Orbital period change of the low-mass X-ray binary EXO 0748-676

Details Orbital period change of the low-mass X-ray binary EXO 0748-676 Orbital period change of the low-mass X-ray binary EXO 0748-676

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992pasj...44..633a&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 44, no. 6, p. 633-640.

Astronomy and Astrophysics

Astronomy

10

Orbital Elements, Stellar Orbits, X Ray Binaries, X Ray Sources, Neutron Stars, Stellar Mass, Transient Response

Scientific paper

The transient low-mass X-ray binary, EXO 0748-676, discovered with EXOSAT, is known to exhibit eclipses of a 492-s duration with a 3.82-hr period, intensity dips at pre-eclipse phases and type-I X-ray bursts. We observed this source with Ginga in 1989 March, 1990 December, 1991 January, and 1991 August and determined nine eclipse center times. Combining these eclipse center times with the previous result of the EXOSAT observations, we find that the orbital period of this source is not decaying monotonically, contrary to the previously reported suggestion. Instead, it shows a more complex behavior. A quadratic fit to the eclipse data yields a positive rate of change in orbital period with an approximate rate of 0.9 x 10 exp 7/yr, although the EXOSAT observations made in 1985 do not fit this trend. A sinusoidal function gives a better fit to the observed orbital period changes with a period of about 12 yr and an amplitude of about 44 lt-s, although the period is much longer than the observation interval of about 6.5 yr. Possible mechanisms for the orbital period change are discussed.

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