A1 Journal article – refereed

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




List of Authors: Ji L, Ducci L, Santangelo A, Zhang S, Suleimanov V, Tsygankov S, Doroshenko V, Nabizadeh A, Zhang SN, Ge MY, Tao L, Bu QC, Qu JL, Lu FJ, Chen L, Song LM, Li TP, Xu YP, Cao XL, Chen Y, Liu CZ, Cai C, Chang Z, Chen G, Chen TX, Chen YB, Chen YP, Cui W, Cui WW, Deng JK, Dong YW, Du YY, Fu MX, Gao GH, Gao H, Gao M, Gu YD, Guan J, Guo CC, Han DW, Huang Y, Huo J, Jia SM, Jiang LH, Jiang WC, Jin J, Jin YJ, Kong LD, Li B, Li CK, Li G, Li MS, Li W, Li X, Li XB, Li XF, Li YG, Li ZW, Liang XH, Liao JY, Liu BS, Liu GQ, Liu HX, Liu HW, Liu XJ, Liu YN, Lu B, Lu XF, Luo Q, Luo T, Ma X, Meng B, Nang Y, Nie JY, Ou G, Sai N, Shang RC, Song XY, Sun L, Tan Y, Tuo YL, Wang C, Wang GF, Wang J, Wang PJ, Wang WS, Wang YS, Wen XY, Wu BY, Wu BB, Wu M, Xiao GC, Xiao S, Xiong SL, Xu H, Yang JW, Yang S, Yang YJ, Yang YJ, Yi QB, Yin QQ, You Y, Zhang AM, Zhang CM, Zhang F, Zhang HM, Zhang J, Zhang P, Zhang T, Zhang W, Zhang WC, Zhang WZ, Zhang Y, Zhang YF, Zhang YJ, Zhang YH, Zhang Y, Zhang Z, Zhang Z, Zhang ZL, Zhao HS, Zhao XF, Zheng SJ, Zhou DK, Zhou JF, Zhu YX, Zhu Y, Zhuang RL

Publisher: OXFORD UNIV PRESS

Publication year: 2020

Journal: Monthly Notices of the Royal Astronomical Society

Journal name in source: MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY

Journal acronym: MON NOT R ASTRON SOC

Volume number: 493

Issue number: 4

Number of pages: 13

ISSN: 0035-8711

eISSN: 1365-2966

DOI: http://dx.doi.org/10.1093/mnras/staa569


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 similar to 1.5. The pulse-profile shape during the flares can be significantly different from 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 supercritical 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.

Downloadable publication

This is an electronic reprint of the original article.
This reprint may differ from the original in pagination and typographic detail. Please cite the original version.




Last updated on 2021-24-06 at 10:01