MAXI J1659-152: the shortest orbital period black-hole binary

E. Kuulkers, C. Kouveliotou, A. J. van der Horst, T. Belloni, Jérôme Chenevez, A. Ibarra, T. Munoz-Darias, A. Bazzano, M. Cadolle Bel, G. De Cesare, M. Diaz Trigo, E. Jourdain, P. Lubinski, L. Natalucci, J. -U. Ness, A. Parmar, A. M. T. Pollock, J. Rodriguez, J. -P. Roques, C. Sanchez-FernandezP. Ubertini, C. Winkler

Research output: Contribution to conferencePaperResearchpeer-review

116 Downloads (Pure)


Following the detection of a bright new X-ray source, MAXI J1659-152, a series of observations was triggered with almost all currently flying high-energy missions. We report here on XMM-Newton, INTEGRAL and RXTE observations during the early phase of the X-ray outburst of this transient black-hole candidate. We confirm the dipping nature in the X-ray light curves. We find that the dips recur on a period of 2.4139+/-0.0005 hrs, and interpret this as the orbital period of the system. It is thus the shortest period black-hole X-ray binary known to date. Using the various observables, we derive the properties of the source. The inclination of the accretion disk with respect to the line of sight is estimated to be 60-75 degrees. The companion star to the black hole is possibly a M5 dwarf star, with a mass and radius of about 0.15 M_sun and 0.23 R_sun, respectively. The system is rather compact (orbital separation is about 1.35 R_sun) and is located at a distance of roughly 7 kpc. In quiescence, MAXI J1659-152 is expected to be optically faint, about 28 mag in the V-band.
Original languageEnglish
Publication date2010
Number of pages5
Publication statusPublished - 2010
Event4th International MAXI Workshop: The First Year of MAXI - Tokyo, Japan
Duration: 30 Nov 20102 Dec 2010


Conference4th International MAXI Workshop


  • MAXI J1659-152
  • Black hole
  • XMM-Newton


Dive into the research topics of 'MAXI J1659-152: the shortest orbital period black-hole binary'. Together they form a unique fingerprint.

Cite this