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A new dynamical model for the black hole binary LMC X-1
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Orosz, Jerome A., Steeghs, D., McClintock, Jeffrey E., Torres, M. A. P., Bochkov, Ivan, Gou, Lijun, Narayan, R., Blaschak, Michael, Levine, Alan M., Remillard, R., Bailyn, Charles D., Dwyer, Morgan M. and Buxton, Michelle (2009) A new dynamical model for the black hole binary LMC X-1. Astrophysical Journal, Vol.697 (No.1). pp. 573-591. doi:10.1088/0004-637X/697/1/573 ISSN 0004-637X.
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WRAP_Steeghs_LMC X-10810.3447v2.pdf - Accepted Version Download (961Kb) | Preview |
Official URL: http://dx.doi.org/10.1088/0004-637X/697/1/573
Abstract
We present a dynamical model of the high mass X-ray binary LMC X-1 based on high-resolution optical spectroscopy and extensive optical and near-infrared photometry. From our new optical data we find an orbital period of P = 3.90917 +/- 0.00005 days. We present a refined analysis of the All Sky Monitor data from RXTE and find an X-ray period of P = 3.9094 +/- 0.0008 days, which is consistent with the optical period. A simple model of Thomson scattering in the stellar wind can account for the modulation seen in the X-ray light curves. The V-K color of the star (1.17 +/- 0.05) implies A(V) = 2.28 +/- 0.06, which is much larger than previously assumed. For the secondary star, we measure a radius of R-2 = 17.0 +/- 0.8 R-circle dot and a projected rotational velocity of V-rot sin i = 129.9 +/- 2.2 km s(-1). Using these measured properties to constrain the dynamical model, we find an inclination of i = 36 degrees.38 +/- 1 degrees.92, a secondary star mass of M-2 = 31.79 +/- 3.48 M-circle dot, and a black hole mass of 10.91 +/- 1.41 M-circle dot. The present location of the secondary star in a temperature-luminosity diagram is consistent with that of a star with an initial mass of 35 M-circle dot that is 5 Myr past the zero-age main sequence. The star nearly fills its Roche lobe (approximate to 90% or more), and owing to the rapid change in radius with time in its present evolutionary state, it will encounter its Roche lobe and begin rapid and possibly unstable mass transfer on a timescale of a few hundred thousand years.
Item Type: | Journal Article | ||||
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Subjects: | Q Science > QB Astronomy | ||||
Divisions: | Faculty of Science, Engineering and Medicine > Science > Physics | ||||
Library of Congress Subject Headings (LCSH): | X-ray binaries, Black holes (Astronomy) | ||||
Journal or Publication Title: | Astrophysical Journal | ||||
Publisher: | IOP Publishing | ||||
ISSN: | 0004-637X | ||||
Official Date: | 20 May 2009 | ||||
Dates: |
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Volume: | Vol.697 | ||||
Number: | No.1 | ||||
Number of Pages: | 19 | ||||
Page Range: | pp. 573-591 | ||||
DOI: | 10.1088/0004-637X/697/1/573 | ||||
Status: | Peer Reviewed | ||||
Publication Status: | Published | ||||
Access rights to Published version: | Restricted or Subscription Access | ||||
Date of first compliant deposit: | 13 December 2015 | ||||
Date of first compliant Open Access: | 13 December 2015 | ||||
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Data sourced from Thomson Reuters' Web of Knowledge
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