SIMBAD references

2020MNRAS.491.1857D - Mon. Not. R. Astron. Soc., 491, 1857-1867 (2020/January-2)

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

DOROSHENKO V., ZHANG S.N., SANTANGELO A., JI L., TSYGANKOV S., MUSHTUKOV A., QU L.J., ZHANG S., GE M.Y., CHEN Y.P., BU Q.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., HU 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.J., LI Z.W., LIANG X.H., LIAO J.Y., LIU C.Z., LIU G.Q., LIU H.W., LIU S.Z., LIU X.J., LIU Y., LIU Y.N., LU B., LU F.J., LU X.F., LUO T., MA X., MENG B., NANG Y., NIE J.Y., OU G., SAI N., SHANG R.C., SONG L.M., SONG X.Y., SUN L., TAN Y., TAO L., TUO Y.L., WANG G.F., WANG J., WANG W.S., WANG Y.S., WEN X.Y., WU B.B., WU M., XIAO G.C., XIONG S.L., XU H., XU Y.P., YANG Y.R., YANG J.W., YANG S., YANG Y.J., ZHANG A.M., ZHANG C.L., ZHANG C.M., ZHANG F., ZHANG H.M., ZHANG J., ZHANG Q., ZHANG T., ZHANG W., ZHANG W.C., ZHANG W.Z., ZHANG Y., ZHANG Y., ZHANG Y.F., ZHANG Y.J., ZHANG Z., ZHANG Z.L., ZHAO H.S., ZHAO J.L., ZHAO X.F., ZHENG S.J., ZHU Y., ZHU Y.X., ZOU C.L. and ZHANG R.L.

Abstract (from CDS):

We report on analysis of observations of the bright transient X-ray pulsar (XRP) Swift J0243.6+6124 obtained during its 2017-2018 giant outburst with Insight-HXMT, NuSTAR, and Swift observatories. We focus on the discovery of a sharp state transition of the timing and spectral properties of the source at super-Eddington accretion rates, which we associate with the transition of the accretion disc to a radiation pressure dominated state, the first ever directly observed for magnetized neutron star. This transition occurs at slightly higher luminosity compared to already reported transition of the source from sub- to supercritical accretion regime associate with onset of an accretion column. We argue that this scenario can only be realized for comparatively weakly magnetized neutron star, not dissimilar to other ultra-luminous X-ray pulsars, which accrete at similar rates. Further evidence for this conclusion is provided by the non-detection of the transition to the propeller state in quiescence which strongly implies compact magnetosphere and thus rules out magnetar-like fields.

Abstract Copyright: © 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): accretion - accretion discs - stars: magnetic field - stars: neutron - pulsars: general - pulsars: individual: Swift J0243.6+6124 - X-rays: binaries

Simbad objects: 4

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2023.02.09-07:22:03

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