Orbital evolution of the Low Mass X-ray Binaries 4U 1822-37, XTE J1710-281 and MXB 1658-298

Details Orbital evolution of the Low Mass X-ray Binaries 4U 1822-37, XTE J1710-281 and MXB 1658-298 Orbital evolution of the Low Mass X-ray Binaries 4U 1822-37, XTE J1710-281 and MXB 1658-298

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010fym..confp..26p&link_type=abstract

"The First Year of MAXI: Monitoring Variable X-ray Sources", Poster Presentations, 4th International MAXI Workshop held November

Physics

Scientific paper

The orbits of X-ray binaries evolve due to redistribution of the angular momentum due to different types of interactions between the components of the binary system and/or mass loss through wind. Accurate measurement of the rate of change of the orbital period is therefore, necessary in order to understand the evolution of compact binary systems. Using the eclipse timing technique, we have derived/updated the estimates of orbital periods and period derivatives in three eclipsing low mass X-ray binaries, 4U 1822-37, XTE J1710-281 and MXB 1658-298. In view of our results, we discuss several physical mechanisms that could be responsible for the observed orbital evolution in these LMXBs.

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