A New Dynamical Model for the Black Hole Binary Lmc X-1

DSpace/Manakin Repository

A New Dynamical Model for the Black Hole Binary Lmc X-1

Citable link to this page


Title: A New Dynamical Model for the Black Hole Binary Lmc X-1
Author: Orosz, Jerome A.; Steeghs, Danny; McClintock, Jeffrey E.; Torres, Manuel A. P.; Bochkov, Ivan; Gou, Lijun; Narayan, Ramesh; Blaschak, Michael; Levine, Alan M.; Remillard, Ronald A.; Bailyn, Charles D.; Dwyer, Morgan M.; Buxton, Michelle

Note: Order does not necessarily reflect citation order of authors.

Citation: Orosz, Jerome A., Danny Steeghs, Jeffrey E. McClintock, Manuel A. P. Torres, Ivan Bochkov, Lijun Gou, Ramesh Narayan, et al. 2009. “A New Dynamical Model for the Black Hole Binary Lmc X-1.” The Astrophysical Journal 697 (1) (May 4): 573–591. doi:10.1088/0004-637x/697/1/573.
Full Text & Related Files:
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 nearinfrared 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 AV = 2.28 ± 0.06, which is much larger than previously assumed. For the secondary star, we measure a radius of R2 = 17.0±0.8 R⊙ and a projected rotational velocity of Vrot sin i = 129.9±2.2 km s −1 . Using these measured properties to constrain the dynamical model, we find an inclination of i = 36.38±1.92◦ , a secondary star mass of M2 = 31.79±3.48 M⊙, and a black hole mass of 10.91 ± 1.41 M⊙. 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⊙ that is 5 Myr past the zero-age main sequence. The star nearly fills its Roche lobe (≈ 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.
Published Version: 10.1088/0004-637X/697/1/573
Other Sources: https://arxiv.org/abs/0810.3447
Terms of Use: This article is made available under the terms and conditions applicable to Other Posted Material, as set forth at http://nrs.harvard.edu/urn-3:HUL.InstRepos:dash.current.terms-of-use#LAA
Citable link to this page: http://nrs.harvard.edu/urn-3:HUL.InstRepos:27804435
Downloads of this work:

Show full Dublin Core record

This item appears in the following Collection(s)


Search DASH

Advanced Search