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13,684 results on '"You Y."'

1. Carbonitriding reduction of TiO2 in the CH4-H2-N2 system: Reduction temperature effect and kinetics

Author

Zhang R., Fan G.-Q., Hou Y., You Y., and Dang J.

Subjects
ti(c, o), tio2, kinetics, ch4-h2-n2 gas mixture, Mining engineering. Metallurgy, TN1-997
Abstract

Understanding reaction kinetics can provide valuable information for the design and optimization of a reaction process. In this study, the reduction degree and carbonitriding ratio of TiO2 in the CH4-H2-N2 system were investigated to understand the kinetics of carbonitriding reduction. The experimental results revealed the following important findings. The reduction degree of TiO2 increased significantly within the temperature range of 1000°C to 1200°C. At the same time, the duration of complete carbonitride time decreased with increasing temperature. However, it was found that excessively high temperatures (1200°C) had a detrimental effect on the degree of reduction. Consequently, the optimal reduction temperature was set at 1100°C, in order to achieve a balance between reduction degree and reaction time. The process of carbonitride reduction of TiO2 in the CH4-H2-N2 system corresponded to the unreacted nuclear model, where the process was mainly controlled by chemical reactions. A calculated apparent activation energy of 99.35 kJ/mol was obtained for the carbonitriding reduction process. The identification of the optimal reduction temperature and the dominant role of chemical reactions provide valuable insights for the design and optimization of carbonitriding processes with titanium compounds.

Published
2024
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3. Isobaric (vapour + liquid) equilibria of binary Pb-Sn and Sb-Sn system AT2Pa

Author

Gao J., Xu J., Yang B., Kong L., Xu B., and You Y.

Subjects
new experimental method, VLE, Pb-Sn, Sb-Sn alloys, MIVM, thermodynamic consistency test, Mining engineering. Metallurgy, TN1-997
Abstract

A new experimental method for determining vapor-liquid equilibrium (VLE) of binary alloys was designed in this study. The VLE data of Pb-Sn and Sb-Sn alloys were determined by using this new method. The experimental data passed the thermodynamic consistency test (Van Ness test), and the y(MAD) was 0.4066 and 0.6667, respectively, indicating that the experimental method is correct and reliable. The activity coefficient of Pb-Sn and Sb-Sn alloys was calculated by using the molecular interaction volume model (MIVM). The maximum average relative deviation Si and maximum average standard deviation Si* are ±1.34% and ±0.009, respectively, which indicates that the calculation of the activity coefficient of the Pb- Sn and Sb-Sn alloys by MIVM is reliable. The VLE data of Pb-Sn and Sb-Sn alloys were calculated based on the VLE theory and MIVM, and the calculated results agreed well with the experimental VLE data. The VLE phase diagrams of Pb-Sn and Sb-Sn alloys were also established in this study. The VLE phase diagrams offer a valid and intuitive way to analyze the product compositions’ dependence of temperature and pressure during the process of vacuum distillation. This will have immense significance in guiding the actual production of vacuum metallurgy.

Published
2018
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4. Pulsed Iron line Emission from the First Galactic Ultraluminous X-ray Pulsar Swift J0243.6+6124

Author

Xiao, Y. X., Xu, Y. J., Ge, M. Y., Lu, F. J., Zhang, S. N., Zhang, S., Tao, L., Qu, J. L., Wang, P. J., Kong, L. D., Tuo, Y. L., You, Y., Zhao, S. J., Peng, J. Q., Du, Y. F., Zhang, Y. H., and Ye, W. T.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We report the phase-resolved spectral results of the first Galactic Pulsating Ultra-Luminous X-ray source (PULX) Swift J0243.6+6124, modeling at its 2017-2018 outburst peak using data collected by the Hard X-ray Modulation Telescope (Insight-HXMT). The broad energy coverage of Insight-HXMT allows us to obtain more accurate spectral continuum to reduce the coupling of broad iron line profiles with other components. We use three different continuum spectrum models but obtain similar iron line results. For the first time, we detected the pulse characteristics of the broad iron line in a PULX. The variation in width and intensity of this iron line with $\sigma \sim 1.2-1.5$\,keV has a phase offset of about 0.25 from the pulse phase. We suggest that the uneven irradiation of the thick inner disk by the accretion column produces the modulated variation of the broad iron line. In addition, the non-pulsed narrow line is suggested to come from the outer disk region.

Published
2024

6. Prospective Correlation of Magnetic Resonance Tumor Regression Grade With Pathologic Outcomes in Total Neoadjuvant Therapy for Rectal Adenocarcinoma.

Author

Hall, William, Li, Jiahe, You, Y, Gollub, Marc, Grajo, Joseph, Rosen, Mark, dePrisco, Greg, Yothers, Greg, Dorth, Jennifer, Rahma, Osama, Russell, Marcia, Gross, Howard, Jacobs, Samuel, Faller, Bryan, George, Sagila, Al Baghdadi, Tareq, Haddock, Michael, Valicenti, Richard, Hong, Theodore, and George, Thomas

Subjects
Female, Humans, Male, Middle Aged, Adenocarcinoma, Chemoradiotherapy, Magnetic Resonance Imaging, Magnetic Resonance Spectroscopy, Neoadjuvant Therapy, Neoplasm Staging, Rectal Neoplasms, Treatment Outcome, Prospective Studies
Abstract

PURPOSE: Total neoadjuvant therapy (TNT) is a newly established standard treatment for rectal adenocarcinoma. Current methods to communicate magnitudes of regression during TNT are subjective and imprecise. Magnetic resonance tumor regression grade (MR-TRG) is an existing, but rarely used, regression grading system. Prospective validation of MR-TRG correlation with pathologic response in patients undergoing TNT is lacking. Utility of adding diffusion-weighted imaging to MR-TRG is also unknown. METHODS: We conducted a multi-institutional prospective imaging substudy within NRG-GI002 (ClinicalTrials.gov identifier: NCT02921256) examining the ability of MR-based imaging to predict pathologic complete response (pCR) and correlate MR-TRG with the pathologic neoadjuvant response score (NAR). Serial MRIs were needed from 110 patients. Three radiologists independently, then collectively, reviewed each MRI for complete response (mriCR), which was tested for positive predictive value (PPV), negative predictive value (NPV), sensitivity, and specificity with pCR. MR-TRG was examined for association with the pathologic NAR score. All team members were blinded to pathologic data. RESULTS: A total of 121 patients from 71 institutions met criteria: 28% were female (n = 34), 84% White (n = 101), and median age was 55 (24-78 years). Kappa scores for T- and N-stage after TNT were 0.38 and 0.88, reflecting fair agreement and near-perfect agreement, respectively. Calling an mriCR resulted in a kappa score of 0.82 after chemotherapy and 0.56 after TNT reflected near-perfect agreement and moderate agreement, respectively. MR-TRG scores were associated with pCR (P < .01) and NAR (P < .0001), PPV for pCR was 40% (95% CI, 26 to 53), and NPV was 84% (95% CI, 75 to 94). CONCLUSION: MRI alone is a poor tool to distinguish pCR in rectal adenocarcinoma undergoing TNT. However, the MR-TRG score presents a now validated method, correlated with pathologic NAR, which can objectively measure regression magnitude during TNT.

Published
2023

7. Monte-Carlo simulations on possible collimation effects of outflows to fan-beamed emission of ultraluminous accreting X-ray pulsars

Author

Hou, X., You, Y., Ji, L., Soria, R., Zhang, S. N., Ge, M. Y., Tao, L., Zhang, S., Feng, H., Zhou, M., Tuo, Y. L., Song, L. M., and Wang, J. C.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

Pulsating ultraluminous X-ray sources (PULXs) are accreting pulsars with apparent X-ray luminosity exceeding $10^{39}\, \rm erg\ s^{-1}$. We perform Monte-Carlo simulations to investigate whether high collimation effect (or strong beaming effect) is dominant in the presence of accretion outflows, for the fan beam emission of the accretion column of the neutron stars in PULXs. We show that the three nearby PULXs (RX J0209.6$-$7427, Swift J0243.6+6124 and SMC X-3), namely the three musketeers here, have their main pulsed emission not strongly collimated even if strong outflows exist. This conclusion can be extended to the current sample of extragalactic PULXs, if accretion outflows are commonly produced from them. This means that the observed high luminosity of PULXs is indeed intrinsic, which can be used to infer the existence of very strong surface magnetic fields of $\sim10^{13-14}$ G, possibly multipole fields. However, if strong outflows are launched from the accretion disks in PULXs as a consequence of disk spherization by radiation pressure, regular dipole magnetic fields of $\sim10^{12}$ G may be required, comparable to that of the three musketeers, which have experienced large luminosity changes from well below their Eddington limit ($2\times10^{38}\, \rm erg\ s^{-1}$ for a NS) to super-Eddington and their maximum luminosity fills the luminosity gap between Galactic pulsars and extragalactic PULXs., Comment: 26 pages, 8 figures, 1 table. Accepted by ApJ

Published
2022
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8. Fan beamed X-ray emission from 1 keV to above 130 keV from the ultraluminous X-ray pulsar RX J0209.6-7427 in the Small Magellanic Cloud

Author

Hou, X., Ge, M. Y., Ji, L., Zhang, S. N., You, Y., Tao, L., Zhang, S., Soria, R., Feng, H., Zhou, M., Tuo, Y. L., Song, L. M., and Wang, J. C.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We present detailed timing and spectral analyses of the transient X-ray pulsar RX J0209.6$-$7427 in the Small Magellanic Cloud during its 2019 giant outburst. With a better known distance than most galactic X-ray pulsars, its peak luminosity is determined to be $(1.11\pm0.06)\times 10^{39}\, \rm erg\ s^{-1}$; it is thus a {\it bonda fide} pulsating ultraluminous X-ray source (PULX). Owing to the broad energy band of \textit{Insight}-HXMT, its pulsed X-ray emission was detected from 1 keV up to the 130$-$180 keV band, which is the highest energy emission detected from any PULXs outside the Milky Way. This allows us to conclude that its main pulsed X-ray emission is from the "fan beam" of the accretion column, and its luminosity is thus intrinsic. We also estimate its magnetic field of (4.8$-$8.6)$\times10^{12}$ G or (1.7$-$2.2)$\times10^{13}$ G, from its spin evolution or transition in the accretion column structure during the outburst; we suggest that the two values of the magnetic field strength correspond to the dipole and multipole magnetic fields of the neutron star, similar to the recent discovery in the Galactic PULX Swift J0243.6+6124. Therefore, the nature of the neutron star and its ULX emission can be understood within the current theoretical frame of accreting neutron stars. This may have implications for understanding the nature of those farther away extragalactic PULXs., Comment: 31 pages, 14 figures, 5 tables. Accepted by ApJ

Published
2022

9. Long-term memory and synapse-like dynamics in two-dimensional nanofluidic channels

Author

Robin, P., Emmerich, T., Ismail, A., Niguès, A., You, Y., Nam, G. -H., Keerthi, A., Siria, A., Geim, A. K., Radha, B., and Bocquet, L.

Subjects
Condensed Matter - Soft Condensed Matter, Condensed Matter - Statistical Mechanics
Abstract

Fine-tuned ion transport across nanoscale pores is key to many biological processes such as neurotransmission. Recent advances have enabled the confinement of water and ions to two dimensions, unveiling transport properties unreachable at larger scales and triggering hopes to reproduce the ionic machinery of biological systems. Here we report experiments demonstrating the emergence of memory in the transport of aqueous electrolytes across (sub)nanoscale channels. We unveiled two types of nanofluidic memristors, depending on channel material and confinement, with memory from minutes to hours. We explained how large timescales could emerge from interfacial processes like ionic self-assembly or surface adsorption. Such behavior allowed us to implement Hebbian learning with nanofluidic systems. This result lays the ground for biomimetic computations on aqueous electrolytic chips.

Published
2022
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10. Transforming U.S. Particle Physics Education: A Snowmass 2021 Study

Author

Bitter, O., Hansen, E. V., Kravitz, S., Velan, V., and You, Y.

Subjects
Physics - Physics Education, Physics - Physics and Society
Abstract

The pursuit of knowledge in particle physics requires constant learning. As new tools become available, new theories are developed, and physicists search for new answers with ever-evolving methods. However, it is the case that formal educational systems serve as the primary training grounds for particle physicists. Graduate school (and undergraduate school to a lesser extent) is where researchers learn most of the technical skills required for research, develop scientific problem-solving abilities, learn how to establish themselves in their field, and begin developing their career. It is unfortunate, then, that the skills gained by physicists during their formal education are often mismatched with the skills actually required for a successful career in physics. We performed a survey of the U.S. particle physics community to determine the missing elements of graduate and undergraduate education and to gauge how to bridge these gaps. In this contributed paper, part of the 2021-22 Snowmass Community Planning Exercise, we report the results of this survey. We also recommend several specific community actions to improve the quality of particle physics education; the "community" here refers to physics departments, national labs, professional societies, funding agencies, and individual physicists., Comment: contribution to Snowmass 2021

Published
2022

12. Financial toxicity impact on younger versus older adults with cancer in the setting of care delivery

Author

Corrigan, Kelsey L, Fu, Shuangshuang, Chen, Ying‐Shiuan, Kaiser, Kelsey, Roth, Michael, Peterson, Susan K, Shih, Ya‐Chen T, Jagsi, Reshma, Giordano, Sharon H, Volk, Robert J, Yabroff, K Robin, Banegas, Mathew P, Acquati, Chiara, Conti, Rena M, Y., Hilary, Ku, Kimberly, You, Y Nancy, and Smith, Grace L

Subjects
Aging, Cancer, Clinical Research, Good Health and Well Being, Adaptation, Psychological, Adolescent, Adult, Aged, Cost of Illness, Financial Stress, Health Expenditures, Humans, Middle Aged, Neoplasms, Surveys and Questionnaires, Young Adult, cancer survivors, financial toxicity, health care disparities, neoplasms, young adult, Oncology and Carcinogenesis, Public Health and Health Services, Oncology & Carcinogenesis
Abstract

BackgroundYoung adults and other working-age adults with cancer are at risk for cancer-related financial toxicity (FT), including material hardships, depletion of coping resources, and psychological burden. This study compares FT domains in young adults (18-39 years old) (YAs), other working-age adults (40-64 years old), and older adults (≥65 years old) receiving cancer care.MethodsA total of 311 adults were surveyed using the multi-domain Economic Strain and Resilience in Cancer instrument measuring FT (0-10 score indicating least to greatest FT; score ≥5 severe FT). Participants were receiving ambulatory care from March-September 2019. Associations of age with overall FT and material hardship, coping resource depletion, and psychological burden FT domains were tested using Kruskal-Wallis and χ2 tests and multivariable generalized linear models with gamma distribution.ResultsYAs (median age, 31.5 years) comprised 9.6% of the sample; other working-age adults comprised 56.9%. Overall, material, coping, and psychological FT scores were worse in younger age adults versus older adults (P

Published
2022

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

Author

Cai, C., Xiong, S. L., Li, C. K., Liu, C. Z., Zhang, S. N., Li, X. B., Song, L. M., Li, B., Xiao, S., Yi, Q. B., Zhu, Y., Zheng, Y. G., Chen, W., Luo, Q., Huang, Y., Song, X. Y., Zhao, H. S., Zhao, Y., Zhang, Z., Bu, Q. C., Cao, X. L., Chang, Z., Chen, L., Chen, T. X., Chen, Y. B., Chen, Y., Chen, Y. P., Cui, W. W., Du, Y. Y., Gao, G. H., Gao, H., Ge, M. Y., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huo, J., Jia, S. M., Jiang, W. C., Jin, J., Kong, L. D., Li, G., Li, T. P., Li, W., Li, X., Li, X. F., Li, Z. W., Liang, X. H., Liao, J. Y., Liu, B. S., Liu, H. W., Liu, H. X., Liu, X. J., Lu, F. J., Lu, X. F., Luo, T., Ma, R. C., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Qu, J. L., Ren, X. Q., Sai, N., Sun, L., Tan, Y., Tao, L., Tuo, Y. L., Wang, C., Wang, L. J., Wang, P. J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. B., Wu, B. Y., Wu, M., Xiao, G. C., Xu, Y. P., Yang, R. J., Yang, S., Yang, Y. J., Yang, Y. R., Yang, X. J., Yin, Q. Q., You, Y., Zhang, F., Zhang, H. M., Zhang, J., Zhang, P., Zhang, S., Zhang, W. C., Zhang, W., Zhang, Y. F., Zhang, Y. H., Zhao, X. F., Zheng, S. J., and Zhou, D. K.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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
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15. Transforming U.S. Particle Physics Education: A Snowmass 2021 Study

Author

Bitter, O, Hansen, EV, Kravitz, S, Velan, V, and You, Y

Subjects
physics.ed-ph, physics.soc-ph
Abstract

The pursuit of knowledge in particle physics requires constant learning. Asnew tools become available, new theories are developed, and physicists searchfor new answers with ever-evolving methods. However, it is the case that formaleducational systems serve as the primary training grounds for particlephysicists. Graduate school (and undergraduate school to a lesser extent) iswhere researchers learn most of the technical skills required for research,develop scientific problem-solving abilities, learn how to establish themselvesin their field, and begin developing their career. It is unfortunate, then,that the skills gained by physicists during their formal education are oftenmismatched with the skills actually required for a successful career inphysics. We performed a survey of the U.S. particle physics community todetermine the missing elements of graduate and undergraduate education and togauge how to bridge these gaps. In this contributed paper, part of the 2021-22Snowmass Community Planning Exercise, we report the results of this survey. Wealso recommend several specific community actions to improve the quality ofparticle physics education; the "community" here refers to physics departments,national labs, professional societies, funding agencies, and individualphysicists.

Published
2022

20. Genomic Landscape of Lynch Syndrome Colorectal Neoplasia Identifies Shared Mutated Neoantigens for Immunoprevention

Author

Bolivar, Ana M., Duzagac, Fahriye, Deng, Nan, Reyes-Uribe, Laura, Chang, Kyle, Wu, Wenhui, Bowen, Charles M., Taggart, Melissa W., Thirumurthi, Selvi, Lynch, Patrick M., You, Y. Nancy, Rodriguez-Pascual, Jesus, Lipkin, Steven M., Kopetz, Scott, Scheet, Paul, Lizee, Gregory A., Reuben, Alexandre, Sinha, Krishna M., and Vilar, Eduardo

Published
2024
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21. Accretion Torque Reversals in GRO J1008-57 Revealed by Insight-HXMT

Author

Wang, W., Tang, Y. M., Tuo, Y. L., Epili, P. R., Zhang, S. N., Song, L. M., Lu, F. J., Qu, J. L., Zhang, S., Ge, M. Y., Huang, Y., Li, B., Bu, Q. C., Cai, C., Cao, X. L., Chang, Z., Chen, L., Chen, T. X., Chen, Y. B., Chen, Y., Chen, Y. P., Cui, W. W., Du, Y. Y., Gao, G. H., Gao, H., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huo, J., Jia, S. M., Jiang, W. C., Jin, J., Kong, L. D., Li, C. K., Li, G., Li, T. P., Li, W., Li, X., Li, X. B., Li, X. F., Li, Z. W., Liang, X. H., Liao, J. Y., Liu, B. S., Liu, C. Z., Liu, H. X., Liu, H. W., Lu, X. F., Luo, Q., Luo, T., Ma, R. C., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Ren, X. Q., Sai, N., Song, X. Y., Sun, L., Tao, L., Wang, C., Wang, L. J., Wang, P. J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. Y., Wu, B. B., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Xu, Y. P., Yang, R. J., Yang, S., Yang, J. J., Yang, Y. J., Yi, B. B., Yin, Q. Q., You, Y., Zhang, F., Zhang, H. M., Zhang, J., Zhang, P., Zhang, W., Zhang, W. C., Zhang, Y. F., Zhang, Y. H., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zheng, Y. G., and Zhou, D. K.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

GRO J1008-57, as a Be/X-ray transient pulsar, is considered to have the highest magnetic field in known neutron star X-ray binary systems. Observational data of the X-ray outbursts in GRO J1008-57 from 2017 to 2020 were collected by the Insight-HXMT satellite. In this work, the spin period of the neutron star in GRO J1008-57 was determined to be about 93.28 seconds in August 2017, 93.22 seconds in February 2018, 93.25 seconds in June 2019 and 93.14 seconds in June 2020. GRO J1008-57 evolved in the spin-up process with a mean rate of $-(2.10\pm 0.05)\times$10$^{-4}$ s/d from 2009 -- 2018, and turned into a spin down process with a rate of $(6.7\pm 0.6)\times$10$^{-5}$ s/d from Feb 2018 to June 2019. During the type II outburst of 2020, GRO J1008-57 had the spin-up torque again. During the torque reversals, the pulse profiles and continuum X-ray spectra did not change significantly, and the cyclotron resonant scattering feature around 80 keV was only detected during the outbursts in 2017 and 2020. Based on the observed mean spin-up rate, we estimated the inner accretion disk radius in GRO J1008-57 (about 1 - 2 times of the Alfv\'{e}n radius) by comparing different accretion torque models of magnetic neutron stars. During the spin-down process, the magnetic torque should dominate over the matter accreting inflow torque, and we constrained the surface dipole magnetic field $B\geq 6\times 10^{12}$ G for the neutron star in GRO J1008-57, which is consistent with the magnetic field strength obtained by cyclotron line centroid energy., Comment: 10 pages, 5 figures, and 3 tables, the Journal of High Energy Astrophysics in press

Published
2021

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

Author

Ding, Y. Z., Wang, W., Zhang, P., Bu, Q. C., Cai, C., Cao, X. L., Zhi, C., Chen, L., Chen, T. X., Chen, Y. B., Chen, Y., Chen, Y. P., Cui, W. W., Du, Y. Y., Gao, G. H., Gao, H., Ge, M. Y., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jia, S. M., Jiang, W. C., Jin, J., Kong, L. D., Li, B., Li, C. K., Li, G., Li, T. P., Li, W., Li, X., Li, X. B., Li, X. F., Li, Z. W., Liang, X. H., Liao, J. Y., Liu, B. S., Liu, C. Z., Liu, H. X., Liu, H. W., Liu, X. J., Lu, F. J., Lu, X. F., L., Q., T., L., Ma, R. C., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Qu, J. L., Ren, X. Q., Sai, N., Song, L. M., Song, X. Y., Sun, L., Tan, Y., Tao, L., Tuo, Y. L., Wang, L. J., Wang, P. J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. Y., Wu, B. B., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Xu, Y. P., Yang, R. J., Yang, S., Yang, Y. J., Yi, Q. B., Yin, Q. Q., You, Y., Zhang, F., Zhang, H. M., Zhang, J., Zhang, S., Zhang, S. N., Zhang, W. C., Zhang, W., Zhang, Y. F., Zhang, Y. H., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zheng, Y. G., and Zhou, D. K.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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., Comment: 14 pages, 9 figures, and 6 tables. This work has been submitted to MNRAS after the referee's report

Published
2021
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23. Insight-HXMT observations of Swift J0243.6+6124: the evolution of RMS pulse fractions at super-Eddington luminosity

Author

Wang, P. J., Kong, L. D., Zhang, S., Chen, Y. P., Zhang, S. N., Qu, J. L., Ji, L., Tao, L., Ge, M. Y., Lu, F. J., Chen, L., Song, L. M., Li, T. P., Xu, Y. P., Cao, X. L., Chen, Y., Liu, C. Z., Bu, Q. C., Cai, C., Chang, Z., Chen, G., Chen, T. X., Chen, Y. B., Cui, W., Cui, W. W., Deng, J. K., Dong, Y. W., Du, Y. Y., Fu, M. X., Gao, G. H., Gao, H., Gao, M., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jia, S. M., Jiang, L. H., Jiang, W. C., Jin, J., Jin, Y. J., Li, 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., Liang, X. H., Liao, J. Y., Liu, B. S., Liu, G. Q., Liu, H. W., Liu, X. J., Liu, Y. N., Lu, B., Lu, X. F., Luo, Q., Luo, T., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Sai, N., Shang, R. C., Song, X. Y., Sun, L., Tan, Y., Tuo, Y. L., Wang, C., Wang, G. F., Wang, J., Wang, L. J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. Y., Wu, B. B., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Yang, J. W., Yang, S., Yang, Yan Ji, Yang, Yi Jung, Yi, Q. B., Yin, Q. Q., You, Y., Zhang, 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, Zhao, Zhang, Zhi, Zhang, Z. L., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zheng, Y. G., Zhou, D. K., Zhou, J. F., Zhu, Y. X., Zhu, Y., and Zhuang, R. L.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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 source (ULX) 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 super-critical 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 $7.71\times10^{38}$~erg~s$^{-1}$, but smaller at above. A transition luminosity is found to be energy independent. Such a phenomena is firstly confirmed by Insight-HXMT observations and we speculate it may have relation with the radiation pressure dominated accretion disk.

Published
2020
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24. Physical origin of the nonphysical spin evolution of MAXI J1820+070

Author

Guan, J., Tao, L., Qu, J. L., Zhang, S. N., Zhang, W., Zhang, S., Ma, R. C., Ge, M. Y., Song, L. M., Lu, F. J., Li, T. P., Xu, Y. P., Chen, Y., Cao, X. L., Liu, C. Z., Zhang, L., Wang, Y. N., Chen, Y. P., Bu, Q. C., Cai, C., Chang, Z., Chen, L., Chen, T. X., Chen, Y. B., Cui, W. W., Du, Y. Y., Gao, G. H., Gao, H., Gu, Y. D., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jia, S. M., Jiang, W. C., Jin, J., Kong, L. D., Li, B., Li, C. K., Li, G., Li, W., Li, X., Li, X. B., Li, X. F., Li, Z. W., Liang, X. H., Liao, J. Y., Liu, B. S., Liu, H. W., Liu, H. X., Liu, X. J., Lu, X. F., Luo, Q., Luo, T., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Ren, X. Q., Sai, N., Song, X. Y., Sun, L., Tan, Y., Wang, C., Wang, L. J., Wang, P. J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. B., Wu, B. Y., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Yang, R. J., Yang, S., Yang, Y. J., Yi, Q. B., Yin, Q. Q., You, Y., Zhang, F., Zhang, H. M., Zhang, J., Zhang, P., Zhang, W. C., Zhang, Y. F., Zhang, Y. H., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zheng, Y. G., and Zhou, D. K.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, 83C57
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
2020
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25. X-ray reprocessing in accreting pulsar GX 301-2 observed with Insight-HXMT

Author

Ji, L., Doroshenko, V., Suleimanov, V., Santangelo, A., Orlandini, M., Liu, J., Ducci, L., Zhang, S. N., Nabizadeh, A., Gavran, D., Zhang, S., Ge, M. Y., Li, X. B., Tao, L., Bu, Q. C., Qu, J. L., Lu, F. J., Chen, L., Song, L. M., Li, T. P., Xu, Y. P., Cao, X. L., Chen, Y., Liu, C. Z., Cai, C., Chang, Z., Chen, T. X., Chen, Y. P., Cui, W. W., Du, Y. Y., Gao, G. H., Gao, H., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jia, S. M., Jiang, W. C., Jin, J., Kong, L. D., Li, B., Li, C. K., Li, G., Li, W., Li, X., Li, X. F., Li, Z. W., Liang, X. H., Liao, J. Y., Liu, B. S., Liu, H. X., Liu, H. W., Liu, X. J., Lu, X. F., Luo, Q., Luo, T., Ma, R. C., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Ren, X. Q., Sai, N., Song, X. Y., Sun, L., Tan, Y., Tuo, Y. L., Wang, C., Wang, L. J., Wang, P. J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. Y., Wu, B. B., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Yang, R. J., Yang, S., Yang, Yan-Ji, Yang, Yi-Jung, Yi, Q. B., Yin, Q. Q., You, Y., Zhang, F., Zhang, H. M., Zhang, J., Zhang, P., Zhang, W., Zhang, W. C., Zhang, Yi, Zhang, Y. F., Zhang, Y. H., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zheng, Y. G., and Zhou, D. K.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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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26. Insight-HXMT observations of a possible fast transition from jet to wind dominated state during a huge flare of GRS~1915+105

Author

Kong, L. D., Zhang, S., Chen, Y. P., Zhang, S. N., Ji, L., Wang, P. J., Tao, L., Ge, M. Y., Liu, C. Z., Song, L. M., Lu, F. J., Qu, J. L., Li, T. P., Xu, Y. P., Cao, X. L., Chen, Y., Bu, Q. C., Cai, C., Chang, Z., Chen, G., Chen, L., Chen, T. X., Cui, W. W., Du, Y. Y., Gao, G. H., Gao, H., Gao, M., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jia, S. M., Jiang, W. C., Jin, J., Li, B., Li, C. K., Li, G., Li, W., Li, X., Li, X. B., Li, X. F., Li, Z. W., Liang, X. H., Liao, J. Y., Liu, B. S., Liu, H. W., Liu, H. X., Liu, X. J., Lu, X. F., Luo, Q., Luo, T., Ma, R. C., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Ren, X. Q., Sai, N., Song, X. Y., Sun, L., Tan, Y., Tuo, Y. L., Wang, C., Wang, L. J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. B., Wu, B. Y., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Yang, R. J., Yang, S., Yang, Y. J., Yi, Q. B., Yin, Q. Q., You, Y., Zhang, F., Zhang, H. M., Zhang, J., Zhang, P., Zhang, W. C., Zhang, W., Zhang, Y. F., Zhang, Y. H., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zheng, Y. G., and Zhou, D. K.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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
2020
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27. Survival of Patients with Hepatitis B-Related Hepatocellular Carcinoma with Concomitant Metabolic Associated Fatty Liver Disease

Author

You Y, Yang T, Wei S, Liu Z, Liu C, Shen Z, Yang Y, Feng Y, Yao P, and Zhu Q

Subjects
steatosis, diabetes, obesity, hbe ag, Specialties of internal medicine, RC581-951
Abstract

Yajing You,1,&ast; Tao Yang,2,&ast; Shuhang Wei,1 Zongxin Liu,1 Chenxi Liu,1 Zijian Shen,3 Yinuo Yang,1 Yuemin Feng,1 Ping Yao,2 Qiang Zhu1,2 1Department of Gastroenterology, Shandong Provincial Hospital, Shandong University, Jinan, Shandong, 250021, People’s Republic of China; 2Department of Gastroenterology, The First Affiliated Hospital of Xinjiang Medical University, Urumqi, Xinjiang Uygur Autonomous Region, 830000, People’s Republic of China; 3Department of Radiology, Shandong Provincial Hospital, Affiliated to Shandong First Medical University, Jinan, Shandong, 250021, People’s Republic of China&ast;These authors contributed equally to this workCorrespondence: Qiang Zhu, Department of Gastroenterology, The First Affiliated Hospital of Xinjiang Medical University, Urumqi, Xinjiang Uygur Autonomous Region, 830000, People’s Republic of China, Email zhuqiang@sdu.edu.cn Ping Yao, Department of Gastroenterology, The First Affiliated Hospital of Xinjiang Medical University, Urumqi, Xinjiang Uygur Autonomous Region, 830000, People’s Republic of China, Email pingyaozh@sina.comPurpose: Metabolic associated fatty liver disease is a novel concept defined as fatty liver associated with metabolic disorders. We investigated the effect of metabolic associated fatty liver disease on hepatocellular carcinoma patient mortality.Patients and Methods: A total of 624 patients with hepatocellular carcinoma between 2012 and 2020 were enrolled in this retrospective study. Hepatic steatosis was diagnosed using computed tomography or magnetic resonance imaging. Metabolic associated fatty liver disease was defined based on the proposed criteria in 2020. Propensity score matching was performed for patients with metabolic associated fatty liver disease and those without the condition. A Cox proportional hazards regression model was used to evaluate the association between metabolic associated fatty liver disease and hepatocellular carcinoma patient outcomes.Results: Patients with hepatocellular carcinoma and metabolic associated fatty liver disease tended to achieve better outcomes than did those without metabolic associated fatty liver disease after matching (p< 0.001). Metabolic associated fatty liver disease was significantly associated with better prognosis in patients with concurrent hepatitis B infection (p< 0.001). Moreover, high levels of hepatitis B viral DNA in serum samples was associated with a significantly increased risk of death in patients without non-metabolic associated fatty liver disease (p=0.045). Additionally, the association between metabolic associated fatty liver disease and survival in hepatitis B virus-related hepatocellular carcinoma was similar in all subgroups based on metabolic traits.Conclusion: Metabolic associated fatty liver disease increases the survival rate of patients with hepatocellular carcinoma and hepatitis B virus infection. The potential interaction of steatosis and virus replication should be considered for future research and clinical treatment strategies.Keywords: steatosis, diabetes, obesity, HBe Ag

Published
2023

28. The Ratio of Fibrinogen to Albumin is Related to the Occurrence of Retinopathy in Type 2 Diabetic Patients

Author

Chen X, Zhao J, You Y, Li Z, and Chen S

Subjects
fibrinogen to albumin ratio, type 2 diabetes mellitus, diabetic retinopathy, inflammation, influencing factors, Specialties of internal medicine, RC581-951
Abstract

Xiaoyi Chen,1,2 Jingyu Zhao,3 Yanxue You,1,2 Zelin Li,2 Shuchun Chen2 1Graduate School, Hebei North University, Zhangjiakou, 075000, People’s Republic of China; 2Department of Endocrinology, Hebei General Hospital, Shijiazhuang, 050051, People’s Republic of China; 3Graduate School, North China University of Science and Technology, Tangshan, 063210, People’s Republic of ChinaCorrespondence: Shuchun Chen, Department of Endocrinology, Hebei General Hospital, 348, Heping West Road, Shijiazhuang, Hebei, 050051, People’s Republic of China, Email chenshuchunwork88@163.comPurpose: Type 2 diabetic retinopathy is a long-term chronic inflammatory disease. The aim of this study was to investigate the relationship between fibrinogen to albumin ratio (FAR) and retinopathy in type 2 diabetic patients.Methods: This was a retrospective study that included 500 patients with type 2 diabetes mellitus (T2DM), and were divided into non-diabetic retinopathy group (NDR, n=297) and diabetic retinopathy group (DR, n=203) according to fundus examination findings, and the DR group was further divided into non-proliferative retinopathy group (NPDR, n=182) and proliferative retinopathy group (PDR, n=21). Baseline data of patients were collected, and the fibrinogen to albumin ratio (FAR) and neutrophil to lymphocyte ratio (NLR) were calculated to analyze the correlation between FAR and NLR and type 2 diabetic retinopathy.Results: The FAR and NLR were significantly higher in the DR group compared with the NDR group (both P < 0.001). Spearman correlation analysis showed that FAR was positively correlated with NLR and DR (P < 0.05). As the FAR quartile increased, the prevalence of DR increased (14.8%, 16.7%, 25.1%, and 43.30%, respectively; P < 0.05). Multifactorial logistic regression analysis showed that FAR, diabetic course, systolic blood pressure (SBP) and diabetic peripheral neuropathy (DPN) were risk factors for the development of DR in patients with T2DM. The area under the ROC curve for FAR to predict DR progression was 0.708, with an optimal critical value of 7.04, and the area under the ROC curve for diabetes duration and SBP to predict DR was 0.705 and 0.588, respectively.Conclusion: Our findings show for the first time that FAR is an independent risk factor for assessing DR in patients with type 2 diabetes.Keywords: fibrinogen to albumin ratio, type 2 diabetes mellitus, diabetic retinopathy, inflammation, influencing factors

Published
2023

29. A variable ionized disk wind in the black-hole candidate EXO 1846-031

Author

Wang, Yanan, Ji, Long, Garcia, Javier A., Dauser, Thomas, Mendez, Mariano, Mao, Junjie, Tao, L., Altamirano, Diego, Maggi, Pierre, Zhang, S. N., Ge, M. Y., Zhang, L., Qu, J. L., Zhang, S., Ma, X., Lu, F. J., Li, T. P., Huang, Y., Zheng, S. J., Chang, Z., Tuo, Y. L., Song, L. M., Xu, Y. P., Chen, Y., Liu, C. Z., Bu, Q. C., Cai, C., Cao, X. L., Chen, L., Chen, T. X., Chen, Y. P., Cui, W. W., Du, Y. Y., Gao, G. H., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huo, J., Jia, S. M., Jiang, W. C., Jin, J., Kong, L. D., Li, B., Li, C. K., Li, G., Li, W., Li, X., Li, X. B., Li, X. F., Li, Z. W., Liang, X. H., Liao, J. Y., Liu, H. W., Liu, X. J., Lu, X. F., Luo, Q., Luo, T., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Sai, N., Shang, R. C., Song, X. Y., Sun, L., Tan, Y., Wang, W. S., Wang, Y. D., Wang, Y. S., Wen, X. Y., Wu, B. B., Wu, B. Y., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Yang, S., Yang, Y. J., Yi, Q. B., Yin, Q. Q., You, Y., Zhang, F., Zhang, H. M., Zhang, J., Zhang, W. C., Zhang, W., Zhang, Y. F., Zhao, H. S., Zhao, X. F., and Zhou, D. K.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

After 34 years, the black-hole candidate EXO 1846-031 went into outburst again in 2019. We investigate its spectral properties in the hard intermediate and the soft states with NuSTAR and Insight-HXMT. A reflection component has been detected in the two spectral states but possibly originating from different illumination spectra: in the intermediate state, the illuminating source is attributed to a hard coronal component, which has been commonly observed in other X-ray binaries, whereas in the soft state the reflection is probably produced by the disk self-irradiation. Both cases support EXO 1846-031 as a low inclination system of ~40 degrees. An absorption line is clearly detected at ~7.2 keV in the hard intermediate state, corresponding to a highly ionized disk wind (log {\xi} > 6.1) with a velocity up to 0.06c. Meanwhile, quasi-simultaneous radio emissions have been detected before and after the X-rays, implying the co-existence of disk winds and jets in this system. Additionally, the observed wind in this source is potentially driven by magnetic forces. The absorption line disappeared in the soft state and a narrow emission line appeared at ~6.7 keV on top of the reflection component, which may be evidence for disk winds, but data with the higher spectral resolution are required to examine this., Comment: Accepted for publication in ApJ

Published
2020
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30. Constraining the transient high-energy activity of FRB180916.J0158+65 with Insight-HXMT followup observations

Author

Guidorzi, C., Orlandini, M., Frontera, F., Nicastro, L., Xiong, S. L., Liao, J. Y., Li, G., Zhang, S. N., Amati, L., Virgilli, E., Zhang, S., Bu, Q. C., Cai, C., Cao, X. L., Chang, Z., Chen, L., Chen, T. X., Chen, Y., Chen, Y. P., Cui, W. W., Du, Y. Y., Gao, G. H., Gao, H., Gao, M., Ge, M. Y., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jia, S. M., Jiang, W. C., Jin, J., Kong, L. D., Li, B., Li, C. K., Li, T. P., Li, W., Li, X., Li, X. B., Li, X. F., Li, Z. W., Liang, X. H., Liu, B. S., Liu, C. Z., Liu, H. X., Liu, H. W., Liu, X. J., Lu, F. J., Lu, X. F., Luo, Q., Luo, T., Ma, R. C., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Qu, J. L, Ren, X. Q., Sai, N., Song, L. M., Song, X. Y., Sun, L., Tan, Y., Tao, L., Tuo, Y. L., Wang, C., Wang, L. J., Wang, P. J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. Y., Wu, B. B., Wu, M., Xiao, G. C., Xiao, S., Xu, Y. P., Yang, R., Yang, S., Yang, Y. J., Yi, Q. B., Yin, Q. Q., You, Y., Zhang, F., Zhang, H. M., Zhang, J., Zhang, P., Zhang, W. C., Zhang, W., Zhang, Y. F., Zhang, Y. H., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zheng, Y. G., and Zhou, D. K.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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<10^46 erg for durations <0.1 s over several tens of ks exposure. We can rule out the occurrence of giant flares similar to the ones that were observed in the few cases of Galactic magnetars. The absence of reported radio activity during our observations does not allow us to make any statements on the possible simultaneous high-energy emission., Comment: 10 pages, 3 figures, accepted by A&A

Published
2020
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31. Insight-HXMT firm detection of the highest energy fundamental cyclotron resonance scattering feature in the spectrum of GRO J1008-57

Author

Ge, M. Y., Ji, L., Zhang, S. N., Santangelo, A., Liu, C. Z., Doroshenko, V., Staubert, R., Qu, J. L., Zhang, S., Lu, F. J., Song, L. M., Li, T. P., Tao, L., Xu, Y. P., Cao, X. L., Chen, Y., Bu, Q. C., Cai, C., Chang, Z., Chen, G., Chen, L., Chen, T. X., Chen, Y. B., Chen, Y. P., Cui, W., Cui, W. W., Deng, J. K., Dong, Y. W., Du, Y. Y., Fu, M. X., Gao, G. H., Gao, H., Gao, M., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jia, S. M., Jiang, L. H., Jiang, W. C., Jin, J., Jin, Y. J., Kong, L. D., Li, 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., Liang, X. H., Liao, J. Y., Liu, B. S., Liu, G. Q., Liu, H. W., Liu, X. J., Liu, Y. N., Lu, B., Lu, X. F., Luo, Q., Luo, T., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Sai, N., Shang, R. C., Song, X. Y., Sun, L., Tan, Y., Tuo, Y. L., Wang, C., Wang, G. F., Wang, J., Wang, L. J., Wang, W. S., Wang, Y. D., Wang, Y. S., Wen, X. Y., Wu, B. B., Wu, B. Y., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Xu, H., Yang, J. W., Yang, S., Yang, Y. J., Yi, Q. B., Yin, Q. Q., You, Y., Zhang, 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., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zheng, Y. G., Zhou, D. K., Zhou, J. F., Zhuang, R. L., Zhu, Y. X., and Zhu, Y.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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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32. HXMT Identification of a non-thermal X-ray burst from SGR J1935+2154 and with FRB 200428

Author

Li, C. K., Lin, L., Xiong, S. L., Ge, M. Y., Li, X. B., Li, T. P., Lu, F. J., Zhang, S. N., Tuo, Y. L., Nang, Y., Zhang, B., Xiao, S., Chen, Y., Song, L. M., Xu, Y. P., Liu, C. Z., Jia, S. M., Cao, X. L., Qu, J. L., Zhang, S., Gu, Y. D., Liao, J. Y., Zhao, X. F., Tan, Y., Nie, J. Y., Zhao, H. S., Zheng, S. J., Zheng, Y. G., Luo, Q., Cai, C., Li, B., Xue, W. C., Bu, Q. C., Chang, Z., Chen, G., Chen, T. X., Chen, Y. B., Chen, Y. P., Cui, W., Cui, W. W., Deng, J. K., Dong, Y. W., Du, Y. Y., Fu, M. X., Gao, G. H., Gao, H., Gao, M., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jiang, L. H., Jiang, W. C., Jin, J., Jin, Y. J., Kong, L. D., Li, G., Li, M. S., Li, W., Li, X., Li, X. F., Li, Y. G., Li, Z. W., Liang, X. H., Liu, B. S., Liu, G. Q., Liu, H. W., Liu, X. J., Liu, Y. N., Lu, B., Lu, X. F., Luo, T., Ma, X., Meng, B., Ou, G., Sai, N., Shang, R. C., Song, X. Y., Sun, L., Tao, L., Wang, C., Wang, G. F., Wang, J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. B., Wu, B. Y., Wu, M., Xiao, G. C., Xu, H., Yang, J. W., Yang, S., Yang, Y. J., Yang, Yi-Jung, Yi, Q. B., Yin, Q. Q., You, Y., Zhang, A. M., Zhang, C. M., Zhang, F., Zhang, H. M., Zhang, J., Zhang, T., Zhang, W., Zhang, W. C., Zhang, W. Z., Zhang, Y., Zhang, Yue, Zhang, Y. F., Zhang, Y. J., Zhang, Z., Zhang, Zhi, Zhang, Z. L., Zhou, D. K., Zhou, J. F., Zhu, Y., Zhu, Y. X., and Zhuang, R. L.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
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., Comment: 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
2020
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33. Insight-HXMT insight into switch of the accretion mode: the case of the X-ray pulsar 4U 1901+03

Author

Tuo, Y. L., Ji, L., Tsygankov, S. S., Mihara, T., Song, L. M., Ge, M. Y., Nabizadeh, A., Tao, L., Qu, J. L., Zhang, Y., Zhang, S., Zhang, S. N., Bu, Q. C., Chen, L., Xu, Y. P., Cao, X. L., Chen, Y., Liu, C. Z., Cai, C., Chang, Z., Chen, G., Chen, T. X., Chen, Y. B., Chen, Y. P., Cui, W., Cui, W. W., Deng, J. K., Dong, Y. W., Du, Y. Y., Fu, M. X., Gao, G. H., Gao, H., Gao, M., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jia, S. M., Jiang, L. H., Jiang, W. C., Jin, J., Jin, Y. J., Kong, L. D., Li, 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. W., Liang, X. H., Liao, J. Y., Liu, B. S., Liu, G. Q., Liu, H. W., Liu, X. J., Liu, Y. N., Lu, B., Lu, F. J., Lu, X. F., Luo, Q., Luo, T., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Sai, N., Shang, R. C., Song, X. Y., Sun, L., Tan, Y., Wang, C., Wang, G. F., Wang, J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. Y., Wu, B. B., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Yang, J. W., Yang, S., Yang, Y. J., Yi, Q. B., Yin, Q. Q., You, Y., Zhang, A. M., Zhang, C. M., Zhang, F., Zhang, H. M., Zhang, J., Zhang, T., Zhang, W., Zhang, W. C., Zhang, W. Z., Zhang, Y. F., Zhang, Y. J., Zhang, Y. H., Zhang, Z., Zhang, Z. L., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zheng, Y. G., Zhou, D. K., Zhou, J. F., Zhu, Y. X., Zhu, Y., and Zhuang, R. L.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We use the In data collected during the 2019 outburst from X-ray pulsar 4U 1901+03 to complement the orbital parameters reported by Fermi/GBM. Using the Insight-HXMT, we examine the correlation between the derivative of the intrinsic spin frequency and bolometric flux based on accretion torque models. It was found that the pulse profiles significantly evolve during the outburst. The existence of two types of the profile's pattern discovered in the Insight-HXMT data indicates that this source experienced transition between a super-critical and a sub-critical accretion regime during its 2019 outburst. Based on the evolution of the pulse profiles and the torque model, we derive the distance to 4U 1901+03 as 12.4+-0.2 kpc., Comment: 8 pages, 5 figures, accepted by JHEAP

Published
2020

34. The evolution of the broadband temporal features observed in the black-hole transient MAXI J1820+070 with Insight-HXMT

Author

Wang, Yanan, Ji, Long, Zhang, S. N., Méndez, Mariano, Qu, J. L., Maggi, Pierre, Ge, M. Y., Qiao, Erlin, Tao, L., Zhang, S., Altamirano, Diego, Zhang, L., Ma, X., Lu, F. J., Li, T. P., Huang, Y., Zheng, S. J., Chen, Y. P., Chang, Z., Tuo, Y. L., Gungor, C., Song, L. M., Xu, Y. P., Cao, X. L., Chen, Y., Liu, C. Z., Bu, Q. C., Cai, C., Chen, G., Chen, L., Chen, T. X., Chen, Y. B., Cui, W., Cui, W. W., Deng, J. K., Dong, Y. W., Du, Y. Y., Fu, M. X., Gao, G. H., Gao, H., Gao, M., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huo, J., Jia, S. M., Jiang, L. H., Jiang, W. C., Jin, J., Jin, Y. J., Kong, L. D., Li, 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., Liang, X. H., Liao, J. Y., Liu, G. Q., Liu, H. W., Liu, X. J., Liu, Y. N., Lu, B., Lu, X. F., Luo, Q., Luo, T., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Sai, N., Shang, R. C., Song, X. Y., Sun, L., Tan, Y., Wang, G. F., Wang, J., Wang, W. S., Wang, Y. D., Wang, Y. S., Wen, X. Y., Wu, B. B., Wu, B. Y., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Yang, J. W., Yang, S., Yang, Y. J., Yi, Q. B., Yin, Q. Q., You, Y., Zhang, 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., Zhao, H. S., Zhao, X. F., Zhou, D. K., Zhou, J. F., Zhuang, R. L., Zhu, Y. X., and Zhu, Y.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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
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35. Discovery of delayed spin-up behavior following two large glitches in the Crab pulsar, and the statistics of such processes

Author

Ge, M. Y., Zhang, S. N., Lu, F. J., Li, T. P., Yuan, J. P., Zheng, X. P., Huang, Y., Zheng, S. J., Chen, Y. P., Chang, Z., Tuo, Y. L., Cheng, Q., Güngör, C., Song, L. M., Xu, Y. P., Cao, X. L., Chen, Y., Liu, C. Z., Zhang, S., Qu, J. L., Bu, Q. C., Cai, C., Chen, G., Chen, L., Chen, M. Z., Chen, T. X., Chen, Y. B., Cui, W., Cui, W. W., Deng, J. K., Dong, Y. W., Du, Y. Y., Fu, M. X., Gao, G. H., Gao, H., Gao, M., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Hao, L. F., Huo, J., Jia, S. M., Jiang, L. H., Jiang, W. C., Jin, C. J., Jin, J., Jin, Y. J., Kong, L. D., Li, 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., Liu, Z. Y., Liang, X. H., Liao, J. Y., Liu, G. Q., Liu, H. W., Liu, X. J., Liu, Y. N., Lu, B., Lu, X. F., Luo, Q., Luo, T., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Sai, N., Shang, R. C., Song, X. Y., Sun, L., Tan, Y., Tao, L., Wang, C., Wang, G. F., Wang, J., Wang, J. B., Wang, M., Wang, N., Wang, W. S., Wang, Y. D., Wang, Y. S., Wen, X. Y., Wen, Z. G., Wu, B. B., Wu, B. Y., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Xu, Y. H., Yan, W. M., Yang, J. W., Yang, S., Yang, Y. J., Yi, Q. B., Yin, Q. Q., You, Y., Yue, Y. L., Zhang, 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., Zhao, H. S., Zhao, X. F., Zheng, W., Zhou, D. K., Zhou, J. F., Zhou, X., Zhuang, R. L., Zhu, Y. X., and Zhu, Y.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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 $<0.48$ hour. We also carried out a statistical study of these five glitches with observed spin-up processes. The two glitches occurred in 2004 and 2011 have delayed spin-up time scales ($\tau_{1}$) of $1.7\pm0.8$\,days and $1.6\pm0.4$\,days, respectively. We find that the $\Delta{\nu}$ vs. $|\Delta{\dot\nu}|$ relation of these five glitches is similar to those with no detected delayed spin-up process, indicating that they are similar to the others in nature except that they have larger amplitudes. For these five glitches, the amplitudes of the delayed spin-up process ($|\Delta{\nu}_{\rm d1}|$) and recovery process ($\Delta{\nu}_{\rm d2}$), their time scales ($\tau_{1}$, $\tau_{2}$), and permanent changes in spin frequency ($\Delta{\nu}_{\rm p}$) and total frequency step ($\Delta{\nu}_{\rm g}$) have positive correlations. From these correlations, we suggest that the delayed spin-up processes are common for all glitches, but are too short and thus difficult to be detected for most glitches., Comment: 25 pages, 8 figures

Published
2020
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36. A search for prompt gamma-ray counterparts to fast radio bursts in the Insight-HXMT data

Author

Guidorzi, C., Marongiu, M., Martone, R., Nicastro, L., Xiong, S. L., Liao, J. Y., Li, G., Zhang, S. N., Amati, L., Frontera, F., Orlandini, M., Rosati, P., Virgilli, E., Zhang, S., Bu, Q. C., Cai, C., Cao, X. L., Chang, Z., Chen, G., Chen, L., Chen, T. X., Chen, Y. B., Chen, Y. P., Cui, W., Cui, W. W., Deng, J. K., Dong, Y. W., Du, Y. Y., Fu, M. X., Gao, G. H., Gao, H., Gao, M., Ge, M. Y., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jia, S. M., Jiang, L. H., Jiang, W. C., Jin, J., Jin, Y. J., Kong, L. D., Li, B., Li, C. K., Li, M. S., Li, T. P., Li, W., Li, X., Li, X. B., Li, X. F., Li, Y. G., Li, Z. W., Liang, X. H., Liu, B. S., Liu, C. Z., Liu, G. Q., Liu, H. W., Liu, X. J., Liu, Y. N., Lu, B., Lu, F. J., Lu, X. F., Luo, Q., Luo, T., Ma, R. C., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Oui, G., Qu, J. L, Sai, N., Shang, R. C., Song, L. M., Song, X. Y., Sun, L., Tani, Y., Tao, L., Tuo, Y. L., Wang, C., Wang, G. F., Wang, J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. Y., Wu, B. B., Wu, M., Xiao, G. C., Xiao, S., Xu, Y. P., Yang, J. W., Yang, S., Yang, Y. J., Yi, Q. B., Yin, Q. Q., You, Y., Zhang, 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., Zhang, X. F., Zheng, S. J., Zhou, D. K., Zhou, J. F., Zhu, Y. X., Zhu, Y., and Zhuang, R. L.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

No robust detection of prompt electromagnetic counterparts to fast radio bursts (FRBs) has yet been obtained, in spite of several multi-wavelength searches carried out so far. Specifically, X/gamma-ray counterparts are predicted by some models. We planned on searching for prompt gamma-ray counterparts in the Insight-Hard X-ray Modulation Telescope (Insight-HXMT) data, taking advantage of the unique combination of large effective area in the keV-MeV energy range and of sub-ms time resolution. We selected 39 FRBs that were promptly visible from the High-Energy (HE) instrument aboard Insight-HXMT. After calculating the expected arrival times at the location of the spacecraft, we searched for a significant excess in both individual and cumulative time profiles over a wide range of time resolutions, from several seconds down to sub-ms scales. Using the dispersion measures in excess of the Galactic terms, we estimated the upper limits on the redshifts. No convincing signal was found and for each FRB we constrained the gamma-ray isotropic-equivalent luminosity and the released energy as a function of emission timescale. For the nearest FRB source, the periodic repeater FRB180916.J0158+65, we find $L_{\gamma,iso}<5.5\times 10^{47}$ erg/s over 1 s, whereas $L_{\gamma,iso}<10^{49}-10^{51}$ erg/s for the bulk of FRBs. The same values scale up by a factor of ~100 for a ms-long emission. Even on a timescale comparable with that of the radio pulse itself no keV-MeV emission is observed. A systematic association with either long or short GRBs is ruled out with high confidence, except for subluminous events, as is the case for core-collapse of massive stars (long) or binary neutron star mergers (short) viewed off axis. Only giant flares from extra-galactic magnetars at least ten times more energetic than Galactic siblings are ruled out for the nearest FRB., Comment: 15 pages, 3 figures, 6 tables, accepted by A&A

Published
2020
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37. Switches between accretion structures during flares in 4U 1901+03

Author

Ji, L., Ducci, L., Santangelo, A., Zhang, S., Suleimanov, V., Tsygankov, S., Doroshenko, V., Nabizadeh, A., Zhang, S. N., Ge, M. Y., Tao, L., Bu, Q. C., Qu, J. L., Lu, F. J., Chen, L., Song, L. M., Li, T. P., Xu, Y. P., Cao, X. L., Chen, Y., Liu, C. Z., Cai, C., Chang, Z., Chen, G., Chen, T. X., Chen, Y. B., Chen, Y. P., Cui, W., Cui, W. W., Deng, J. K., Dong, Y. W., Du, Y. Y., Fu, M. X., Gao, G. H., Gao, H., Gao, M., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jia, S. M., Jiang, L. H., Jiang, W. C., Jin, J., Kong, L. D., Li, 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., Liang, X. H., Liao, J. Y., Liu, G. Q., Liu, H. X., Liu, H. W., Liu, X. J., Liu, Y. N., Lu, B., Lu, X. F., Luo, Q., Luo, T., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Ren, X. Q., Sai, N., Song, X. Y., Sun, L., Tan, Y., Tuo, Y. L., Wang, C., Wang, G. F., Wang, J., Wang, P. J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. Y., Wu, B. B., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Yang, J. W., Yang, S., Yang, Yan-Ji, Yang, Yi-Jung, Yi, Q. B., Yin, Q. Q., You, Y., Zhang, A. M., Zhang, C. M., Zhang, F., Zhang, H. M., Zhang, J., Zhang, P., Zhang, T., Zhang, W., Zhang, W. C., Zhang, W. Z., Zhang, Yi, Zhang, Y. F., Zhang, Y. J., Zhang, Y. H., Zhang, Yue, Zhang, Z., Zhang, Z. L., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zhou, D. K., Zhou, J. F., Zhu, Y. X., and Zhu, Y.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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., Comment: 11 pages, 8 figures, accepted for publication in MNRAS

Published
2020
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38. Joint Analysis of Energy and RMS Spectra from MAXI J1535-571 with Insight-HXMT

Author

Kong, L. D., Zhang, S., Chen, Y. P., Ji, L., Zhang, S. N., Yang, Y. R., Tao, L., Ma, X., Qu, J. L., Lu, F. J., Bu, Q. C., Chen, L., Song, L. M., Li, T. P., Xu, Y. P., Cao, X. L., Chen, Y., Liu, C. Z., Cai, C., Chang, Z., Chen, G., Chen, T. X., Chen, Y. B., Cui, W., Cui, W. W., Deng, J. K., Dong, Y. W., Du, Y. Y., Fu, M. X., Gao, G. H., Gao, H., Gao, M., Ge, M. Y., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jia, S. M., Jiang, L. H., Jiang, W. C., Jin, J., Li, 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., Liang, X. H., Liao, J. Y., Liu, G. Q., Liu, H. X., Liu, H. W., Liu, S. Z., Liu, X. J., Liu, Y. N., Lu, B., Lu, X. F., Luo, Q., Luo, T., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Ren, X. Q., Sai, N., Song, X. Y., Sun, L., Tan, Y., Tuo, Y. L., Wang, C., Wang, G. F., Wang, J., Wang, P. J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. Y., Wu, B. B., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Xu, H., Yang, J. W., Yang, S., Yang, Y. J., Yi, Q. B., You, Y., Zhang, A. M., Zhang, C. M., Zhang, F., Zhang, H. M., Zhang, J., Zhang, P., Zhang, T., Zhang, W., Zhang, W. C., Zhang, W. Z., Zhang, Y., Zhang, Y. F., Zhang, Y. J., Zhang, Y. H., Zhang, Z., Zhang, Z. L., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zheng, Y. G., Zhou, D. K., Zhou, J. F., Zhu, Y. X., and Zhu, Y.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

A new black hole X-ray binary (BHXRB) MAXI J1535-571 was discovered by MAXI during its outburst in 2017. Using observations taken by the first Chinese X-ray satellite, the Hard X-ray Modulation Telescope (dubbed as Insight-HXMT), we perform a joint spectral analysis (2-150 keV) in both energy and time domains. The energy spectra provide the essential input for probing the intrinsic Quasi-Periodic Oscillation (QPO) fractional rms spectra (FRS). Our results show that during the intermediate state, the energy spectra are in general consistent with those reported by Swift/XRT and NuSTAR. However, the QPO FRS become harder and the FRS residuals may suggest the presence of either an additional power-law component in the energy spectrum or a turn-over in the intrinsic QPO FRS at high energies.

Published
2020

39. Diagnostic of the spectral properties of Aquila X-1 by Insight-HXMT snapshots during the early propeller phase

Author

Güngör, C., Ge, M. Y., Zhang, S., Santangelo, A., Zhang, S. N., Lu, F. J., Zhang, Y., Chen, Y. P., Tao, L., Yang, Y. J., Bu, Q. C., Cai, C., Cao, X. L., Chang, Z., Chen, G., Chen, L., Chen, T. X., Chen, Y., Chen, Y. B., Cui, W., Cui, W. W., Deng, J. K., Dong, Y. W., Du, Y. Y., Fu, M. X., Gao, G. H., Gao, H., Gao, M., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Ji, L., Jia, S. M., Jiang, L. H., Jiang, W. C., Jin, J., Kong, L. D., Li, 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. W., Liang, X. H., Liao, J. Y., Liu, C. Z., Liu, G. Q., Liu, H. W., Liu, X. J., Liu, Y. N., Lu, B., Lu, X. F., Luo, T., Luo, Q., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Sai, N., Song, L. M., Song, X. Y., Sun, L., Tan, Y., Tuo, Y. L., Wang, C., Wang, G. F., Wang, J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. B., Wu, B. Y., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Xu, Y. P., Yang, J. W., Yang, S., Yi, Q. B., Yin, Q. Q., You, Y., Zhang, A. M., Zhang, C. M., Zhang, F., Zhang, H. M., Zhang, J., Zhang, T., Zhang, W., Zhang, W. C., Zhang, W. Z., Zhang, Y. F., Zhang, Y. J., Zhang, Z., Zhang, Z. L., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zhou, D. K., Zhou, J. F., Zhu, Y., and Zhu, Y. X.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
Abstract

We study the 2018 outburst of Aql X-1 via the monitor of all sky X-ray image (MAXI) data. We show that the outburst starting in February 2018 is a member of short-low class in the frame of outburst duration and the peak count rate although the outburst morphology is slightly different from the other fast-rise-exponential-decay (FRED) type outbursts with a milder rising stage. We study the partial accretion in the weak propeller stage of Aql X-1 via the MAXI data of the 2018 outburst. We report on the spectral analysis of 3 observations of Aquila X-1 obtained by Insight - hard X-ray modulation telescope (Insight-HXMT) during the late decay stage of the 2018 outburst. We discuss that the data taken by Insight-HXMT is just after the transition to the weak propeller stage. Our analysis shows the necessity of a comptonization component to take into account the existence of an electron cloud resulting photons partly up-scattered., Comment: 8 pages, 4 figures, accepted for publication in JHEAp

Published
2019

40. Naproxen chemoprevention promotes immune activation in Lynch syndrome colorectal mucosa

Author

Reyes-Uribe, Laura, Wu, Wenhui, Gelincik, Ozkan, Bommi, Prashant V, Francisco-Cruz, Alejandro, Solis, Luisa M, Lynch, Patrick M, Lim, Ramona, Stoffel, Elena M, Kanth, Priyanka, Samadder, N Jewel, Mork, Maureen E, Taggart, Melissa W, Milne, Ginger L, Marnett, Lawrence J, Vornik, Lana, Liu, Diane D, Revuelta, Maria, Chang, Kyle, You, Y Nancy, Kopelovich, Levy, Wistuba, Ignacio I, Lee, J Jack, Sei, Shizuko, Shoemaker, Robert H, Szabo, Eva, Richmond, Ellen, Umar, Asad, Perloff, Marjorie, Brown, Powel H, Lipkin, Steven M, and Vilar, Eduardo

Subjects
Biomedical and Clinical Sciences, Oncology and Carcinogenesis, Immunology, Biotechnology, Digestive Diseases, Colo-Rectal Cancer, Cancer, Prevention, Clinical Trials and Supportive Activities, Clinical Research, Genetics, Adult, Aged, Animals, Anti-Inflammatory Agents, Non-Steroidal, Chemoprevention, Colorectal Neoplasms, Hereditary Nonpolyposis, Dinoprostone, Disease Models, Animal, Female, Humans, Intestinal Mucosa, Male, Mice, Middle Aged, Naproxen, HNPCC syndrome, cancer syndromes, chemoprevention, gene expression, non-steroidal anti-inflammatory drugs, Clinical Sciences, Paediatrics and Reproductive Medicine, Gastroenterology & Hepatology, Clinical sciences, Nutrition and dietetics
Abstract

ObjectivePatients with Lynch syndrome (LS) are at markedly increased risk for colorectal cancer. It is being increasingly recognised that the immune system plays an essential role in LS tumour development, thus making an ideal target for cancer prevention. Our objective was to evaluate the safety, assess the activity and discover novel molecular pathways involved in the activity of naproxen as primary and secondary chemoprevention in patients with LS.DesignWe conducted a Phase Ib, placebo-controlled, randomised clinical trial of two dose levels of naproxen sodium (440 and 220 mg) administered daily for 6 months to 80 participants with LS, and a co-clinical trial using a genetically engineered mouse model of LS and patient-derived organoids (PDOs).ResultsOverall, the total number of adverse events was not different across treatment arms with excellent tolerance of the intervention. The level of prostaglandin E2 in the colorectal mucosa was significantly decreased after treatment with naproxen when compared with placebo. Naproxen activated different resident immune cell types without any increase in lymphoid cellularity, and changed the expression patterns of the intestinal crypt towards epithelial differentiation and stem cell regulation. Naproxen demonstrated robust chemopreventive activity in a mouse co-clinical trial and gene expression profiles induced by naproxen in humans showed perfect discrimination of mice specimens with LS and PDOs treated with naproxen and control.ConclusionsNaproxen is a promising strategy for immune interception in LS. We have discovered naproxen-induced gene expression profiles for their potential use as predictive biomarkers of drug activity.Trial registration numbergov Identifier: NCT02052908.

Published
2021

41. Significance of Immunogenic Cell Death-Related Prognostic Gene Signature in Cervical Cancer Prognosis and Anti-Tumor Immunity

Author

Jiang S, Cui Z, Zheng J, Wu Q, Yu H, You Y, Zheng C, and Sun Y

Subjects
icd, cervical cancer, immunity, prognosis, immunotherapy response, Pathology, RB1-214, Therapeutics. Pharmacology, RM1-950
Abstract

Shan Jiang,1,2 Zhaolei Cui,3 Jianfeng Zheng,1 Qiaoling Wu,1 Haijuan Yu,1 Yiqing You,3 Chaoqiang Zheng,3 Yang Sun1 1Department of Gynecology, Clinical Oncology School of Fujian Medical University, Fujian Cancer Hospital, Fuzhou, 350014, People’s Republic of China; 2College of Integrative Medicine, Fujian University of Traditional Chinese Medicine, Fuzhou, 350122, People’s Republic of China; 3Laboratory of Biochemistry and Molecular Biology Research, Department of Clinical Laboratory, Clinical Oncology School of Fujian Medical University, Fujian Cancer Hospital, Fuzhou, 350014, People’s Republic of ChinaCorrespondence: Yang Sun, Department of Gynecology, Clinical Oncology School of Fujian Medical University, Fujian Cancer Hospital, No. 420 Fuma Road, Fuzhou, Fujian, 350014, People’s Republic of China, Email sunyang@fjzlhospital.comBackground: Immunogenic cell death (ICD) can reshape the immune microenvironment of tumors. Driven by stressful pressure, by directly destroying tumor cells and activating the body’s adaptive immunity, ICD acts as a modulator of cell death, enabling the body to generate an anti-tumor immune response that produces a more effective therapeutic effect, while tumor cells are driven to kill. Hence, this research aimed to find and evaluate ICD-related genetic signatures as cervical cancer (CC) prognostic factors.Methods: Data of CC patients from the Tumor Genome Atlas (TCGA) were used as the basis to obtain immunogenic cell-death-related prognostic genes (IPGs) in patients with CC, using the least absolute shrinkage and selection operator and Cox regression screening, and the IPGs scoring system was constructed to classify patients into high- and low-risk groups, with the Gene Expression Omnibus (GEO) dataset as the validation group. Finally, the difference analysis of single-sample gene set enrichment analysis, tumor microenvironment (TME), immune cells, tumor mutational burden, and chemotherapeutic drug sensitivity between the high-risk and low-risk groups was investigated.Results: A prognostic model with four IPGs (PDIA3, CASP8, IL1, and LY96) was developed, and it was found that the group of CC patients with a higher risk score of IPGs expression had a lower survival rate. Single and multifactor Cox regression analysis also showed that this risk score was a reliable predictor of overall survival. In comparison to the low-risk group, the high-risk group had lower TME scores and immune cell infiltration, and gene set variation analysis showed that immune-related pathways were more enriched in the high-risk group.Conclusion: A risk model constructed from four IPGs can independently predict the prognosis of CC patients and recommend more appropriate immunotherapy strategies for patients.Keywords: ICD, cervical cancer, immunity, prognosis, immunotherapy response

Published
2023

42. ctDNA applications and integration in colorectal cancer: an NCI Colon and Rectal–Anal Task Forces whitepaper

Author

Dasari, Arvind, Morris, Van K, Allegra, Carmen J, Atreya, Chloe, Benson, Al B, Boland, Patrick, Chung, Ki, Copur, Mehmet S, Corcoran, Ryan B, Deming, Dustin A, Dwyer, Andrea, Diehn, Maximilian, Eng, Cathy, George, Thomas J, Gollub, Marc J, Goodwin, Rachel A, Hamilton, Stanley R, Hechtman, Jaclyn F, Hochster, Howard, Hong, Theodore S, Innocenti, Federico, Iqbal, Atif, Jacobs, Samuel A, Kennecke, Hagen F, Lee, James J, Lieu, Christopher H, Lenz, Heinz-Josef, Lindwasser, O Wolf, Montagut, Clara, Odisio, Bruno, Ou, Fang-Shu, Porter, Laura, Raghav, Kanwal, Schrag, Deborah, Scott, Aaron J, Shi, Qian, Strickler, John H, Venook, Alan, Yaeger, Rona, Yothers, Greg, You, Y Nancy, Zell, Jason A, and Kopetz, Scott

Subjects
Cancer, Clinical Research, Colo-Rectal Cancer, Digestive Diseases, Good Health and Well Being, Biomarkers, Tumor, Circulating Tumor DNA, Colon, Colorectal Neoplasms, Humans, Liquid Biopsy, National Cancer Institute (U.S.), Neoplasm, Residual, Rectal Neoplasms, United States, Oncology and Carcinogenesis
Abstract

An increasing number of studies are describing potential uses of circulating tumour DNA (ctDNA) in the care of patients with colorectal cancer. Owing to this rapidly developing area of research, the Colon and Rectal-Anal Task Forces of the United States National Cancer Institute convened a panel of multidisciplinary experts to summarize current data on the utility of ctDNA in the management of colorectal cancer and to provide guidance in promoting the efficient development and integration of this technology into clinical care. The panel focused on four key areas in which ctDNA has the potential to change clinical practice, including the detection of minimal residual disease, the management of patients with rectal cancer, monitoring responses to therapy, and tracking clonal dynamics in response to targeted therapies and other systemic treatments. The panel also provides general guidelines with relevance for ctDNA-related research efforts, irrespective of indication.

Published
2020

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

Author

Jia, S. M., Bu, Q. C., Qu, J. L., Lu, F. J., Zhang, S. N., Huang, Y., Ma, X., Tao, L., Xiao, G. C., Zhang, W., Chen, L., Song, L. M., Zhang, S., Li, T. B., Xu, Y. P., Cao, X. L., Chen, Y., Liu, C. Z., Cai, C., Chang, Z., Chen, G., Chen, T. X., Chen, Y. B., Chen, Y. P., Cui, W., Cui, W. W., Deng, J. K., Dong, Y. W., Du, Y. Y., Fu, M. X., Gao, G. H., Gao, H., Gao, M., Ge, M. Y., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huo, J., Jiang, L. H., Jiang, W. C., Jin, J., Kong, L. D., Li, 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., Liang, X. H., Liao, J. Y., Liu, G. Q., Liu, H. W., Liu, X. J., Liu, Y. N., Lu, B., Lu, X. F., Luo, Q., Luo, T., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Sai, N., Song, X. Y., Sun, L., Tan, Y., Tuo, Y. L., Wang, C., Wang, G. F., Wang, J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. Y., Wu, B. B., Wu, M., Xiao, S., Xiong, S. L., Yang, J. W., Yang, S., Yang, Y. J., Yin, Q. Q., Yi, Q. B., You, Y., Zhang, A. M., Zhang, C. M., Zhang, F., Zhang, H. M., Zhang, J., Zhang, T., Zhang, W. C., Zhang, W. Z., Zhang, Y., Zhang, Y. F., Zhang, Y. J., Zhang, Z., Zhang, Z. L., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zhou, D. K., Zhou, J. F., Zhu, Y. X., and Zhu, Y.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, High Energy Physics - Phenomenology
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 ($Insight$-HXMT) from July 2017 to August 2018. A complete $Z$-track hardness-intensity diagram (HID) is obtained. The normal branch oscillations (NBOs) at $\sim$ 6 Hz in the lower part of the normal branch (NB) and the flare branch oscillations (FBOs) at $\sim$ 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 $Insight$-HXMT, while the horizontal branch oscillations (HBOs) at $\sim$ 40 Hz and the kilohertz quasi-periodic oscillations (kHz QPOs) at $\sim$ 800 Hz are found simultaneously up to 60 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 $\sim$ 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
2019

44. Insight-HXMT observation on 4U~1608--52: evolving spectral properties of a bright type-I X-ray burst

Author

Chen, Y. P., Zhang, S., Zhang, S. N., Ji, L., Kong, L. D., Santangelo, A., Qu, J. L., Lu, F. J., Li, T. P., Song, L. M., Xu, Y. P., Cao, X. L., Chen, Y., Liu, C. Z., Bu, Q. C., Cai, C., Chang, Z., Chen, G., Chen, L., Chen, T. X., Chen, Y. B., Cui, W., Cui, W. W., Deng, J. K., Dong, Y. W., Du, Y. Y., Fu, M. X., Gao, G. H., Gao, H., Gao, M., Ge, M. Y., Gu, Y. D., Guan, J., Guo, C. C., Han, D. W., Huang, Y., Huo, J., Jia, S. M., Jiang, L. H., Jiang, W. C., Jin, J., Li, 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., Liang, X. H., Liu, J. Y. Liao G. Q., Liu, H. W., Liu, X. J., Liu, Y. N., Lu, B., Lu, X. F., Luo, Q., Luo, T., Ma, X., Meng, B., Nang, Y., Nie, J. Y., Ou, G., Sai, N., Sun, L., Tan, Y., Tao, L., Tuo, Y. L., Wang, C., Wang, G. F., Wang, J., Wang, W. S., Wang, Y. S., Wen, X. Y., Wu, B. Y., Wu, B. B., Wu, M., Xiao, G. C., Xiao, S., Xiong, S. L., Yang, J. W., Yang, S., Yang, Yang-Ji, Yang, Yi-Jung, Yi, Q. B., Yin, Q. Q., You, Y., Zhang, A. M., Zhang, C. L., Zhang, C. M., Zhang, F., Zhang, H. M., Zhang, J., Zhang, T., Zhang, W. C., Zhang, W., Zhang, W. Z., Zhang, Yi., Zhang, Y. F., Zhang, Y. J., Zhang, Yue., Zhang, Z., Zhang, Z. L., Zhao, H. S., Zhao, X. F., Zheng, S. J., Zhou, D. K., Zhou, J. F., Zhu, Y., and Zhu, Y. X.

Subjects
Astrophysics - High Energy Astrophysical Phenomena
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 $\sim$ 40 percentages. We speculate that the enhanced emission is from a region beyond the PRE radius, or through the Comptonization of the corona., Comment: accepted by JHEA(Journal of High Energy Astrophysics)

Published
2019

45. Role of remote interfacial phonons in the resistivity of graphene

Author

You, Y. G., Ahn, J. H., Park, B. H., Kwon, Y., Campbell, E. E. B., and Jhang, S. H.

Subjects
Condensed Matter - Mesoscale and Nanoscale Physics
Abstract

The temperature ($\it T$) dependence of electrical resistivity in graphene has been experimentally investigated between 10 and 400 K for samples prepared on various substrates; HfO$_2$, SiO$_2$ and h-BN. The resistivity of graphene shows a linear $\it T$-dependence at low $\it T$ and becomes superlinear above a substrate-dependent transition temperature. The results are explained by remote interfacial phonon scattering by surface optical phonons at the substrates. The use of an appropriate substrate can lead to a significant improvement in the charge transport of graphene.

Published
2019
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46. Patient-reported Bowel Function and Bowel-related Quality of Life After Pelvic Radiation for Rectal Adenocarcinoma: The Impact of Radiation Fractionation and Surgical Resection

Author

Rooney, Michael K., De, Brian, Corrigan, Kelsey, Smith, Grace L., Taniguchi, Cullen, Minsky, Bruce D., Ludmir, Ethan B., Koay, Eugene J., Das, Prajnan, Koong, Albert C., Peacock, Oliver, Chang, George, You, Y. Nancy, Morris, Van K., Nogueras-González, Graciela, and Holliday, Emma B.

Published
2023
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47. Experimental Investigation of Temperature Influence on Nanoparticle Adhesion in an Artificial Blood Vessel

Author

Yue K, Yang C, You Y, Wang X, and Zhang X

Subjects
artificial vessel, drug delivery, nanoparticle, temperature variation, particle–wall adhesion, Medicine (General), R5-920
Abstract

Kai Yue,1,2 Chao Yang,1 Yu You,1,2 Xueying Wang,3 Xinxin Zhang1 1School of Energy and Environmental Engineering, University of Science and Technology Beijing, Beijing, 100083, People’s Republic of China; 2Shunde Graduate School of University of Science and Technology Beijing, Shunde, Guangdong Province, 528399, People’s Republic of China; 3School of Chemistry and Chemical Engineering, University of Jinan, Jinan, Shandong Province, 250022, People’s Republic of ChinaCorrespondence: Kai Yue, Email yuekai@ustb.edu.cnBackground: A good understanding of the adhesion behaviors of the nanocarriers in microvessels in chemo-hyperthermia synergistic therapy is conducive to nanocarrier design for targeted drug delivery.Methods: In this study, we constructed an artificial blood vessel system using gelatins with a complete endothelial monolayer formed on the inner vessel wall. The numbers of adhered NPs under different conditions were measured, as well as the interaction forces between the arginine–glycine–aspartic acid (RGD) ligands and endothelial cells.Results: The experimental results on the adhesion of ligand–coated nanoparticles (NPs) with different sizes and morphologies in the blood vessel verified that the gelatin-based artificial vessel possessed good cytocompatibility and mechanical properties, which are suitable for the investigation on NP adhesion characteristics in microvessels. When the temperature deviated from 37 °C, an increase or decrease in temperature resulted in a decrease in the number of adhered NPs, but the margination probability of NP adhesion increased at high temperatures due to the enhanced Brownian movement and flow disturbance. It is found that the effect of cooling was less than that of heating according to the observed changes in cell morphology and a decrease in cell activity under the static and perfusion culture conditions within the temperature range of 25 °C– 43 °C. Furthermore, the measurement results of change in the RGD ligand-cell interaction with temperature showed good agreement with those in the number of adhered NPs.Conclusion: The Findings suggest that designing ligands that can bind to the receptor and are least susceptible to temperature variation can be an effective means to enhance drug retention.Keywords: artificial vessel, drug delivery, nanoparticle, temperature variation, particle–wall adhesion

Published
2023

49. Global, regional, and national burden of disorders affecting the nervous system, 1990–2021: a systematic analysis for the Global Burden of Disease Study 2021

Author

Steinmetz, J, Seeher, K, Schiess, N, Nichols, E, Cao, B, Servili, C, Cavallera, V, Cousin, E, Hagins, H, Moberg, M, Mehlman, M, Abate, Y, Abbas, J, Abbasi, M, Abbasian, M, Abbastabar, H, Abdelmasseh, M, Abdollahi, M, Abdollahifar, M, Abd-Rabu, R, Abdulah, D, Abdullahi, A, Abedi, A, Abedi, V, Abeldano Zuniga, R, Abidi, H, Abiodun, O, Aboagye, R, Abolhassani, H, Aboyans, V, Abrha, W, Abualhasan, A, Abu-Gharbieh, E, Aburuz, S, Adamu, L, Addo, I, Adebayo, O, Adekanmbi, V, Adekiya, T, Adikusuma, W, Adnani, Q, Adra, S, Afework, T, Afolabi, A, Afraz, A, Afzal, S, Aghamiri, S, Agodi, A, Agyemang-Duah, W, Ahinkorah, B, Ahmad, A, Ahmad, D, Ahmad, S, Ahmadzade, A, Ahmed, A, Ahmed, H, Ahmed, J, Ahmed, L, Ahmed, M, Ahmed, S, Ajami, M, Aji, B, Ajumobi, O, Akade, S, Akbari, M, Akbarialiabad, H, Akhlaghi, S, Akinosoglou, K, Akinyemi, R, Akonde, M, Al Hasan, S, Alahdab, F, Al-Ahdal, T, Al-Amer, R, Albashtawy, M, Albataineh, M, Aldawsari, K, Alemi, H, Alemi, S, Algammal, A, Al-Gheethi, A, Alhalaiqa, F, Alhassan, R, Ali, A, Ali, E, Ali, L, Ali, M, Ali, R, Ali, S, Shujait Ali, S, Ali, Z, Alif, S, Alimohamadi, Y, Aliyi, A, Aljofan, M, Aljunid, S, Alladi, S, Almazan, J, Almustanyir, S, Al-Omari, B, Alqahtani, J, Alqasmi, I, Alqutaibi, A, Al-Shahi Salman, R, Altaany, Z, Al-Tawfiq, J, Altirkawi, K, Alvis-Guzman, N, Al-Worafi, Y, Aly, H, Aly, S, Alzoubi, K, Amani, R, Amindarolzarbi, A, Amiri, S, Amirzade-Iranaq, M, Amu, H, Amugsi, D, Amusa, G, Amzat, J, Ancuceanu, R, Anderlini, D, Anderson, D, Andrei, C, Androudi, S, Angappan, D, Angesom, T, Anil, A, Ansari-Moghaddam, A, Anwer, R, Arafat, M, Aravkin, A, Areda, D, Ariffin, H, Arifin, H, Arkew, M, Arnlov, J, Arooj, M, Artamonov, A, Artanti, K, Aruleba, R, Asadi-Pooya, A, Asena, T, Asghari-Jafarabadi, M, Ashraf, M, Ashraf, T, Atalell, K, Athari, S, Atinafu, B, Atorkey, P, Atout, M, Atreya, A, Aujayeb, A, Avan, A, Ayala Quintanilla, B, Ayatollahi, H, Ayinde, O, Mohammad Ayyoubzadeh, S, Azadnajafabad, S, Azizi, Z, Azizian, K, Azzam, A, Babaei, M, Badar, M, Badiye, A, Baghdadi, S, Bagherieh, S, Bai, R, Baig, A, Balakrishnan, S, Balalla, S, Baltatu, O, Banach, M, Bandyopadhyay, S, Banerjee, I, Baran, M, Barboza, M, Barchitta, M, Bardhan, M, Barker-Collo, S, Barnighausen, T, Barrow, A, Bashash, D, Bashiri, H, Bashiru, H, Basiru, A, Basso, J, Basu, S, Batiha, A, Batra, K, Baune, B, Bedi, N, Begde, A, Begum, T, Behnam, B, Behnoush, A, Beiranvand, M, Bejot, Y, Bekele, A, Belete, M, Belgaumi, U, Bemanalizadeh, M, Bender, R, Benfor, B, Bennett, D, Bensenor, I, Berice, B, Bettencourt, P, Beyene, K, Bhadra, A, Bhagat, D, Bhangdia, K, Bhardwaj, N, Bhardwaj, P, Bhargava, A, Bhaskar, S, Bhat, A, Bhat, V, Bhatti, G, Bhatti, J, Bhatti, R, Bijani, A, Bikbov, B, Bilalaga, M, Biswas, A, Bitaraf, S, Bitra, V, Bjorge, T, Bodolica, V, Bodunrin, A, Boloor, A, Braithwaite, D, Brayne, C, Brenner, H, Briko, A, Bringas Vega, M, Brown, J, Budke, C, Buonsenso, D, Burkart, K, Burns, R, Bustanji, Y, Butt, M, Butt, N, Butt, Z, Cabral, L, dos Santos, F, Calina, D, Campos-Nonato, I, Cao, C, Carabin, H, Cardenas, R, Carreras, G, Carvalho, A, Castaneda-Orjuela, C, Casulli, A, Catala-Lopez, F, Catapano, A, Caye, A, Cegolon, L, Cenderadewi, M, Cerin, E, Chacon-Uscamaita, P, Chan, J, Chanie, G, Charan, J, Chattu, V, Chekol Abebe, E, Chen, H, Chen, J, Chi, G, Chichagi, F, Chidambaram, S, Chimoriya, R, Ching, P, Chitheer, A, Chong, Y, Chopra, H, Choudhari, S, Chowdhury, E, Chowdhury, R, Christensen, H, Chu, D, Chukwu, I, Chung, E, Coberly, K, Columbus, A, Comachio, J, Conde, J, Cortesi, P, Costa, V, Couto, R, Criqui, M, Cruz-Martins, N, Dabbagh Ohadi, M, Dadana, S, Dadras, O, Dai, X, Dai, Z, D'Amico, E, Danawi, H, Dandona, L, Dandona, R, Darwish, A, Das, S, Dascalu, A, Dash, N, Dashti, M, De la Hoz, F, de la Torre-Luque, A, De Leo, D, Dean, F, Dehghan, A, Dejene, H, Demant, D, Demetriades, A, Demissie, S, Deng, X, Desai, H, Devanbu, V, Dhama, K, Dharmaratne, S, Dhimal, M, Dias da Silva, D, Diaz, D, Dibas, M, Ding, D, Dinu, M, Dirac, M, Diress, M, Do, T, Doan, K, Dodangeh, M, Doheim, M, Dokova, K, Dongarwar, D, Dsouza, H, Dube, J, Duraisamy, S, Durojaiye, O, Dutta, S, Dziedzic, A, Edinur, H, Eissazade, N, Ekholuenetale, M, Ekundayo, T, El Nahas, N, El Sayed, I, Elahi Najafi, M, Elbarazi, I, Elemam, N, Elgar, F, Elgendy, I, Elhabashy, H, Elhadi, M, Elilo, L, Ellenbogen, R, Elmeligy, O, Elmonem, M, Elshaer, M, Elsohaby, I, Emamverdi, M, Emeto, T, Endres, M, Esezobor, C, Eskandarieh, S, Fadaei, A, Fagbamigbe, A, Fahim, A, Faramarzi, A, Fares, J, Farjoud Kouhanjani, M, Faro, A, Farzadfar, F, Fatehizadeh, A, Fathi, M, Fathi, S, Fatima, S, Feizkhah, A, Fereshtehnejad, S, Ferrari, A, Ferreira, N, Fetensa, G, Firouraghi, N, Fischer, F, Fonseca, A, Force, L, Fornari, A, Foroutan, B, Fukumoto, T, Gadanya, M, Gaidhane, A, Galali, Y, Galehdar, N, Gan, Q, Gandhi, A, Ganesan, B, Gardner, W, Garg, N, Gau, S, Gautam, R, Gebre, T, Gebrehiwot, M, Gebremeskel, G, Gebreslassie, H, Getacher, L, Ghaderi Yazdi, B, Ghadirian, F, Ghaffarpasand, F, Ghanbari, R, Ghasemi, M, Ghazy, R, Ghimire, S, Gholami, A, Gholamrezanezhad, A, Ghotbi, E, Ghozy, S, Gialluisi, A, Gill, P, Glasstetter, L, Gnedovskaya, E, Golchin, A, Golechha, M, Goleij, P, Golinelli, D, Gomes-Neto, M, Goulart, A, Goyal, A, Gray, R, Grivna, M, Guadie, H, Guan, B, Guarducci, G, Guicciardi, S, Gunawardane, D, Guo, H, Gupta, B, Gupta, R, Gupta, S, Gupta, V, Gutierrez, R, Habibzadeh, F, Hachinski, V, Haddadi, R, Hadei, M, Hadi, N, Haep, N, Haile, T, Haj-Mirzaian, A, Hall, B, Halwani, R, Hameed, S, Hamiduzzaman, M, Hammoud, A, Han, H, Hanifi, N, Hankey, G, Hannan, M, Hao, J, Harapan, H, Hareru, H, Hargono, A, Harlianto, N, Haro, J, Hartman, N, Hasaballah, A, Hasan, F, Hasani, H, Hasanian, M, Hassan, A, Hassan, S, Hassanipour, S, Hassankhani, H, Hassen, M, Haubold, J, Hay, S, Hayat, K, Hegazy, M, Heidari, G, Heidari, M, Heidari-Soureshjani, R, Hesami, H, Hezam, K, Hiraike, Y, Hoffman, H, Holla, R, Hopf, K, Horita, N, Hossain, M, Hossain, S, Hosseinzadeh, 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I., Eskandarieh S., Fadaei A., Fagbamigbe A. F., Fahim A., Faramarzi A., Fares J., Farjoud Kouhanjani M., Faro A., Farzadfar F., Fatehizadeh A., Fathi M., Fathi S., Fatima S. A. F., Feizkhah A., Fereshtehnejad S. -M., Ferrari A. J., Ferreira N., Fetensa G., Firouraghi N., Fischer F., Fonseca A. C., Force L. M., Fornari A., Foroutan B., Fukumoto T., Gadanya M. A., Gaidhane A. M., Galali Y., Galehdar N., Gan Q., Gandhi A. P., Ganesan B., Gardner W. M., Garg N., Gau S. -Y., Gautam R. K., Gebre T., Gebrehiwot M., Gebremeskel G. G., Gebreslassie H. G., Getacher L., Ghaderi Yazdi B., Ghadirian F., Ghaffarpasand F., Ghanbari R., Ghasemi M., Ghazy R. M., Ghimire S., Gholami A., Gholamrezanezhad A., Ghotbi E., Ghozy S., Gialluisi A., Gill P. S., Glasstetter L. M., Gnedovskaya E. V., Golchin A., Golechha M., Goleij P., Golinelli D., Gomes-Neto M., Goulart A. C., Goyal A., Gray R. J., Grivna M., Guadie H. A., Guan B., Guarducci G., Guicciardi S., Gunawardane D. A., Guo H., Gupta B., Gupta R., Gupta S., Gupta V. B., Gupta V. K., Gutierrez R. A., Habibzadeh F., Hachinski V., Haddadi R., Hadei M., Hadi N. R., Haep N., Haile T. G., Haj-Mirzaian A., Hall B. J., Halwani R., Hameed S., Hamiduzzaman M., Hammoud A., Han H., Hanifi N., Hankey G. J., Hannan M. A., Hao J., Harapan H., Hareru H. E., Hargono A., Harlianto N. I., Haro J. M., Hartman N. N., Hasaballah A. I., Hasan F., Hasani H., Hasanian M., Hassan A., Hassan S., Hassanipour S., Hassankhani H., Hassen M. B., Haubold J., Hay S. I., Hayat K., Hegazy M. I., Heidari G., Heidari M., Heidari-Soureshjani R., Hesami H., Hezam K., Hiraike Y., Hoffman H. J., Holla R., Hopf K. P., Horita N., Hossain M. M., Hossain M. B., Hossain S., Hosseinzadeh H., Hosseinzadeh M., Hostiuc S., Hu C., Huang J., Huda M. N., Hussain J., Hussein N. R., Huynh H. -H., Hwang B. -F., Ibitoye S. E., Ilaghi M., Ilesanmi O. S., Ilic I. M., Ilic M. D., Immurana M., Iravanpour F., Islam S. M. S., Ismail F., Iso H., Isola G., Iwagami M., Iwu C. C. D., Iyer M., Jaan A., Jacob L., Jadidi-Niaragh F., Jafari M., Jafarinia M., Jafarzadeh A., Jahankhani K., Jahanmehr N., Jahrami H., Jaiswal A., Jakovljevic M., Jamora R. D. G., Jana S., Javadi N., Javed S., Javeed S., Jayapal S. K., Jayaram S., Jiang H., Johnson C. O., Johnson W. D., Jokar M., Jonas J. B., Joseph A., Joseph N., Joshua C. E., Jurisson M., Kabir A., Kabir Z., Kabito G. G., Kadashetti V., Kafi F., Kalani R., Kalantar F., Kaliyadan F., Kamath A., Kamath S., Kanchan T., Kandel A., Kandel H., Kanmodi K. K., Karajizadeh M., Karami J., Karanth S. D., Karaye I. M., Karch A., Karimi A., Karimi H., Karimi Behnagh A., Kasraei H., Kassebaum N. J., Kauppila J. H., Kaur H., Kaur N., Kayode G. A., Kazemi F., Keikavoosi-Arani L., Keller C., Keykhaei M., Khadembashiri M. A., Khader Y. S., Khafaie M. A., Khajuria H., Khalaji A., Khamesipour F., Khammarnia M., Khan M., Khan M. A. B., Khan Y. H., Suheb M. Z. K., Khanmohammadi S., Khanna T., Khatab K., Khatatbeh H., Khatatbeh M. M., Khateri S., Khatib M. N., Khayat Kashani H. R., Khonji M. S., Khorashadizadeh F., Khormali M., Khubchandani J., Kian S., Kim G., Kim J., Kim M. S., Kim Y. J., Kimokoti R. W., Kisa A., Kisa S., Kivimaki M., Kochhar S., Kolahi A. -A., Koly K. N., Kompani F., Koroshetz W. J., Kosen S., Kourosh Arami M., Koyanagi A., Kravchenko M. A., Krishan K., Krishnamoorthy V., Defo B. K., Kuddus M. A., Kumar A., Kumar G. A., Kumar M., Kumar N., Kumsa N. B., Kundu S., Kurniasari M. D., Kusuma D., Kuttikkattu A., Kyu H. H., La Vecchia C., Ladan M. A., Lahariya C., Laksono T., Lal D. K., Lallukka T., Lam J., Lami F. H., Landires I., Langguth B., Lasrado S., Latief K., Latifinaibin K., Lau K. M. -M., Laurens M. B., Lawal B. K., Le L. K. D., Le T. T. T., Ledda C., Lee M., Lee S. -W., Lee S. W., Lee W. -C., Lee Y. H., Leonardi M., Lerango T. L., Li M. -C., Li W., Ligade V. S., Lim S. S., Linehan C., Liu C., Liu J., Liu W., Lo C. -H., Lo W. D., Lobo S. W., Logroscino G., Lopes G., Lopukhov P. D., Lorenzovici L., Lorkowski S., Loureiro J. A., Lubinda J., Lucchetti G., Saute R. L., Ma Z. F., Mabrok M., Machoy M., Madadizadeh F., El Razek M. M. A., Maghazachi A. A., Maghbouli N., Mahjoub S., Mahmoudi M., Majeed A., Malagon-Rojas J. N., Malakan Rad E., Malhotra K., Malik A. A., Malik I., Mallhi T. H., Malta D. C., Manilal A., Mansouri V., Mansournia M. A., Marasini B. P., Marateb H. R., Maroufi S. F., Martinez-Raga J., Martini S., Martins-Melo F. R., Martorell M., Marz W., Marzo R. R., Massano J., Mathangasinghe Y., Mathews E., Maude R. J., Maugeri A., Maulik P. K., Mayeli M., Mazaheri M., McAlinden C., McGrath J. J., Meena J. K., Mehndiratta M. M., Mendez-Lopez M. A. M., Mendoza W., Mendoza-Cano O., Menezes R. G., Merati M., Meretoja A., Merkin A., Mersha A. M., Mestrovic T., Mi T., Miazgowski T., Michalek I. M., Mihretie E. T., Minh L. H. N., Mirfakhraie R., Mirica A., Mirrakhimov E. M., Mirzaei M., Misganaw A., Misra S., Mithra P., Mizana B. A., Mohamadkhani A., Mohamed N. S., Mohammadi E., Mohammadi H., Mohammadi S., Mohammadshahi M., Mohammed M., Mohammed S., Mohan S., Mojiri-Forushani H., Moka N., Mokdad A. H., Molinaro S., Moller H., Monasta L., Moniruzzaman M., Montazeri F., Moradi M., Moradi Y., Moradi-Lakeh M., Moraga P., Morovatdar N., Morrison S. D., Mosapour A., Mosser J. F., Mossialos E., Motaghinejad M., Mousavi P., Ehsan Mousavi S., Mubarik S., Muccioli L., Mughal F., Mukoro G. D., Mulita A., Mulita F., Musaigwa F., Mustafa A., Mustafa G., Muthu S., Nagarajan A. J., Naghavi P., Naik G. R., Nainu F., Nair T. S., Najmuldeen H. H. R., Nakhostin Ansari N., Nambi G., Namdar Areshtanab H., Nargus S., Nascimento B. R., Naser A. Y., Nashwan A. J. J., Nasoori H., Nasreldein A., Natto Z. S., Nauman J., Nayak B. P., Nazri-Panjaki A., Negaresh M., Negash H., Negoi I., Negoi R. I., Negru S. M., Nejadghaderi S. 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M., Saravanan A., Sarveazad A., Satpathy M., Saylan M., Sayyah M., Scarmeas N., Schlaich M. P., Schuermans A., Schwarzinger M., Schwebel D. C., Selvaraj S., Sendekie A. K., Sengupta P., Senthilkumaran S., Serban D., Sergindo M. T., Sethi Y., SeyedAlinaghi S., Seylani A., Shabani M., Shabany M., Shafie M., Shahabi S., Shahbandi A., Shahid S., Shahraki-Sanavi F., Shahsavari H. R., Shahwan M. J., Shaikh M. A., Shaji K. S., Sham S., Shama A. T. T., Shamim M. A., Shams-Beyranvand M., Shamsi M. A., Shanawaz M., Sharath M., Sharfaei S., Sharifan A., Sharma M., Sharma R., Shashamo B. B., Shayan M., Sheikhi R. A., Shekhar S., Shen J., Shenoy S. M., Shetty P. H., Shiferaw D. S., Shigematsu M., Shiri R., Shittu A., Shivakumar K. M., Shokri F., Shool S., Shorofi S. A., Shrestha S., Siankam Tankwanchi A. B., Siddig E. E., Sigfusdottir I. D., Silva J. P., Silva L. M. L. R., Sinaei E., Singh B. B., Singh G., Singh P., Singh S., Sirota S. B., Sivakumar S., Sohag A. A. 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Abstract

Background: Disorders affecting the nervous system are diverse and include neurodevelopmental disorders, late-life neurodegeneration, and newly emergent conditions, such as cognitive impairment following COVID-19. Previous publications from the Global Burden of Disease, Injuries, and Risk Factor Study estimated the burden of 15 neurological conditions in 2015 and 2016, but these analyses did not include neurodevelopmental disorders, as defined by the International Classification of Diseases (ICD)-11, or a subset of cases of congenital, neonatal, and infectious conditions that cause neurological damage. Here, we estimate nervous system health loss caused by 37 unique conditions and their associated risk factors globally, regionally, and nationally from 1990 to 2021. Methods: We estimated mortality, prevalence, years lived with disability (YLDs), years of life lost (YLLs), and disability-adjusted life-years (DALYs), with corresponding 95% uncertainty intervals (UIs), by age and sex in 204 countries and territories, from 1990 to 2021. We included morbidity and deaths due to neurological conditions, for which health loss is directly due to damage to the CNS or peripheral nervous system. We also isolated neurological health loss from conditions for which nervous system morbidity is a consequence, but not the primary feature, including a subset of congenital conditions (ie, chromosomal anomalies and congenital birth defects), neonatal conditions (ie, jaundice, preterm birth, and sepsis), infectious diseases (ie, COVID-19, cystic echinococcosis, malaria, syphilis, and Zika virus disease), and diabetic neuropathy. By conducting a sequela-level analysis of the health outcomes for these conditions, only cases where nervous system damage occurred were included, and YLDs were recalculated to isolate the non-fatal burden directly attributable to nervous system health loss. A comorbidity correction was used to calculate total prevalence of all conditions that affect the nervous s

Published
2024

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