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The Crust Cooling Curve of the Neutron Star in MXB 1659-29

Published online by Cambridge University Press:  22 February 2018

Rudy Wijnands
Rudy Wijnands*
Affiliation:
School of Physics & Astronomy, U. of St Andrews, UK

Abstract

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We have monitored the quasi-persistent neutron-star X-ray transient MXB 1659-29 in quiescence using Chandra. The purpose of our observations was to monitor the quiescent behavior of the source after its last prolonged outburst episode and to study the cooling curve of the neutron star in this system. We discuss the results obtained and how they constrain the properties of the neutron star in MXB 1659-29.

Resumen

Resumen

Hemos monitoreado con Chandra MXB 1659-29, un sistema transitorio en rayos X, en su etapa de quietud. El propósito de nuestras observaciones es documentar el comportamiento de este objeto en su etapa de quietud, después de su último y extenso episodio explosivo y estudiar la curva de enfriamiento de la estrella de neutrones de este sistema. En este artículo discutimos nuestros resultados, así como las implicaciones que éstos tienen en la restricción de las propiedades de la estrella de neutrones del sistema MXB 1659-29.

Keywords

StarsIndividual (MXB 1659-29) — StarsNeutron — X-RaysStars
Type
The Contributed Papers
Information
International Astronomical Union Colloquium , Volume 194: Compact binaries in the galaxy and beyond , 2004 , pp. 7 - 9
Copyright
Copyright © Instituto de astronomia/revista mexicana de astronomίa y astrofίsica 2004

References

Gänsicke, B. T., Braje, T. M., & Romani, R. W. 2002, A&A, 386, 1001 Google Scholar
in 't Zand, J., Heise, J., Smith, M. J. S., Cocchi, M., Natalucci, L., & Celidonio, G. 1999, IAU Cire. 7138Google Scholar
Rutledge, R. E., Bildsten, L., Brown, E. F., Pavlov, G. G., Zavlin, V. E., Ushomirsky, G., 2002, ApJ, 580, 413 CrossRefGoogle Scholar
Wijnands, R., Miller, J. M., Markwardt, C., Lewin, W. H. G., & van der Klis, M. 2001, ApJ, 560, L159 CrossRefGoogle Scholar
Wijnands, R., Guainazzi, M., van der Klis, M., & Méndez, M., 2002, ApJ, 566, 1060 Google Scholar
Wijnands, R., Nowak, M., Miller, J. M., Homan, J., Wachter, S., & Lewin, W. H. G. 2003, ApJ, 594, 952 Google Scholar
Wijnands, R., Homan, J., Miller, J. M., & Lewin, W. H. G., 2004, ApJL in press (astro-ph/0310612)Google Scholar
Zavlin, V. E., Pavlov, G. G., & Shibanov, Y. A. 1996, A&A, 315, 141 Google Scholar