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The K-correction for LMXBs: an application to X1822-371 and GX339-4

Published online by Cambridge University Press:  01 August 2006

T. Muñoz-Darias ,
J. Casares  and
I. G. Martínez-Pais
T. Muñoz-Darias
Affiliation:
Instituto de Astrofísica de Canarias, 38200, La Laguna, Tenerife, Spain
J. Casares
Affiliation:
Instituto de Astrofísica de Canarias, 38200, La Laguna, Tenerife, Spain
I. G. Martínez-Pais
Affiliation:
Instituto de Astrofísica de Canarias, 38200, La Laguna, Tenerife, Spain Departamento de Astrofísica, Universidad de La Laguna, 38206 La Laguna, Tenerife, Spain
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Abstract

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We model the K-correction for emission lines formed on the irradiated face of companion stars in compact binaries. We compute this K-correction in a general approach as function of the mass ratio and the disc flaring angle. Our results, combined with the detection of high excitation emission lines arising from the donor star, can be used to set constraints to the masses of neutron stars and black holes in persistent Low Mass X-ray Binaries (LMXBs).

The application of our model to X1822-371 (Muñoz-Darias, Casares & Martínez-Pais 2005) lends strong support to the presence of a massive neutron star in this LMXB (i.e. MNS > 1.6M⊙). Here, we also present the K-correction for the Black Hole binary GX339-4, where we obtain a solid lower limit to the black hole mass of MBH > 5.8M⊙.

Keywords

Accretionaccretion disks – binaries: close – X-rays: stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S238: Black Holes from Stars to Galaxies – Across the Range of Masses , August 2006 , pp. 413 - 414
Copyright
Copyright © International Astronomical Union 2007

References

Casares, J., Steeghs, D., Hynes, R. I., Charles, P. A. & O'Brien, K. 2003, ApJ, 590, 1041CrossRefGoogle Scholar
Casares, J., Cornelisse, R., Steeghs, D., Charles, P. A., Hynes, R. I., O'Brien, K. & Strohmayer, T. E. 2006, MNRAS, 373, 1235CrossRefGoogle Scholar
Hynes, R. I., Steeghs, D., Casares, J., Charles, P. A. & O'Brien, K. 2003, ApJ, 583, L95CrossRefGoogle Scholar
Heinz, S. & Nowak, M. A. 2001, MNRAS, 320, 249Google Scholar
Hellier, C. & Mason, K. O. 1989, MNRAS, 239, 715Google Scholar
Jonker, P. G. & van der Klis, M. 2001, ApJ, 553, L43Google Scholar
Munoz-Darias, T., Casares, J. & Martinez-Pais, I. G. 2005, ApJ, 635, 502Google Scholar
Samimi, J. et al. 1979, Nature, 278, 434Google Scholar
Steeghs, D. & Casares, J. 2002, ApJ, 568, 273CrossRefGoogle Scholar