment of young stellar objects and providing useful targets for trigonometric parallax measurements. Only a few NH$_{3}$ (9,6) masers were known so far, and their origin is still poorly understood. Here we aim to find new NH$_{3}$ (9,6) masers to provide a better observational basis to study their role in high-mass star-forming regions. We carried out NH$_{3}$ (9,6) observations toward Cepheus A and G34.26$+$0.15 with the Effelsberg-100 m telescope and the Karl G. Janksy Very Large Array. We discovered new NH$_{3}$ (9,6) masers in Cep A and G34.26$+$0.15, which increases the number of high-mass star-forming regions hosting NH$_{3}$ (9,6) masers from five to seven. Long term monitoring (20 months) at Effelsberg shows that the intensity of the (9,6) maser in G34.26$+$0.15 is decreasing, while the Cep A maser remains stable. Compared to the Effelsberg data and assuming linear variations between the epochs of observation, the JVLA data indicate no missing flux. This suggests that the NH$_3$ (9,6) emission arises from single compact emission regions that are not resolved by the interferometric measurements. As JVLA imaging shows, the NH$_{3}$ (9,6) emission in Cep A originates from a sub-arcsecond sized region, slightly to the west of the peak position of the 1.36\,cm continuum object, HW2. In G34.26$+$0.15, three NH$_{3}$ (9,6) maser spots are observed: one is close to the head of the cometary ultracompact \h2 region C and the other two are emitted from a compact region to the west of the hypercompact \h2 region A. The newly found (9,6) masers appear to be related to outflows. Higher angular resolution of JVLA and VLBI observations are needed to provide more accurate positions and constraints for pumping scenarios., Comment: 10 pages, 6 figures, 3 tables. Publicated in A&A

Published
2021
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17. Measurement of the cosmic ray helium energy spectrum from 70 GeV to 80 TeV with the DAMPE space mission

Author

Alemanno, F., An, Q., Azzarello, P., Barbato, F. C. T., Bernardini, P., Bi, X. J., Cai, M. S., Catanzani, E., Chang, J., Chen, D. Y., Chen, J. L., Chen, Z. F., Cui, M. Y., Cui, T. S., Cui, Y. X., Dai, H. T., D'Amone, A., De Benedittis, A., De Mitri, I., de Palma, F., Deliyergiyev, M., Di Santo, M., Dong, T. K., Dong, Z. X., Donvito, G., Droz, D., Duan, J. L., Duan, K. K., D'Urso, D., Fan, R. R., Fan, Y. Z., Fang, K., Fang, F., Feng, C. Q., Feng, L., Fusco, P., Gao, M., Gargano, F., Gong, K., Gong, Y. Z., Guo, D. Y., Guo, J. H., Guo, X. L., Han, S. X., Hu, Y. M., Huang, G. S., Huang, X. Y., Huang, Y. Y., Ionica, M., Jiang, W., Kong, J., Kotenko, A., Kyratzis, D., Lei, S. J., Li, S., Li, W. L., Li, X., Li, X. Q., Liang, Y. M., Liu, C. M., Liu, H., Liu, J., Liu, S. B., Liu, W. Q., Liu, Y., Loparco, F., Luo, C. N., Ma, M., Ma, P. X., Ma, T., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Niu, X. Y., Pan, X., Parenti, A., Peng, W. X., Peng, X. Y., Perrina, C., Qiao, R., Rao, J. N., Ruina, A., Salinas, M. M., Shang, G. Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Silveri, L., Song, J. X., Stolpovskiy, M., Su, H., Su, M., Sun, Z. Y., Surdo, A., Teng, X. J., Tykhonov, A., Wang, H., Wang, J. Z., Wang, L. G., Wang, S., Wang, X. L., Wang, Y., Wang, Y. F., Wang, Y. Z., Wang, Z. M., Wei, D. M., Wei, J. J., Wei, Y. F., Wen, S. C., Wu, D., Wu, J., Wu, L. B., Wu, S. S., Wu, X., Xia, Z. Q., Xu, H. T., Xu, Z. H., Xu, Z. L., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, P., Yang, Y. Q., Yao, H. J., Yu, Y. H., Yuan, G. W., Yuan, Q., Yue, C., Zang, J. J., Zhang, F., Zhang, S. X., Zhang, W. Z., Zhang, Y., Zhang, Y. J., Zhang, Y. L., Zhang, Y. P., Zhang, Y. Q., Zhang, Z., Zhang, Z. Y., Zhao, C., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., and Zhu, Y.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract

The measurement of the energy spectrum of cosmic ray helium nuclei from 70 GeV to 80 TeV using 4.5 years of data recorded by the DArk Matter Particle Explorer (DAMPE) is reported in this work. A hardening of the spectrum is observed at an energy of about 1.3 TeV, similar to previous observations. In addition, a spectral softening at about 34 TeV is revealed for the first time with large statistics and well controlled systematic uncertainties, with an overall significance of $4.3\sigma$. The DAMPE spectral measurements of both cosmic protons and helium nuclei suggest a particle charge dependent softening energy, although with current uncertainties a dependence on the number of nucleons cannot be ruled out., Comment: 11 pages, 13 figures, published in Phys. Rev. Lett. Add one more digit for first three columns in Table S2

Published
2021
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19. The Mode Switching in Pulsar J1326$-$6700

Author

Wen, Z. G., Yan, W. M., Yuan, J. P., Wang, H. G., Chen, J. L., Mijit, M., Yuen, R., Wang, N., Tu, Z. Y., and Dang, S. J.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report on a detailed study of the mode switching in pulsar J1326$-$6700 by analyzing the data acquired from the Parkes 64 m radio telescope at 1369 MHz. During the abnormal mode, the emission at the central and trailing components becomes extremely weak. Meanwhile, the leading emission shifts toward earlier longitude by almost 2{\deg}, and remains in this position for typically less than a minute. The mean flux density of the normal mode is almost five times that of the abnormal mode. Our data show that, for PSR J1326$-$6700, 85% of the time was spent in the normal mode and 15% was in the abnormal mode. The intrinsic distributions of mode timescales can be well described by Weibull distributions, which present a certain amount of memory in mode switching. Furthermore, a quasiperiodicity has been identified in the mode switching in pulsar J1326$-$6700. The estimated delay emission heights based on the kinematical effects indicate that the abnormal mode may have originated from higher altitude than the normal mode., Comment: 10 pages, 8 figures

Published
2020
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20. Galactic interstellar sulfur isotopes: A radial $^{32}$S$/$$^{34}$S gradient?

Author

Yu, H. Z., Zhang, J. S., Henkel, C., Yan, Y. T., Liu, W., Tang, X. D., Langer, N., Luan, T. C., Chen, J. L., Wang, Y. X., Deng, G. G., and Zhou, Y. P.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

We present observations of $^{12}$C$^{32}$S, $^{12}$C$^{34}$S, $^{13}$C$^{32}$S and $^{12}$C$^{33}$S J=2$-$1 lines toward a large sample of massive star forming regions by using the Arizona Radio Observatory 12-m telescope and the IRAM\,30-m. Taking new measurements of the carbon $^{12}$C/$^{13}$C ratio, the $^{32}$S$/$$^{34}$S isotope ratio was determined from the integrated $^{13}$C$^{32}$S/$^{12}$C$^{34}$S line intensity ratios for our sample. Our analysis shows a $^{32}$S$/$$^{34}$S gradient from the inner Galaxy out to a galactocentric distance of 12\,kpc. An unweighted least-squares fit to our data yields $^{32}$S$/$$^{34}$S = (1.56 $\pm$ 0.17)$\rm D_{\rm GC}$ + (6.75 $\pm$ 1.22) with a correlation coefficient of 0.77. Errors represent 1$\sigma$ standard deviations. Testing this result by (a) excluding the Galactic center region, (b) excluding all sources with C$^{34}$S opacities $>$ 0.25, (c) combining our data and old data from previous study, and (d) using different sets of carbon isotope ratios leads to the conclusion that the observed $^{32}$S$/$$^{34}$S gradient is not an artefact but persists irrespective of the choice of the sample and carbon isotope data. A gradient with rising $^{32}$S$/$$^{34}$S values as a function of galactocentric radius implies that the solar system ratio should be larger than that of the local interstellar medium. With the new carbon isotope ratios we obtain indeed a local $^{32}$S$/$$^{34}$S isotope ratio about 10$\%$ below the solar system one, as expected in case of decreasing $^{32}$S$/$$^{34}$S ratios with time and increased amounts of stellar processing. However, taking older carbon isotope ratios based on a lesser amount of data, such a decrease is not seen. No systematic variation of $^{34}$S$/$$^{33}$S ratios along galactocentric distance was found., Comment: 28 pages, 11 figures, 5 tables. Accepted for publication in ApJ

Published
2020
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21. Giant micropulse emission in the Vela pulsar at C band

Author

Chen, J. L., Wen, Z. G., Hao, L. F., Yuan, J. P., Li, J., Wang, H. G., Yan, W. M., Lee, K. J., Wang, N., Xu, Y. H., Li, Z. X., Huang, Y. X., Yuen, R., and Mijit, M.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present here the analysis of giant micropulses from the Vela pulsar. A total of 4187 giant micropulses with peak flux density $>$2.5 Jy were detected during almost 4 hours of observations carried out with the Yunnan 40-m radio telescope at 6800 MHz. Nine of the giant micropulses arrived approximately 3 to 4 ms earlier than the peak of average pulse profile, longer than that at lower frequencies. The remaining giant micropulses were clustered into three distributions which correspond to three main emission regions, including four occurring on the trailing edge of averaged profile., Comment: 9 pages, 8 figures

Published
2020
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22. A systematic observational study on Galactic interstellar ratio 18O/17O: I. C18O and C17O J=1-0 data analysis

Author

Zhang, J. S., Liu, W., Yan, Y. T., Yu, H. Z., Liu, J. T., Zheng, Y. H., Romano, D., Zhang, Z. -Y., Wang, J. Z., Chen, J. L., Wang, Y. X., Zhang, W. J., Lu, H. H., Chen, L. S., Zou, Y. P., Yang, H. Q., Wen, T., and Lu, F. S.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The interstellar oxygen isotopic ratio of 18O/17O can reflect the relative amount of the secular enrichment by ejecta from high-mass versus intermediate-mass stars. Previous observations found a Galactic gradient of 18O/17O, i.e., low ratios in the Galactic center and large values in the Galactic disk, which supports the insideout formation scenario of our Galaxy. However, the observed objects are not many and, in particular, not so many at large galactocentric distances. Thus we started a systematic study on Galactic interstellar 18O/17O, through observations of C18O and C17O multi-transition lines toward a large sample of 286 sources (at least one order of magnitude larger than previous ones), from the Galactic center region to the far outer Galaxy (~22 kpc). Here we present our observations of J=1-0 lines of C18O and C17O, with the ARO12m and the IRAM 30m telescope. We detected successfully both C18O and C17O 1-0 lines for 34 sources among our IRAM30m sample of 50 targets and for 166 sources among our ARO12m sample of 260 targets. The C18O optical depth effect on our ratio results, evaluated by fitting results of C17O spectra with hyperfine components and our RADEX non-LTE model calculation for the strongest source, was found to be insignificant. Beam dilution does not seem to be a problem either, which was supported by the fact of no systematic variation between the isotopic ratio and the heliocentric distance, and consistent measured ratios from two telescopes for most of those detected sources. Our results, though there are still very few detections made for sources in the outer Galaxy, confirm the apparent 18O/17O gradient of 18O/17O = (0.10+-0.03)R_GC+(2.95+-0.30), with a Pearson's rank correlation coefficient R = 0.69. This is supported by the newest Galactic chemical evolution model including the impact of massive stellar rotators and novae., Comment: 35 pages, 7 figures, published in ApJS

Published
2020
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23. Chemical upgrade of carbon monoxide to acetate on an atomically dispersed copper catalyst via CO-insertion

Author

Fu, X, Wang, Y, Shen, H, Yu, Y, Xu, F, Zhou, G, Xie, W, Qin, R, Dun, C, Pao, C-W, Chen, J-L, Liu, Y, Guo, J, Yue, Q, Urban, JJ, Wang, C, and Kang, Y

Subjects
Engineering, Physical Sciences, Materials Engineering, Atomic, Molecular and Optical Physics, Condensed Matter Physics, Affordable and Clean Energy, Climate Action, Materials engineering, Atomic, molecular and optical physics, Condensed matter physics
Abstract

Electrochemical conversion of small molecules such as carbon dioxide (CO2) and carbon monoxide (CO) to high-value multi-carbon products (C2+) offers a chemical upgrade approach for fuels and chemical feedstock production using renewable energy, in the possible absence of the petrochemical industry under the new energy system such as hydrogen economy. Identifying robust and efficient electrocatalysts to selectively produce C2+ products remains a challenge. Herein, we report a synthetic strategy of atomically dispersing copper atoms on nitrogen-rich porous carbon (Cu–N–C) through pyrolysis of a supramolecular assembly. Benefitting from the unsaturated coordination structure, in KOH electrolyte, the Cu–N–C with a Cu content of 6.9 wt% exhibits a maximum acetate Faradaic efficiency (FE) of 30% with an acetate partial current density as high as 48 mA cm−2 in electrochemical CO reduction. Different from the C–C coupling mechanism on metallic copper, we propose a CO insertion mechanism for the acetate production on the single site copper catalyst.

Published
2021

24. Periodic mode changing in PSR J1048-5832

Author

Yan, W. M., Manchester, R. N., Wang, N., Wen, Z. G., Yuan, J. P., Lee, K. J., and Chen, J. L.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

By analysing the data acquired from the Parkes 64-m radio telescope at 1369 MHz, we report on the phase-stationary non-drift amplitude modulation observed in PSR J1048-5832. The high-sensitivity observations revealed that the central and trailing components of the pulse profile of this pulsar switch between a strong mode and a weak mode periodically. However, the leading component remains unchanged. Polarization properties of the strong and weak modes are investigated. Considering the similarity to mode changing, we argue that the periodic amplitude modulation in PSR J1048$-$5832 is periodic mode changing. The fluctuation spectral analysis showed that the modulation period is very short (~2.1 s or 17 P1), where P1 is the rotation period of the pulsar. We find that this periodic amplitude modulation is hard to explain by existing models that account for the periodic phenomena in pulsars like subpulse drifting., Comment: 8 pages, 8 figures, 3 tables, accepted in MNRAS for publication

Published
2019
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25. Measurement of the cosmic-ray proton spectrum from 40 GeV to 100 TeV with the DAMPE satellite

Author

An, Q., Asfandiyarov, R., Azzarello, P., Bernardini, P., Bi, X. J., Cai, M. S., Chang, J., Chen, D. Y., Chen, H. F., Chen, J. L., Chen, W., Cui, M. Y., Cui, T. S., Dai, H. T., D'Amone, A., De Benedittis, A., De Mitri, I., Di Santo, M., Ding, M., Dong, T. K., Dong, Y. F., Dong, Z. X., Donvito, G., Droz, D., Duan, J. L., Duan, K. K., D'Urso, D., Fan, R. R., Fan, Y. Z., Fang, F., Feng, C. Q., Feng, L., Fusco, P., Gallo, V., Gan, F. J., Gao, M., Gargano, F., Gong, K., Gong, Y. Z., Guo, D. Y., Guo, J. H., Guo, X. L., Han, S. X., Hu, Y. M., Huang, G. S., Huang, X. Y., Huang, Y. Y., Ionica, M., Jiang, W., Jin, X., Kong, J., Lei, S. J., Li, S., Li, W. L., Li, X., Li, X. Q., Li, Y., Liang, Y. F., Liang, Y. M., Liao, N. H., Liu, C. M., Liu, H., Liu, J., Liu, S. B., Liu, W. Q., Liu, Y., Loparco, F., Luo, C. N., Ma, M., Ma, P. X., Ma, S. Y., Ma, T., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Niu, X. Y., Pan, X., Peng, W. X., Peng, X. Y., Qiao, R., Rao, J. N., Salinas, M. M., Shang, G. Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Song, J. X., Su, H., Su, M., Sun, Z. Y., Surdo, A., Teng, X. J., Tykhonov, A., Vitillo, S., Wang, C., Wang, H., Wang, H. Y., Wang, J. Z., Wang, L. G., Wang, Q., Wang, S., Wang, X. H., Wang, X. L., Wang, Y. F., Wang, Y. P., Wang, Y. Z., Wang, Z. M., Wei, D. M., Wei, J. J., Wei, Y. F., Wen, S. C., Wu, D., Wu, J., Wu, L. B., Wu, S. S., Wu, X., Xi, K., Xia, Z. Q., Xu, H. T., Xu, Z. H., Xu, Z. L., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, P., Yang, Y. Q., Yang, Z. L., Yao, H. J., Yu, Y. H., Yuan, Q., Yue, C., Zang, J. J., Zhang, F., Zhang, J. Y., Zhang, J. Z., Zhang, P. F., Zhang, S. X., Zhang, W. Z., Zhang, Y., Zhang, Y. J., Zhang, Y. L., Zhang, Y. P., Zhang, Y. Q., Zhang, Z., Zhang, Z. Y., Zhao, H., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., Zhou, Y., Zhu, X., Zhu, Y., and Zimmer, S.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

The precise measurement of the spectrum of protons, the most abundant component of the cosmic radiation, is necessary to understand the source and acceleration of cosmic rays in the Milky Way. This work reports the measurement of the cosmic ray proton fluxes with kinetic energies from 40 GeV to 100 TeV, with two and a half years of data recorded by the DArk Matter Particle Explorer (DAMPE). This is the first time an experiment directly measures the cosmic ray protons up to ~100 TeV with a high statistics. The measured spectrum confirms the spectral hardening found by previous experiments and reveals a softening at ~13.6 TeV, with the spectral index changing from ~2.60 to ~2.85. Our result suggests the existence of a new spectral feature of cosmic rays at energies lower than the so-called knee, and sheds new light on the origin of Galactic cosmic rays., Comment: 37 pages, 5 figures, published in Science Advances

Published
2019
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26. Energy partition in two M-class circular-ribbon flares

Author

Zhang, Q. M., Cheng, J. X., Feng, L., Su, Y., Lu, L., Huang, Y., Li, D., Zhou, T. H., and Chen, J. L.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

In this paper, we investigate the energy partition of two homologous M1.1 circular-ribbon flares (CRFs) in active region (AR) 12434. They were observed by \textit{SDO}, \textit{GOES}, and \textit{RHESSI} on 2015 October 15 and 16, respectively. The peak thermal energy, nonthermal energy of flare-accelerated electrons, total radiative loss of hot plasma, and radiant energies in 1$-$8 {\AA} and 1$-$70 {\AA} of the flares are calculated. The two flares have similar energetics. The peak thermal energies are (1.94$\pm$0.13)$\times$10$^{30}$ erg. The nonthermal energies in flare-accelerated electrons are (3.9$\pm$0.7)$\times$10$^{30}$ erg. The radiative outputs of the flare loops in 1$-$70 {\AA}, which are $\sim$200 times greater than the outputs in 1$-$8 {\AA}, account for $\sim$62.5\% of the peak thermal energies. The radiative losses of SXR-emitting plasma are one order of magnitude lower than the peak thermal energies. Therefore, the total heating requirements of flare loops including radiative loss are (2.1$\pm$0.1)$\times$10$^{30}$ erg, which could sufficiently be supplied by nonthermal electrons., Comment: 17 pages, 12 figures, accepted by ApJ

Published
2019
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27. The on-orbit calibration of DArk Matter Particle Explorer

Author

Ambrosi, G., An, Q., Asfandiyarov, R., Azzarello, P., Bernardini, P., Cai, M. S., Caragiulo, M., Chang, J., Chen, D. Y., Chen, H. F., Chen, J. L., Chen, W., Cui, M. Y., Cui, T. S., Dai, H. T., D'Amone, A., De Benedittis, A., De Mitri, I., Ding, M., Di Santo, M., Dong, J. N., Dong, T. K., Dong, Y. F., Dong, Z. X., Droz, D., Duan, K. K., Duan, J. L., D'Urso, D., Fan, R. R., Fan, Y. Z., Fang, F., Feng, C. Q., Feng, L., Fusco, P., Gallo, V., Gan, F. J., Gao, M., Gao, S. S., Gargano, F., Garrappa, S., Gong, K., Gong, Y. Z., Guo, J. H., Hu, Y. M., Huang, G. S., Huang, Y. Y., Ionica, M., Jiang, D., Jiang, W., Jin, X., Kong, J., Lei, S. J., Li, S., Li, X., Li, W. L., Li, Y., Liang, Y. F., Liang, Y. M., Liao, N. H., Liu, C. M., Liu, H., Liu, J., Liu, S. B., Liu, W. Q., Liu, Y., Loparco, F., Ma, M., Ma, P. X., Ma, S. Y., Ma, T., Ma, X. Q., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Niu, X. Y., Pan, X., Peng, X. Y., Peng, W. X., Qiao, R., Rao, J. N., Salinas, M. M., Shang, G. Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Song, J. X., Su, H., Su, M., Sun, Z. Y., Surdo, A., Teng, X. J., Tian, X. B., Tykhonov, A., Vitillo, S., Wang, C., Wang, H., Wang, H. Y., Wang, J. Z., Wang, L. G., Wang, Q., Wang, S., Wang, X. H., Wang, X. L., Wang, Y. F., Wang, Y. P., Wang, Y. Z., Wang, Z. M., Wen, S. C., Wei, D. M., Wei, J. J., Wei, Y. F., Wu, D., Wu, J., Wu, L. B., Wu, S. S., Wu, X., Xi, K., Xia, Z. Q., Xin, Y. L., Xu, H. T., Xu, Z. H., Xu, Z. L., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, P., Yang, Y. Q., Yang, Z. L., Yao, H. J., Yu, Y. H., Yuan, Q., Yue, C., Zang, J. J., Zhang, D. L., Zhang, F., Zhang, J. B., Zhang, J. Y., Zhang, J. Z., Zhang, L., Zhang, P. F., Zhang, S. X., Zhang, W. Z., Zhang, Y., Zhang, Y. J., Zhang, Y. Q., Zhang, Y. L., Zhang, Y. P., Zhang, Z., Zhang, Z. Y., Zhao, H., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., Zhou, Y., Zhu, X., Zhu, Y., and Zimmer, S.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment
Abstract

The DArk Matter Particle Explorer (DAMPE), a satellite-based cosmic ray and gamma-ray detector, was launched on December 17, 2015, and began its on-orbit operation on December 24, 2015. In this work we document the on-orbit calibration procedures used by DAMPE and report the calibration results of the Plastic Scintillator strip Detector (PSD), the Silicon-Tungsten tracKer-converter (STK), the BGO imaging calorimeter (BGO), and the Neutron Detector (NUD). The results are obtained using Galactic cosmic rays, bright known GeV gamma-ray sources, and charge injection into the front-end electronics of each sub-detector. The determination of the boundary of the South Atlantic Anomaly (SAA), the measurement of the live time, and the alignments of the detectors are also introduced. The calibration results demonstrate the stability of the detectors in almost two years of the on-orbit operation.

Published
2019
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28. Frequency of depressive symptoms among female migrant workers in China: associations with acculturation, discrimination, and reproductive health

Author

Lommel, L, Hu, X, Sun, M, and Chen, J-L

Subjects
Health Services and Systems, Health Sciences, Clinical Research, Brain Disorders, Mental Health, Basic Behavioral and Social Science, Behavioral and Social Science, Depression, Prevention, Aetiology, 2.3 Psychological, social and economic factors, Mental health, Good Health and Well Being, Acculturation, Adult, China, Cross-Sectional Studies, Depressive Disorder, Discrimination, Psychological, Female, Humans, Incidence, Middle Aged, Reproductive Health, Risk Factors, Stress, Psychological, Surveys and Questionnaires, Transients and Migrants, Young Adult, Acculturative stress, Discrimination, Reproductive health, Migrant women, Public Health and Health Services, Public Health, Epidemiology, Health services and systems, Public health
Abstract

OBJECTIVES:Depression has been associated with numerous adverse health conditions. This study sought to determine the frequency of significant depressive symptoms and whether or not acculturative stress, discrimination, and reproductive health conditions were risk factors for significant depressive symptoms in migrant working women in China. STUDY DESIGN:The design of this study is cross-sectional. METHODS:Data were derived from a survey of female migrant workers at three employment sites in Changsha, China. The associations between acculturative stress, discrimination, reproductive health, and risk for significant depressive symptoms were obtained using F-tests for mean differences, correlations, ordinary least squares regression, and logistic regression analysis. RESULTS:Between March and June 2017, 232 eligible female participants completed the survey among whom the median age was 34.36 years (standard error 0.43) and 25.58% reported significant depressive symptoms. Significant depressive symptoms were associated with higher education (F-test, P = .006), all four acculturative stress factors (r = 0.15 to r = 0.29), both institutional and interpersonal discrimination (r = 0.29, r = 0.35), age (r = - 0.13), and self-rated health (r = - 0.19). In multivariate regression analysis of depression scale scores, interpersonal discrimination was the strongest predictor (beta = 0.238, P = .002) among the nine factors identified in bivariate analysis. None of the other predictors (age, self-rated health, education, acculturative stress, and institutional discrimination) showed significant associations with the depression scale. Similar results were obtained for a multivariate logistic regression analysis of a clinically important threshold for depression (

Published
2020

29. Hardy's paradox for multi-settings and high-dimensional systems

Author

Meng, H. X., Zhou, J., Xu, Z. P., Su, H. Y., Gao, T., Yan, F. L., and Chen, J. L.

Subjects
Quantum Physics
Abstract

Recently, Chen et al introduced an alternative form of Hardy's paradox for $2$-settings and high-dimensional systems [Phy. Rev. A 88, 062116 (2013)], in which there is a great progress in improving the maximum probability of the nonlocal event. Here, we construct a general Hardy's paradox for multi-settings and high-dimensional systems, which (i) includes the paradox in [Phy. Rev. A 88, 062116 (2013)] as a special case, (ii) for spin-1/2 systems, is equivalent to the ladder proof of nonlocality without inequalities in [Phy. Rev. Lett. 13, 2755 (1997)], (iii) for spin-1 systems, increases the maximum probability of the nonlocal event by adding the number of settings, specially, with only 5-settings it can be improved to 0.40184, which is more than two times higher than 0.171, the maximal success probability to prove nonlocality in Adan's paradox [Phy. Rev. A 58, 1687 (1998)]., Comment: 7 pages

Published
2018
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30. Dynamic magnetic-transformation-induced exchange bias in (Fe2O3)0.1-(FeTiO3)0.9

Author

Song, P., Ma, L., Li, G. K., Zhen, C. M., Wang, C., Wang, W. H., Liu, E. K., Chen, J. L., Wu, G. H., Xia, Y. H., Zhang, J., Xie, C. M., Li, H., and Hou, D. L.

Subjects
Condensed Matter - Materials Science
Abstract

Up to now, for the conventional exchange bias (EB) systems there has been one pinning phase and one pinned phase, and the pinning and pinned phases are inherent to the material and do not mutually transform into each other. Interestingly, we show here that EB is observed in a special system (Fe2O3)0.1(FeTiO3)0.9 (HI9) different from the conventional EB system. Neutron powder diffraction and magnetic measurement confirm that for HI9: i) two types of short range antiferromagnetic ordering coexist, ii) there are two pinning phases and one pinned phase, iii) the pinned phase is not intrinsic to the structure but can be dynamically produced from the pinning phase with the help of an external magnetic field. Consequently, two anomalous EB behaviors are observed: i) both the coercivity (HC) and the exchange bias field (HE) simultaneously decrease to zero at 30 K, ii) for a high cooling field (Hcool) HE decreases logarithmically with increasing Hcool. Using Arrott plots it is confirmed that the first order magnetic phase transformation (FOMPT) from the AFM Fe2+ to ferromagnetic (FM) Fe2+ and the second order magnetic phase transformation (SOMPT) for the process whereby the FM Fe2+ aligns with the external field direction coexist in HI-9. The Morin transition and FOMPT cause the anomalous EB behaviors. This work may provide fresh ideas for research into EB behavior.

Published
2018
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31. Direct detection of a break in the teraelectronvolt cosmic-ray spectrum of electrons and positrons

Author

Ambrosi, G., An, Q., Asfandiyarov, R., Azzarello, P., Bernardini, P., Bertucci, B., Cai, M. S., Chang, J., Chen, D. Y., Chen, H. F., Chen, J. L., Chen, W., Cui, M. Y., Cui, T. S., D'Amone, A., De Benedittis, A., De Mitri, I., Di Santo, M., Dong, J. N., Dong, T. K., Dong, Y. F., Dong, Z. X., Donvito, G., Droz, D., Duan, K. K., Duan, J. L., Duranti, M., D'Urso, D., Fan, R. R., Fan, Y. Z., Fang, F., Feng, C. Q., Feng, L., Fusco, P., Gallo, V., Gan, F. J., Gao, M., Gao, S. S., Gargano, F., Garrappa, S., Gong, K., Gong, Y. Z., Guo, D. Y., Guo, J. H., Hu, Y. M., Huang, G. S., Huang, Y. Y., Ionica, M., Jiang, D., Jiang, W., Jin, X., Kong, J., Lei, S. J., Li, S., Li, X., Li, W. L., Li, Y., Liang, Y. F., Liang, Y. M., Liao, N. H., Liu, H., Liu, J., Liu, S. B., Liu, W. Q., Liu, Y., Loparco, F., Ma, M., Ma, P. X., Ma, S. Y., Ma, T., Ma, X. Q., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Niu, X. Y., Peng, X. Y., Peng, W. X., Qiao, R., Rao, J. N., Salinas, M. M., Shang, G. Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Song, J. X., Su, H., Su, M., Sun, Z. Y., Surdo, A., Teng, X. J., Tian, X. B., Tykhonov, A., Vagelli, V., Vitillo, S., Wang, C., Wang, H., Wang, H. Y., Wang, J. Z., Wang, L. G., Wang, Q., Wang, S., Wang, X. H., Wang, X. L., Wang, Y. F., Wang, Y. P., Wang, Y. Z., Wen, S. C., Wang, Z. M., Wei, D. M., Wei, J. J., Wei, Y. F., Wu, D., Wu, J., Wu, L. B., Wu, S. S., Wu, X., Xi, K., Xia, Z. Q., Xin, Y. L., Xu, H. T., Xu, Z. L., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, P., Yang, Y. Q., Yang, Z. L., Yao, H. J., Yu, Y. H., Yuan, Q., Yue, C., Zang, J. J., Zhang, C., Zhang, D. L., Zhang, F., Zhang, J. B., Zhang, J. Y., Zhang, J. Z., Zhang, L., Zhang, P. F., Zhang, S. X., Zhang, W. Z., Zhang, Y., Zhang, Y. J., Zhang, Y. Q., Zhang, Y. L., Zhang, Y. P., Zhang, Z., Zhang, Z. Y., Zhao, H., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., Zhou, Y., Zhu, X., Zhu, Y., and Zimmer, S.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment, High Energy Physics - Phenomenology
Abstract

High energy cosmic ray electrons plus positrons (CREs), which lose energy quickly during their propagation, provide an ideal probe of Galactic high-energy processes and may enable the observation of phenomena such as dark-matter particle annihilation or decay. The CRE spectrum has been directly measured up to $\sim 2$ TeV in previous balloon- or space-borne experiments, and indirectly up to $\sim 5$ TeV by ground-based Cherenkov $\gamma$-ray telescope arrays. Evidence for a spectral break in the TeV energy range has been provided by indirect measurements of H.E.S.S., although the results were qualified by sizeable systematic uncertainties. Here we report a direct measurement of CREs in the energy range $25~{\rm GeV}-4.6~{\rm TeV}$ by the DArk Matter Particle Explorer (DAMPE) with unprecedentedly high energy resolution and low background. The majority of the spectrum can be properly fitted by a smoothly broken power-law model rather than a single power-law model. The direct detection of a spectral break at $E \sim0.9$ TeV confirms the evidence found by H.E.S.S., clarifies the behavior of the CRE spectrum at energies above 1 TeV and sheds light on the physical origin of the sub-TeV CREs., Comment: 18 pages, 6 figures, Nature in press, doi:10.1038/nature24475

Published
2017
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32. Site preference and diffusion behaviors of H influenced by the implanted-He in 3C-\b{eta} SiC

Author

Wang, Sen, He, H. Y., Ding, R., Pan, B. C., and Chen, J. L.

Subjects
Condensed Matter - Materials Science
Abstract

SiC materials are potential plasma facing materials in fusion reactors. In this study, site preference and diffusion behaviors of H in pure 3C-\b{eta} SiC and in He-implanted 3C-\b{eta} SiC are investigated, on the basis of the first-principles calculations. We find that the most stable sites for H in pure 3C-\b{eta}SiC is the anti-bond site of C (ABc) in Si-C, while it becomes the bond-center (BC) site of Si-C bonds in the He-implanted 3C-\b{eta} SiC. Analysis on the electronic structures reveals that such change is attributed to the reduction of hybridization of C-Si bonds induced by He. Moreover, the presence of He strongly affect the vibrational features in the high frequency region, causing a blue shift of 25 cm-1 for C-H stretch mode with H at ABc site and a red shift of 165cm-1 for that at BC site, with respect to that in the pure system. In pure 3C-\b{eta} SiC, H is diffusive with an energy cost of about 0.5 eV, preferring to rotate around the C atom in a Si-C tetrahedron with an energy barrier of just about 0.10 eV. In contrast, in He-implanted 3C-\b{eta} SiC, the energy barriers for H migration goes up to be about 0.95 eV, indicating the implanted-He blocks the diffusive H to some extent. Our calculations also show that the influence of He on H diffusion is effective in a short range, just covering the nearest neighbor.

Published
2017

33. The DArk Matter Particle Explorer mission

Author

Chang, J., Ambrosi, G., An, Q., Asfandiyarov, R., Azzarello, P., Bernardini, P., Bertucci, B., Cai, M. S., Caragiulo, M., Chen, D. Y., Chen, H. F., Chen, J. L., Chen, W., Cui, M. Y., Cui, T. S., D'Amone, A., De Benedittis, A., De Mitri, I., Di Santo, M., Dong, J. N., Dong, T. K., Dong, Y. F., Dong, Z. X., Donvito, G., Droz, D., Duan, K. K., Duan, J. L., Duranti, M., D'Urso, D., Fan, R. R., Fan, Y. Z., Fang, F., Feng, C. Q., Feng, L., Fusco, P., Gallo, V., Gan, F. J., Gan, W. Q., Gao, M., Gao, S. S., Gargano, F., Gong, K., Gong, Y. Z., Guo, J. H., Hu, Y. M., Huang, G. S., Huang, Y. Y., Ionica, M., Jiang, D., Jiang, W., Jin, X., Kong, J., Lei, S. J., Li, S., Li, X., Li, W. L., Li, Y., Liang, Y. F., Liang, Y. M., Liao, N. H., Liu, Q. Z., Liu, H., Liu, J., Liu, S. B., Liu, W. Q., Liu, Y., Loparco, F., Lü, J., Ma, M., Ma, P. X., Ma, S. Y., Ma, T., Ma, X. Q., Ma, X. Y., Marsella, G., Mazziotta, M. N., Mo, D., Miao, T. T., Niu, X. Y., Pohl, M., Peng, X. Y., Peng, W. X., Qiao, R., Rao, J. N., Salinas, M. M., Shang, G. Z., Shen, W. H., Shen, Z. Q., Shen, Z. T., Song, J. X., Su, H., Su, M., Sun, Z. Y., Surdo, A., Teng, X. J., Tian, X. B., Tykhonov, A., Vagelli, V., Vitillo, S., Wang, C., Wang, Chi, Wang, H., Wang, H. Y., Wang, J. Z., Wang, L. G., Wang, Q., Wang, S., Wang, X. H., Wang, X. L., Wang, Y. F., Wang, Y. P., Wang, Y. Z., Wen, S. C., Wang, Z. M., Wei, D. M., Wei, J. J., Wei, Y. F., Wu, D., Wu, J., Wu, S. S., Wu, X., Xi, K., Xia, Z. Q., Xin, Y. L., Xu, H. T., Xu, Z. L., Xu, Z. Z., Xue, G. F., Yang, H. B., Yang, J., Yang, P., Yang, Y. Q., Yang, Z. L., Yao, H. J., Yu, Y. H., Yuan, Q., Yue, C., Zang, J. J., Zhang, C., Zhang, D. L., Zhang, F., Zhang, J. B., Zhang, J. Y., Zhang, J. Z., Zhang, L., Zhang, P. F., Zhang, S. X., Zhang, W. Z., Zhang, Y., Zhang, Y. J., Zhang, Y. Q., Zhang, Y. L., Zhang, Y. P., Zhang, Z., Zhang, Z. Y., Zhao, H., Zhao, H. Y., Zhao, X. F., Zhou, C. Y., Zhou, Y., Zhu, X., Zhu, Y., and Zimmer, S.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Experiment, Physics - Instrumentation and Detectors
Abstract

The DArk Matter Particle Explorer (DAMPE), one of the four scientific space science missions within the framework of the Strategic Pioneer Program on Space Science of the Chinese Academy of Sciences, is a general purpose high energy cosmic-ray and gamma-ray observatory, which was successfully launched on December 17th, 2015 from the Jiuquan Satellite Launch Center. The DAMPE scientific objectives include the study of galactic cosmic rays up to $\sim 10$ TeV and hundreds of TeV for electrons/gammas and nuclei respectively, and the search for dark matter signatures in their spectra. In this paper we illustrate the layout of the DAMPE instrument, and discuss the results of beam tests and calibrations performed on ground. Finally we present the expected performance in space and give an overview of the mission key scientific goals., Comment: 45 pages, including 29 figures and 6 tables. Published in Astropart. Phys

Published
2017
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34. Anisotropy in the thermal hysteresis of resistivity and charge density wave nature of single crystal SrFeO3-delta: X-ray absorption and photoemission studies

Author

Hsieh, S. H., Solanki, R. S., Wang, Y. F., Shao, Y. C., Lee, S. H., Yao, C. H., Du, C. H., Wang, H. T., Chiou, J. W., Chin, Y. Y., Tsai, H. M., Chen, J. -L., Pao, C. W., Cheng, C. -M., Chen, W. -C., Lin, H. J., Lee, J. F., Chou, F. C., and Pong, W. F.

Subjects
Condensed Matter - Strongly Correlated Electrons
Abstract

The local electronic and atomic structures of the high-quality single crystal of SrFeO3-{delta} ({delta}~0.19) were studied using temperature-dependent x-ray absorption and valence-band photoemission spectroscopy (VB-PES) to investigate the origin of anisotropic resistivity in the ab-plane and along the c-axis close to the region of thermal hysteresis (near temperature for susceptibility maximum, Tm~78 K). All experiments herein were conducted during warming and cooling processes. The Fe L3,2-edge X-ray linear dichrois results show that during cooling from room temperature to below the transition temperature, the unoccupied Fe 3d eg states remain in persistently out-of-plane 3d3z2-r2 orbitals. In contrast, in the warming process below the transition temperature, they change from 3d3z2-r2 to in-plane 3dx2-y2 orbitals. The nearest-neighbor (NN) Fe-O bond lengths also exhibit anisotropic behavior in the ab-plane and along the c-axis below Tm. The anisotropic NN Fe-O bond lengths and Debye-Waller factors stabilize the in-plane Fe 3dx2-y2 and out-of-plane 3d3z2-r2 orbitals during warming and cooling, respectively. Additionally, a VB-PES study further confirms that a relative band gap opens at low temperature in both the ab-plane and along the c-axis, providing the clear evidence of the charge-density-wave nature of SrFeO3-{delta} ({delta}~ 0.19) single crystal., Comment: 45 pages, 7 figures

Published
2017

37. The mode switching of PSR B2020+28

Author

Wen, Z. G., Wang, N., Yan, W. M., Yuan, J. P., Liu, Z. Y., Chen, M. Z., and Chen, J. L.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

This paper reports on polarimetric radiation properties based on the switching modes of normal PSR B2020+28 by analysing the data acquired from the Nanshan 25-m radio telescope at 1556 MHz. With nearly 8 hours quasi-continuous observation, the data presented some striking and updated phenomena. The change of relative intensity between the leading and trailing components is the predominant feature of mode switching. The intensity ratio between the leading and trailing components are measured for the individual profiles averaged over 30 seconds. It is found that there is an excess of high ratios over the normal distribution, which indicates that two modes exist in the pulsar. The distribution of abnormal mode has a narrower width indicating that the abnormal mode is more stable than the normal mode. A total of 76 mode switching events are detected in our data. It spends 89\% in the normal mode and 11\% in the abnormal mode. The intrinsic distributions of mode timescales are constrained with power-law distributions. The significant difference in the index of the duration distribution between normal and abnormal modes possibly indicates that the timescale for the abnormal mode to get stable is shorter than that for the normal mode. The frequent switching between both modes may indicate that the oscillations between different magnetospheric states are rapid.

Published
2016
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39. Lack of association between classical HLA genes and asymptomatic SARS-CoV-2 infection

Author

Marchal, A, Cirulli, E, Neveux, I, Bellos, E, Thwaites, R, Schiabor Barrett, K, Zhang, Y, Nemes-Bokun, I, Kalinova, M, Catchpole, A, Tangye, S, Spaan, A, Lack, J, Ghosn, J, Burdet, C, Gorochov, G, Tubach, F, Hausfater, P, Abel, L, Aiuti, A, Al-Muhsen, S, Al-Mulla, F, Amara, A, Anderson, M, Andreakos, E, Arias, A, Arkin, L, Feldman, H, Bastard, P, Belot, A, Biggs, C, Bogunovic, D, Bolze, A, Bondarenko, A, Borghesi, A, Bousfiha, A, Brodin, P, Bryceson, Y, Butte, M, Casanova, J, Casari, G, Christodoulou, J, Cobat, A, Colobran, R, Condino-Neto, A, Constantinescu, S, Cooper, M, Dalgard, C, Desai, M, Drolet, B, Duval, X, El Baghdadi, J, Eloy, P, Espinosa-Padilla, S, Fellay, J, Flores, C, Franco, J, Froidure, A, Gregersen, P, Grimbacher, B, Haerynck, F, Hagin, D, Halwani, R, Hammarstrom, L, Heath, J, Hsieh, E, Husebye, E, Imai, K, Itan, Y, Jouanguy, E, Kaja, E, Karamitros, T, Kisand, K, Ku, C, Lau, Y, Ling, Y, Lucas, C, Maniatis, T, Mansouri, D, Marodi, L, Mentre, F, Meyts, I, Milner, J, Mironska, K, Mogensen, T, Morio, T, Ng, L, Notarangelo, L, Novelli, A, Novelli, G, O'Farrelly, C, Okada, S, Okamoto, K, Ozcelik, T, Pan-Hammarstrom, Q, Pape, J, Perez de Diego, R, Perez-Tur, J, Perlin, D, Pesole, G, Planas, A, Prando, C, Pujol, A, Puel, A, Quintana-Murci, L, Ramaswamy, S, Renia, L, Resnick, I, Rodriguez-Gallego, C, Sancho-Shimizu, V, Sediva, A, Seppanen, M, Shahrooei, M, Shcherbina, A, Slaby, O, Snow, A, Soler-Palacin, P, Soumelis, V, Tancevski, I, Tayoun, A, Temel, S, Thorball, C, Tiberghien, P, Trouillet-Assant, S, Turvey, S, Uddin, K, Uddin, M, van de Beek, D, Vinh, D, von Bernuth, H, Wauters, J, Zatz, M, Zawadzki, P, Zhang, Q, Zhang, S, Bureau, S, Vacher, Y, Gysembergh-Houal, A, Demerville, L, Benleulmi-Chaachoua, A, Abad, S, Abassi, R, Abdellaoui, A, Abdelmalek, A, Abdoul, H, Abergel, H, Abeud, F, Abgrall, S, Abisror, N, Adechian, M, Aderdour, N, Admane, H, Adnet, F, Afritt, S, Agostini, H, Aguilar, C, Agut, S, Aiello, T, Kaci, M, Oufella, H, Ajeenthiravasan, G, Alauzy, V, Alby-Laurent, F, Allard, L, Alyanakian, M, Borrero, B, Amam, S, Amrouche, L, Andronikof, M, Anglicheau, D, Anguel, N, Annane, D, Aounzou, M, Aparicio, C, Aratus, G, Arlet, J, Arzoine, J, Aslangul, E, Assefi, M, Aubry, A, Audiffred, L, Audureau, E, Auger, C, Auregan, J, Awotar, C, Milla, S, Azan, D, Azemar, L, Azzouguen, B, Elrufaai, M, Badsi, A, Bakouboula, P, Balcerowiak, C, Balde, F, Baldivia, E, Bangamingo, E, Baptiste, A, Baran-Marszak, F, Barau, C, Barget, N, Baronnet, F, Barthelemy, R, Baudel, J, Baudry, C, Baudry, E, Beaugerie, L, Belamri, A, Belaube, N, Belilita, R, Bellassen, P, Belmokhtar, R, Beltran, I, Benainous, R, Benallaoua, M, Benamouzig, R, Benbara, A, Benhida, J, Benkhelouf, A, Benlagha, J, Benmostafa, C, Benothmane, S, Bentifraouine, M, Berard, L, Bernier, Q, Berti, E, Bertier, A, Berton, L, Bessis, S, Beurton, A, Bianco, C, Bianquis, C, Bidar, F, Blanche, P, Blayau, C, Bleibtreu, A, Blin, E, Bloch-Queyrat, C, Boissier, M, Bollens, D, Bolzoni, M, Bompard, R, Bonnet, N, Bonnouvrier, J, Botha, S, Boucenna, W, Bouchama, F, Bouchaud, O, Bouchghoul, H, Boudjebla, T, Boudjema, N, Bouffard, C, Bougle, A, Bouguerra, M, Bouras, L, Bourcier, A, Durand, A, Bourrier, A, Bouscarat, F, Bouvry, D, Bouziri, N, Bouzrara, O, Bribier, S, Brugier, D, Brunel, M, Bui, E, Buisson, A, Bukreyeva, I, Bureau, C, Cadranel, J, Cailhol, J, Calin, R, Vega, C, Canavaggio, P, Cancella, M, Cantin, D, Cao, A, Carbillon, L, Carlier, N, Cassard, C, Castor, G, Cauchy, M, Cha, O, Chaigne, B, Challal, S, Champion, K, Chariot, P, Chas, J, Chauveau, S, Chauvin, A, Chauvin, C, Chavarot, N, Chebbout, K, Cherai, M, Cherubini, I, Chevalier, A, Chiarabini, T, Chinet, T, Chocron, R, Choinier, P, Chommeloux, J, Choquet, C, Choupeaux, L, Chousterman, B, Ciocan, D, Clarke, A, Clavere, G, Clavier, F, Clement, K, Clerc, S, Cohen, Y, Cohen, F, Cohen, A, Coilly, A, Colboc, H, Colin, P, Collet, M, Comarmond, C, Combacon, E, Combes, A, Comparon, C, Constantin, J, Cordel, H, Cordier, A, Costantini, A, Chalumeau, N, Couffignal, C, Coupeau, D, Creange, A, Lamarre, Y, Da Silveira, C, Guibal El Kayani, S, De Castro, N, De Rycke, Y, Del Pozo, L, Delannoy, Q, Delay, M, Deleris, R, Delforge, J, Delphine, L, Demare, N, Demeret, S, Demoule, A, Deniau, A, Depret, F, Derolez, S, Derradji, O, Derridj, N, Descamps, V, Deschamps, L, Desconclois, C, Desnos, C, Desongins, K, Dhote, R, Diallo, B, Didier, M, Diemer, M, Diez, S, Djadi-Prat, J, Djamouri Monnory, F, Djebara, S, Djebra, N, Djietcheu, M, Djillali, H, Djouadi, N, Donneger, S, Santos, C, Dournon, N, Dres, M, Droctove, L, Drogrey, M, Dropy, M, Drouet, E, Dubosq, V, Dubreucq, E, Dubus, E, Duchemann, B, Duchenoy, T, Dudoignon, E, Dufau, R, Dumas, F, Duran, C, Duron, E, Durrbach, A, Duvivier, C, Ebstein, N, El Khalifa, J, Elabbadi, A, Elie, C, Ernotte, G, Esling, A, Etienne, M, Eyer, X, Fartoukh, M, Fayali, T, Fermaut, M, Fiorentino, A, Fliss, S, Fournier, M, Fournier, B, Francois, H, Freynet, O, Frigout, Y, Fromont, I, Fuentes, 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S., Fayali T., Fermaut M., Fiorentino A., Fliss S., Fournier M. -C., Fournier B., Francois H., Freynet O., Frigout Y., Fromont I., Fuentes A., Furet T., Galand J., Garnier M., Gaubert A., Gaudry S., Gaugain S., Gauthier D., Gautier M., Georgin-Lavialle S., Geromin D., Ghalayini M., Ghaleh B., Ghezal M., Gibelin A., Gimeno L., Girard B., Leprieur B. G., Gomes D., Gomes-Pires E., Gouge A., Gouja A., Goulet H., Goupil S., De Bouille J. G., Gras J., Greffe S., Grimaldi L., Guedeney P., Guidet B., Guillo M., Gulczynski M., Hadjam T., Haguenauer D., Hammal S., Hammoudi N., Hanon O., Harrois A., Hautem C., Hekimian G., Heming N., Hermine O., Ho S., Houllier M., Huot B., Huscenot T., Saied W. I., Ikherbane G., Imarazene M., Ingiliz P., Iratni L., Jaureguiberry S., Jean-Marc J. -F., Jeyarajasingham D., Jouany P., Jouis V., Jourdaine C., Kafif O., Kallala R., Katsahian S., Kelesyan L., Keo V., Ketz F., Khamis W., Khelili E., Khellaf M., Kotokpo Youkou C. G., Kounis I., Kpalma G., Krause J., Labbe V., Lacombe K., Lacorte J. -M., Lafont A. G., Lafont E., Lagha L., Lamhaut L., Lancelot A., Landman C., Lanternier F., Larcheveque C., Combe C. L., Lassel L., Laverdant B., Lavergne C., Lavillegrand J. -R., Lazureanu P., Le Guennec L., Leberre L., Leblanc C., Leboyer M., Lecomte F., Lecorre M., Leenhardt R., Lefebvre M., Lefebvre B., Legendre P., Leger A., Legros L., Legrosse J., Lehuunghia S., Lemarec J., Leporrier-Ext J., Lesein M., Lesur H., Levy V., Levy A., Lopes E., Lopes A., Lopez V., Lopinto J., Lortholary O., Louadah B., Loze B., Lucas M. -L., Lucasamichi A., Luong L. B., Magazimama-Ext A., Maingret D., Mameri L., Manivet P., Mansouri C., Marcault E., Marey J., Marin N., Marois C., Martin O., Martineau L., Martinez-Lopez C., Martyniuck P., De Farcy P. M., Marzouk N., Masmoudi R., Mebazaa A., Mechai F., Mecozzi F., Mediouni C., Megarbane B., Meghadecha M., Mejean E., Mekinian A., Abdelhadi N. M., Mekni R., Meliti T. S., Lima B. M., Meng P., Merbah S., Messani F., Messaoudi Y., Mewasing B. -I., Meziane L., Michelot-Burger C., Mignot F., Minka F. H., Miyara M., Moine P., Molina J. -M., Montegnies-Boulet A., Monti A., Montlahuc C., Montout A. -L., Moores A., Morbieu C., Mortelette H., Mouly S., Muzaffar R., Nacerddine C. I., Nadal M., Nadif H., Nassarmadji K., Natella P., Ndingamondze S., Neraal S., Nguyen C., N'Guyen B., Larmurier I. N., Nlomenyengue L., Noel N., Nunes H., Omar E., Ouazene Z., Ouedraogo E., Ouelaa W., Oukhedouma A., Amara Y. O., Oya H., Oziel J., Padilla T., Paillaud E., Paiva S., Parfait B., Parize P., Parizot C., Parrot A., Pavot A., Peaudecerf L., Pene F., Pepin M., Pernet J., Pernin C., Petit M., Peyrony O., Pietri M. -P., Pietri O., De Chambrun M. 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U., Uzunhan Y., Vaittinadaayar P., Valent A., Valentian M., Valin N., Vallet H., Vaz M., Vazquezibarra M. -A., Vedie B., Velly L., Verstuyft C., Viallette C., Vicaut E., Vignes D., Vimpere D., Virlouvet M., Voiriot G., Voisot L., Weiss E., Weiss N., Winchenne A., Yordanov Y., Zafrani L., Zaidan M., Zaidi W., Zak C., Zarhrate-Ghoul A., Zatout O., Zeino S., Zeitouni M., Zemirli N., Zerah L., Zia O., Ziol M., Zolario O., Zuber J., Andrejak C., Angoulvant F., Bachelet D., Bartoli M., Basmaci R., Behillil S., Beluze M., Benkerrou D., Bhavsar K., Bouadma L., Bouchez S., Bouscambert M., Cervantes-Gonzalez M., Chair A., Chirouze C., Coelho A., Couffin-Cadiergues S., d'Ortenzio E., Debray M. -P., Deconinck L., Deplanque D., Descamps D., Desvallee M., Diallo A., Diouf A., Dorival C., Dubos F., Elharrar B., Enouf V., Esperou H., Esposito-Farese M., Devouge E. F., Gault N., Gaymard A., Gigante T., Gilg M., Guedj J., Hoctin A., Hoffmann I., Houas I., Hulot J. -S., Jaafoura S., Kaguelidou F., Kali S., Khalil A., Khan C., Laouenan C., Laribi S., Le M., Le Hingrat Q., Le Mestre S., Le Nagard H., Lescure F. -X., Letrou S., Levy Y., Lina B., Lingas G., Lucet J. -C., Malvy D., Mambert M., Meziane A., Mouquet H., Mullaert J., Neant N., Nguyen D., Noret M., Nseir S., Papadopoulos A., Paul C., Peiffer-Smadja N., Perpoint T., Petrov-Sanchez V., Peytavin G., Pham H., Picone O., Puechal O., Rabaud C., Rosa-Calatrava M., Rossignol B., Rossignol P., Roy C., Schneider M., Su R., Tardivon C., Tellier M. -C., Teoule F., Terrier O., Timsit J. -F., Tual C., van der Werf S., Vanel N., Veislinger A., Visseaux B., Wiedemann A., Yazdanpanah Y., Alavoine L., Charpentier C., Dechanet A., Ecobichon J. -L., Frezouls W., Houhou N., Lehacaut J., Manchon P., Nouroudine M., Quintin C., Thy M., Vignali V., Chahine A., Waucquier N., Migaud M. -C., Djossou F., Mergeay-Fabre M., Lucarelli A., Demar M., Bruneau L., Gerardin P., Maillot A., Payet C., Laviolle B., Laine F., Paris C., Desille-Dugast M., Fouchard J., Pistone T., Perreau P., Gissot V., Goas C. 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Abstract

Human genetic studies of critical COVID-19 pneumonia have revealed the essential role of type I interferon-dependent innate immunity to SARS-CoV-2 infection. Conversely, an association between the HLA-B∗15:01 allele and asymptomatic SARS-CoV-2 infection in unvaccinated individuals was recently reported, suggesting a contribution of pre-existing T cell-dependent adaptive immunity. We report a lack of association of classical HLA alleles, including HLA-B∗15:01, with pre-omicron asymptomatic SARS-CoV-2 infection in unvaccinated participants in a prospective population-based study in the United States (191 asymptomatic vs. 945 symptomatic COVID-19 cases). Moreover, we found no such association in the international COVID Human Genetic Effort cohort (206 asymptomatic vs. 574 mild or moderate COVID-19 cases and 1,625 severe or critical COVID-19 cases). Finally, in the Human Challenge Characterisation study, the three HLA-B∗15:01 individuals infected with SARS-CoV-2 developed symptoms. As with other acute primary infections studied, no classical HLA alleles favoring an asymptomatic course of SARS-CoV-2 infection were identified.

Published
2024

40. Design and construction of a multi-layer CsI(Tl) telescope for high-energy reaction studies

Author

Yan, D., Sun, Z. Y., Yue, K., Wang, S. T., Zhang, X. H., Yu, Y. H., Chen, J. L., Tang, S. W., Fang, F., Zhou, Y., Sun, Y., Wang, Z. M., and Sun, Y. Z.

Subjects
Physics - Instrumentation and Detectors
Abstract

A prototype of a new CsI(Tl) telescope, which will be used in the reaction studies of light isotopes with energy of several hundred AMeV, has been constructed and tested at the Institute of Modern Physics, Chinese Academy of Sciences. The telescope has a multi-layer structure and the range information will be obtained to improve the particle identification performance. This prototype has seven layers of different thickness. A 5.0% (FWHM) energy resolution has been extracted for one of the layers in a beam test experiment. Obvious improvement for the identification of $^{14}$O and $^{15}$O isotopes was achieved by using the range information.

Published
2015

41. Molecular-beam epitaxy of monolayer and bilayer WSe2: A scanning tunneling microscopy/spectroscopy study and deduction of exciton binding energy

Author

Liu, H. J., Jiao, L., Xie, L., Yang, F., Chen, J. L., Ho, W. K., Gao, C. L., Jia, J. F., Cui, X. D., and Xie, M. H.

Subjects
Condensed Matter - Materials Science
Abstract

Interests in two-dimensional transition-metal dichalcogenides have prompted some recent efforts to grow ultrathin layers of these materials epitaxially using molecular-beam epitaxy. However, growths of monolayer and bilayer WSe2, an important member of the transition-metal dichalcogenides family, by the molecular-beam epitaxy method remain uncharted probably because of the difficulty in generating tungsten fluxes from the elemental source. In this work, we present a scanning tunneling microscopy and spectroscopy study of molecular-beam epitaxy-grown WSe2 monolayer and bilayer, showing atomically flat epifilm with no domain boundary defect. This contrasts epitaxial MoSe2 films grown by the same method, where a dense network of the domain boudaries defects is present. The scanning tunneling spectroscopy measurements of monolayer and bilayer WSe2 domains of the same sample reveal not only the bandgap narrowing upon increasing the film thickness from monolayer to bilayer, but also a band-bending effect across the boundary between monolayer and bilayer domains. This band-bending appears to be dictated by the edge states at steps of the bilayer islands. Finally, comparison is made between the scanning tunneling spectroscopy-measured electronic bandgaps with the exciton emission energies measured by photoluminescence, and the exciton binding energies in monolayer and bilayer WSe2/MoSe2 are thus estimated.

Published
2015
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42. INFLUENCE OF RAINFALL SPATIAL VARIABILITY ON RUNOFF SIMULATION IN HILLY IRRIGATION AREAS.

Author

CHEN, J. L., LUO, W. B., WANG, W. J., YU, L., LI, Y. L., ZOU, Z. K., HAN, X. D., and HUANG, S. Z.

Subjects
VORONOI polygons, RUNOFF, RAINFALL, HYDROLOGIC models, WATERSHEDS
Abstract

Rainfall spatial variability is a crucial factor determining rainfall input in hydrological models and it significantly affects model simulation accuracy. We selected the Yangshudang watershed in the Zhanghe irrigation district of Yangtze River Basin of China to assess the impact of rainfall spatial variability on SWAT runoff simulation in hilly irrigation areas. Eight different rainfall station network distributions were established and rainfall data were processed, using the SWAT model nearest and Thiessen polygon interpolation methods to analyze rainfall spatial variations in the study area. This study investigated the effects of the number, layout, and rainfall grades of rainfall gauges on runoff simulation performance. The results indicated that a higher number of rainfall gauges and more uniform spatial distribution leads to better runoff simulation performance. Among the scenarios examined, using three rainfall gauges yielded the best results, with R2, NSE, and RSR values of 0.84, 0.81, and 0.44, respectively. Employing Thiessen polygon interpolation with three rainfall gauges the R2 value increased to 0.87, enhancing it by 3.57% and further reducing the simulation errors caused by rainfall spatial variability. Additionally, runoff simulation under different rainfall grades exhibited varying responses to rainfall spatial variability, with minimal impact observed during light rainfall and the greatest impact during moderate and heavy rainfall events. [ABSTRACT FROM AUTHOR]

Published
2024
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46. Investigation of Periodic Modulation Behaviors from Pulsar J2022+5154

Author

Chen, J. L., primary, Wen, Z. G., additional, Wang, Z., additional, Duan, X. F., additional, He, D. L., additional, Wang, N., additional, Wang, H. G., additional, Yuan, J. P., additional, Huang, L., additional, Lyu, C. B., additional, Yuen, R., additional, Yan, W. M., additional, Wu, Z. W., additional, Han, W., additional, Xiang, B. B., additional, and Dong, A. J., additional

Published
2024
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47. Corrigendum to “A2B5-positive oligodendrocyte precursor cell transplantation improves neurological deficits in rats following spinal cord contusion associated with changes in expression of factors involved in the Notch signaling pathway” [Neurochirurgie 68 (2) (2022) 188–95]

Author

Yuan, H., primary, Fang, C.-L., additional, Deng, Y.-P., additional, Huang, J., additional, Niu, R.-Z., additional, Chen, J.-L., additional, Chen, T.-B., additional, Zhu, Z.-Q., additional, Chen, L., additional, Xiong, L.-L., additional, and Wang, T.-H., additional

Published
2024
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49. Effects of genetic correction on the differentiation of hair cell-like cells from iPSCs with MYO15A mutation.

Author

Chen, J-R, Tang, Z-H, Zheng, J, Shi, H-S, Ding, J, Qian, X-D, Zhang, C, Chen, J-L, Wang, C-C, Li, L, Chen, J-Z, Yin, S-K, Shao, J-Z, Huang, T-S, Chen, P, Guan, M-X, and Wang, J-F

Subjects
Fibroblasts, Dermis, Humans, Myosins, Transcription Factors, Pedigree, Cell Differentiation, Base Sequence, Mutation, Polymorphism, Single Nucleotide, Child, Preschool, Female, Male, GATA3 Transcription Factor, PAX2 Transcription Factor, Hair Cells, Auditory, Inner, Induced Pluripotent Stem Cells, CRISPR-Cas Systems, Cellular Reprogramming, PAX8 Transcription Factor, Regenerative Medicine, Neurosciences, Biotechnology, Stem Cell Research - Induced Pluripotent Stem Cell, Stem Cell Research, Genetics, Stem Cell Research - Induced Pluripotent Stem Cell - Human, 2.1 Biological and endogenous factors, 1.1 Normal biological development and functioning, Underpinning research, Aetiology, 5.2 Cellular and gene therapies, Development of treatments and therapeutic interventions, Ear, Biological Sciences, Medical and Health Sciences, Biochemistry & Molecular Biology
Abstract

Deafness or hearing loss is a major issue in human health. Inner ear hair cells are the main sensory receptors responsible for hearing. Defects in hair cells are one of the major causes of deafness. A combination of induced pluripotent stem cell (iPSC) technology with genome-editing technology may provide an attractive cell-based strategy to regenerate hair cells and treat hereditary deafness in humans. Here, we report the generation of iPSCs from members of a Chinese family carrying MYO15A c.4642G>A and c.8374G>A mutations and the induction of hair cell-like cells from those iPSCs. The compound heterozygous MYO15A mutations resulted in abnormal morphology and dysfunction of the derived hair cell-like cells. We used a CRISPR/Cas9 approach to genetically correct the MYO15A mutation in the iPSCs and rescued the morphology and function of the derived hair cell-like cells. Our data demonstrate the feasibility of generating inner ear hair cells from human iPSCs and the functional rescue of gene mutation-based deafness by using genetic correction.

Published
2016

50. Frequency dependence of pulse width for 150 radio normal pulsars

Author

Chen, J. L. and Wang, H. G.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

The frequency dependence of pulse width is studied for 150 normal pulsars, mostly selected from the European Pulsar Network, for which the 10\% multifrequency pulse widths can be well fit with the Thorsett relationship W_{10}=A\nu^{\mu}+W_{\rm 10, min}. The relative fraction of pulse width change between 0.4~GHz and 4.85~GHz, \eta=(W_{4.85}-W_{0.4})/W_{0.4}, is calculated in terms of the best-fit relationship for each pulsar. It is found that 81 pulsars (54\%) have $\eta<-10$\% (group A), showing considerable profile narrowing at high frequencies, 40 pulsars (27\%) have $-$10\%$\leq\eta\leq 10$\% (group B), meaning a marginal change in pulse width, and 29 pulsars (19\%) have $\eta>10$\% (group C), showing a remarkable profile broadening at high frequencies. The fractions of the group-A and group-C pulsars suggest that the profile narrowing phenomenon at high frequencies is more common than the profile broadening phenomenon, but a large fraction of the group-B and group-C pulsars (a total of 46\%) is also revealed. The group-C pulsars, together with a portion of group-B pulsars with a slight pulse broadening, can hardly be explained using the conventional radius-to-frequency mapping, which only applies to the profile narrowing phenomenon. Based on a recent version of the fan beam model, a type of broadband emission model, we propose that the diverse frequency dependence of pulse width is a consequence of different types of distribution of emission spectra across the emission region. The geometrical effect predicting a link between the emission beam shrinkage and the spectrum steepening is tested but disfavored., Comment: 15 figures,7 tables, Published in ApJS

Published
2014
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