2020MNRAS.493.5680J

Query : 2020MNRAS.493.5680J

2020MNRAS.493.5680J - Mon. Not. R. Astron. Soc., 493, 5680-5692 (2020/April-3)

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

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., 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.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., SAI N., SHANG R.C., 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., 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 P., ZHANG T., ZHANG W., ZHANG W.C., ZHANG W.Z., ZHANG Y., ZHANG Y.F., ZHANG Y.J., ZHANG Y.H., ZHANG Y., ZHANG Z., ZHANG Z., ZHANG Z.L., ZHAO H.S., ZHAO X.F., ZHENG S.J., ZHOU D.K., ZHOU J.F., ZHU Y.X., ZHU Y. and ZHUANG R.L.

Abstract (from CDS):

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 ∼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.

Abstract Copyright: © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): stars: neutron - X-rays: binaries - X-rays: individual: 4U 1901+03

Simbad objects: 7

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Number of rows : 7
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 SK 160 HXB 01 17 05.1457288392 -73 26 36.014808156 12.23 13.00 13.15   13.17 O9.7Ia+ 918 0
2 X LMC X-4 HXB 05 32 49.5556042296 -66 22 13.202721768   13.9 14.0 14.290   O8III 714 0
3 1A 0535-668 HXB 05 35 40.9970566152 -66 51 53.547559416       15.036 15.138 B2IIIe 302 0
4 HD 245770 HXB 05 38 54.5748918624 +26 18 56.836952784 9.30 9.84 9.39 8.77 8.30 O9/B0III/Ve 1045 0
5 SWIFT J1626.5-5156 HXB 16 26 36.5197704024 -51 56 30.600051936       16.03 14.59 B0V 94 0
6 3FHL J1746.2-2852 LXB 17 44 33.09 -28 44 27.0           ~ 559 0
7 4U 1901+03 HXB 19 03 39.3926409480 +03 12 15.758070228           B8-9IV 122 0

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