2021RAA....21...70L

Query : 2021RAA....21...70L

2021RAA....21...70L - Research in Astron. and astroph., 21, 70-70 (2021/March-0)

Timing analysis of the black hole candidate EXO 1846-031 with Insight-HXMT monitoring.

LIU H.-X., HUANG Y., XIAO G.-C., BU Q.-C., QU J.-L., ZHANG S., ZHANG S.-N., JIA S.-M., LU F.-J., MA X., TAO L., ZHANG W., 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., GE M.-Y., GU Y.-D., GUAN J., GUO C.-C., HAN D.-W., HUO J., 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., 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 J., WANG L.-J., WANG W.-S., WANG Y.-S., WEN X.-Y., WU B.-Y., WU B.-B., WU M., 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 T., 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., ZHENG Y.-G., ZHOU D.-K., ZHOU J.-F., ZHU Y.-X., ZHUANG R.-L. and ZHU Y.

Abstract (from CDS):

We present the observational results from a detailed timing analysis of the black hole candidate EXO 1846-031 during its outburst in 2019 with the observations of Insight-HXMT, NICER and MAXI. This outburst can be classified roughly into four different states. Type-C quasi-periodic oscillations (QPOs) observed by NICER (about 0.1-6 Hz) and Insight-HXMT (about 0.7-8 Hz) are also reported in this work. Meanwhile, we study various physical quantities related to QPO frequency. The QPO rms-frequency relationship in the energy band 1-10 keV indicates that there is a turning pointing in frequency around 2 Hz, which is similar to that of GRS 1915+105. A possible hypothesis for the relationship above may be related to the inclination of the source, which may require a high inclination to explain it. The relationships between QPO frequency and QPO rms, hardness, total fractional rms and count rate have also been found in other transient sources, which can indicate that the origin of type-C QPOs is non-thermal.

Abstract Copyright: © 2021 National Astronomical Observatories

Journal keyword(s): X-ray binaries - black hole candidate - QPO - EXO 1846-031

Simbad objects: 9

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Number of rows : 9
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 MAXI J1535-571 XB* 15 35 19.73 -57 13 48.1           ~ 214 0
2 V* V381 Nor HXB 15 50 58.6637920704 -56 28 35.258385000           K3III 1254 0
3 SWIFT J1658.2-4242 X 16 58 12.64 -42 41 54.4           ~ 54 0
4 MAXI J1659-152 LXB 16 59 01.680 -15 15 28.73           ~ 274 0
5 V* V821 Ara LXB 17 02 49.3876391280 -48 47 23.087954544         15.322 ~ 2237 0
6 NAME XTE J17464-3213 LXB 17 46 15.59637 -32 14 00.8600           ~ 805 0
7 MAXI J1820+070 LXB 18 20 21.9423816480 +07 11 07.284859440           ~ 511 0
8 EXO 1846-031 LXB 18 49 17.1 -03 03 44           ~ 114 0
9 Granat 1915+105 HXB 19 15 11.55576 +10 56 44.9052           ~ 2810 0

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