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The Origin and Evolution of the Black Hole Binary XTE J1118+480

Published online by Cambridge University Press:  23 April 2012

Jonay I. González Hernández ,
Rafael Rebolo  and
Jorge Casares
Jonay I. González Hernández
Affiliation:
Instituto de Astrofísica de Canarias, Vía Láctea, s/n, E-38205 La Laguna, Tenerife, Spain email: jonay@iac.es Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
Rafael Rebolo
Affiliation:
Instituto de Astrofísica de Canarias, Vía Láctea, s/n, E-38205 La Laguna, Tenerife, Spain email: jonay@iac.es Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
Jorge Casares
Affiliation:
Instituto de Astrofísica de Canarias, Vía Láctea, s/n, E-38205 La Laguna, Tenerife, Spain email: jonay@iac.es Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
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Abstract

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Black hole X-ray binaries with large mass ratios and short orbital periods are expected to change their orbital period due to magnetic breaking, mass loss, gravitational radiation, or mass evaporation of the black hole in alternative descriptions of gravity, like in braneworld gravity scenarios.

The black hole X-ray binary XTE J1118+480, consisting of a late-type secondary star orbiting a ~ 8 M⊙ black hole in a 4.1-hr period, offers a unique opportunity to test these models. New spectroscopic data allow us to determine the time of the inferior conjunction of the secondary star at different epochs. Observations over a 10 year span will provide constraints on the rate of any orbital period change.

We present here a preliminary radial velocity curve obtained with the 10.4m GTC telescope equipped with OSIRIS medium-resolution spectrograph, as part of an ongoing long-term program to study the orbital period evolution in this binary.

Keywords

black hole physicstechniques: radial velocitiesstars: individual (XTE J1118+480)X-rays: binariessupernovae: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S282: From Interacting Binaries to Exoplanets: Essential Modeling Tools , July 2011 , pp. 476 - 477
Copyright
Copyright © International Astronomical Union 2012

References

Casares, J., Bonifacio, P., González Hernández, J. I., et al. , 2007, A&A, 470, 1033Google Scholar
Casares, J., González Hernández, J. I., Israelian, G., & Rebolo, R. 2010, MNRAS, 401, 2517Google Scholar
González Hernández, J. I., Rebolo, R., Israelian, G., et al. , 2004, ApJ, 609, 988Google Scholar
González Hernández, J. I., Rebolo, R., Israelian, G., et al. , 2005, ApJ, 630, 495Google Scholar
González Hernández, J. I., Rebolo, R., Israelian, G. et al. , 2006, ApJ, 644, L49Google Scholar
González Hernández, J. I., Rebolo, R., & Israelian, G. 2008a, A&A, 478, 203Google Scholar
González Hernández, J. I., Rebolo, R., Israelian, G., et al. , 2008b, ApJ, 679, 732Google Scholar
González Hernández, J. I. & Casares, J. 2010, A&A, 516, A58Google Scholar
González Hernández, J. I., Casares, J., Rebolo, R., et al. , 2011, arXiv:1106.4278Google Scholar
Gualandris, A., Colpi, M., Portegies Zwart, S., & Possenti, A. 2005, ApJ, 618, 845Google Scholar
Johannsen, T. 2009, A&A, 507, 617Google Scholar
Psaltis, D. 2007, Phys. Rev. Lett., 98, 181101Google Scholar
Mirabel, I. F., Dhawan, V., Mignani, R. P., et al. , 2001, Nature, 413, 139Google Scholar