Astronomy and Astrophysics – Astronomy
Scientific paper
Jun 1989
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989mnras.238.1233o&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Vol. 238, NO. 3/JUN1, P.1233, 1989
Astronomy and Astrophysics
Astronomy
30
Scientific paper
We report an analysis of the published times of orbital minima of FO Aqr and those derived from two new long observations, confirming our earlier report (Osborne & Mukai 1988) that the orbital period of this system is 4.85 hr, the 1-day alias of the widely accepted 4.03 hr period. We also reconsider the white dwarf spin ephemeris using 171 individual pulse times spanning 7 yr. Th average period derivative dottedP over this interval is found to be + (3.4±0.4) × 10-11. We also find that the period derivative is changing with umlautP = -(2.5±0.8) × 10-11 yr-1. The individual pulse times show an orbital trend, which we interpret as the effect of the sideband pulsation; this enables us to locate the reprocessing site to be at inferior conjunction at orbital phase ˜0.8. Inferior conjunction of the secondary star occurs at phase zero, so we suggest that the accretion stream-disc interacfion region is the reprocessing site. Finally, we consider the spin period behaviour; the umlautP term implies either a change in the accretion rate or the presence of a third body.
Mukai Kazuhiko
Osborne Jeffrey
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