IHEP OpenIR
Measuring the black hole masses in accreting X-ray binaries by detecting the Doppler orbital motion of their accretion disc wind absorption lines
Zhang SN(张双南); 廖金元;Zhang, SN; Liao, JY; Yao, YS
2012
Source PublicationMONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume421Issue:4Pages:3550-3556
AbstractSo far essentially all black hole masses in X-ray binaries have been obtained by observing the companion stars velocity and light curves as functions of the orbital phase. However, a major uncertainty is the estimate of the orbital inclination angle of an X-ray binary. Here we suggest to measure the black hole mass in an X-ray binary by measuring directly the black holes orbital motion, thus obtaining the companion-to-black hole mass ratio. In this method we assume that accretion disc wind moves with the black hole and thus the black holes orbital motion can be obtained from the Doppler velocity of the absorption lines produced in the accretion disc wind. We validate this method by analysing the Chandra/High Energy Transmission Grating observations of GRO J1655-40, in which the black hole orbital motion (KBH= 90.8 +/- 11.3 km s-1) inferred from the Doppler velocity of disc wind absorption lines is consistent with the prediction from its previously measured system parameters. We thus estimate its black hole mass () and then its system inclination (), where MBH does not depend on i. Additional observations of this source covering more orbital phases can improve estimates on its system parameters substantially. We then apply the method to the black hole X-ray binary LMC X-3 observed with Cosmic Origins Spectrograph (COS) on board the Hubble Space Telescope (HST) near orbital phase 0.75. We find that the disc wind absorption lines of C iv doublet were shifted to similar to 50 km s-1, which yields a companion-to-black hole mass ratio of 0.6 for an assumed disc wind velocity of -400 km s-1. Additional observations covering other orbital phases (0.25 in particular) are crucial to ease this assumption and then to directly constrain the mass ratio. This method in principle can also be applied to any accreting compact objects with detectable accretion disc wind absorption line features.
Keywordaccretion, accretion discs black hole physics stars: luminosity function, mass function X-rays: binaries X-rays: individual: GRO J1655-40 X-rays: individual: LMC X-3
Subject AreaAstronomy & Astrophysics
DOI10.1111/j.1365-2966.2012.20579.x
Indexed BySCI ; INSPIREHEP ; ADS
WOS IDWOS:000302620700070
ADS Bibcode2012MNRAS.421.3550Z
ADS URLhttps://ui.adsabs.harvard.edu/abs/2012MNRAS.421.3550Z
ADS CITATIONShttps://ui.adsabs.harvard.edu/abs/2012MNRAS.421.3550Z/citations
inspireid1085052
inspireURLhttps://inspirehep.net/literature/1085052
Citation statistics
Cited Times:5 [INSPIRE]
Cited Times:9 [ADS]
Document Type期刊论文
Identifierhttp://ir.ihep.ac.cn/handle/311005/224234
Collection中国科学院高能物理研究所
Recommended Citation
GB/T 7714
Zhang SN,廖金元;Zhang, SN,Liao, JY,et al. Measuring the black hole masses in accreting X-ray binaries by detecting the Doppler orbital motion of their accretion disc wind absorption lines[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,2012,421(4):3550-3556.
APA 张双南,廖金元;Zhang, SN,Liao, JY,&Yao, YS.(2012).Measuring the black hole masses in accreting X-ray binaries by detecting the Doppler orbital motion of their accretion disc wind absorption lines.MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY,421(4),3550-3556.
MLA 张双南,et al."Measuring the black hole masses in accreting X-ray binaries by detecting the Doppler orbital motion of their accretion disc wind absorption lines".MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 421.4(2012):3550-3556.
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