Other
Scientific paper
May 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...268..790k&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 268, May 15, 1983, p. 790-799.
Other
51
Celestial Mechanics, Eclipsing Binary Stars, Orbit Decay, Orbital Elements, Pulsars, X Ray Sources, Angular Momentum, Neutron Stars, Sas-3, Stellar Mass Ejection, Stellar Rotation, Stellar Winds, Tides, Time Measurement
Scientific paper
Two new times of mid-X-ray eclipse for Cen X-3 are presented on the basis of pulse arrival time analyses of pointed observations with SAS 3. When combined with all other published eclipse times based on Doppler delay measurements, the results show that the 2.1d binary period is decreasing at an average rate of 1.8 x 10 to the -6th/yr. The decrease, however, is seen as having significant fluctuations about a smooth, linear decrease. The changes observed in the orbital period can be accounted for by mass loss from the system through the L2 point, although the rates required are implausibly high. It is also shown that the long-term overall orbital decay can readily be interpreted as the result of torques exerted by the tidally distorted companion star (Krzeminski's star) on the orbiting neutron star. It is noted that the inferred asynchronism between the orbital frequency and the rotation frequency of the companion star may be maintained by mass and angular momentum loss in a stellar wind or by a tidal instability related to the Darwin effect. However, this would not provide a natural explanation for any short-term deviations from a constant rate of orbital decay.
Clark George W.
Kelley Richard L.
Petro Larry D.
Rappaport Saul
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