2022ApJ...937...33Y

Query : 2022ApJ...937...33Y

2022ApJ...937...33Y - Astrophys. J., 937, 33 (2022/September-3)

An Insight-HXMT View of the mHz Quasi-regular Modulation Phenomenon in the Black Hole X-Ray Binary 4U 1630-47.

YANG Z.-X., ZHANG L., HUANG Y., BU Q., ZHANG Z., LIU H.-X., YU W., WANG P.-J., ZHAO Q.C., TAO L., QU J.-L., ZHANG S., ZHANG S.-N., SONG L., LU F., CAO X., CHEN L., CAI C., CHANG Z., CHEN T., CHEN Y., CHEN Y., CHEN Y., CUI W., DING G., DU Y., GAO G., GAO H., GE M., GU Y., GUAN J., GUO C., HAN D., HUO J., JIA S., JIANG W., JIN J., KONG L., LI B., LI G., LI W., LI X., LI X., LI Z., LI C., LIN L., LIU C., LI T., LI X., LIANG X., LIAO J., LIU H., LIU X., LU X., LUO Q., LUO T., MA B., MA R., MA X., MENG B., NANG Y., NIE J., OU G., REN X., SAI N., SONG X., SUN L., TAN Y., TUO Y., WANG C., WANG W., WANG L., WANG Y., WANG J., WEN X., WU B., WU B., WU M., XIAO S., XU Y., XIONG S., YANG S., YANG Y., YI Q., YIN Q., YOU Y., ZHANG B., ZHANG F., ZHANG H., ZHANG J., ZHANG W., ZHANG W., ZHANG B., ZHANG P., ZHANG Y., ZHANG Y., ZHAO H., ZHAO X., ZHENG S. and ZHOU D.

Abstract (from CDS):

Here we report the spectral-timing results of the black hole X-ray binary 4U 1630-47 during its 2021 outburst using observations from the Hard X-ray Modulation Telescope (Insight-HXMT). Type C quasi-periodic oscillations (QPOs) in ∼1.6-4.2 Hz and quasi-regular modulation (QRM) near 60 mHz are detected during the outburst. The mHz QRM has a fractional rms of ∼10%-16% in the 8-35 keV energy band with a Q factor (frequency/width) of ∼2-4. Benefiting from the broad energy band of Insight-HXMT, we study the energy dependence of the ∼60 mHz QRM in 1-100 keV for the first time. We find that the fractional rms of the mHz QRM increases with photon energy, while the time lags of the mHz QRM are soft and decrease with photon energy. Fast recurrence of the mHz QRM, in a timescale of less than 1 hr, has been observed during the outburst. During this period, the corresponding energy spectra moderately change when the source transitions from the QRM state to the non-QRM state. The QRM phenomenon also shows a dependence with the accretion rate. We suggest that the QRM could be caused by an unknown accretion instability aroused from the corona.

Abstract Copyright: © 2022. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Accretion - Astrophysical black holes - Low-mass x-ray binary stars - Stellar mass black holes

Simbad objects: 11

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Number of rows : 11
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 V* QX Nor LXB 16 12 43.0 -52 25 26           ~ 946 1
2 1RXS J161741.2-510455 X 16 17 41.375 -51 04 55.23           ~ 3 0
3 X Nor X-1 LXB 16 34 01.610 -47 23 34.80           ~ 579 0
4 4U 1642-45 LXB 16 45 48.1 -45 36 42           ~ 467 1
5 V* V1033 Sco HXB 16 54 00.1423963019 -39 50 44.761701340       16.14   F3-6IV 1980 0
6 V* V821 Ara LXB 17 02 49.3876391280 -48 47 23.087954544         15.322 ~ 2237 0
7 IGR J17091-3624 LXB 17 09 07.61 -36 24 25.7           ~ 320 1
8 NAME XTE J17464-3213 LXB 17 46 15.59637 -32 14 00.8600           ~ 805 0
9 V* NP Ser LXB 18 16 01.7 -14 02 09   18.8       K 683 2
10 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2810 0
11 V* V404 Cyg HXB 20 24 03.8247037434 +33 52 01.961154861           G9/K0III/V 1370 0

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