Permanent superhumps in V603 Aquilae

Details Permanent superhumps in V603 Aquilae Permanent superhumps in V603 Aquilae

Aug 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991pasp..103..735p&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 103, Aug. 1991, p. 735-747.

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32

Accretion Disks, Dwarf Novae, Magnetic Stars, White Dwarf Stars, Astronomical Photometry, Cataclysmic Variables, Stellar Models

Scientific paper

The results of an intensive program of photometry of the old nova V603 Aquilae (= Nova Aquilae 1918) are reported. In four separate observing runs of high-speed photometry, totaling 15 nights, no evidence is found for previously reported signals with periods of 61.4 and 15.6 minutes, or any other coherent signal with a period in the range 20 seconds to 3 hours. This makes it very unlikely that the star contains a strongly magnetic white dwarf, as has been suggested. The light curves do consistently show a slow wave with a period of about 3.5 hours, about 5 percent longer than the accepted orbital period. This period is stable on time scales of at least a few weeks. Published observations are too scarce to determine a long-term ephemeris, but the period increased between 1981 and 1990 at a mean rate of about 5 seconds/year. Several models for the origin of the periodicity are discussed. There is some resemblance to the well-known 'superhumps' of the SU Ursae Majoris class of dwarf novae. This suggests that the star may be stuck in a more or less permanent state of high mass transfer, with the photometric period arising from the precession of an eccentric accretion disk.

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