A 59 M photometric period in the dwarf nova V 485 Centauri

Details A 59 M photometric period in the dwarf nova V 485 Centauri A 59 M photometric period in the dwarf nova V 485 Centauri

Jan 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993a%26a...267l..55a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 267, no. 2, p. L55-L58.

Astronomy and Astrophysics

Astrophysics

10

Cataclysmic Variables, Dwarf Novae, Line Spectra, Stellar Luminosity, Stellar Spectra, Astronomical Photometry, Orbital Mechanics, Stellar Magnitude, Stellar Orbits

Scientific paper

We present time-resolved V-band CCD photometry of the dwarf nova V485 Cen. It is found that the optical brightness during quiescence is modulated with a period of 59 m. Brightness variations with the same period may also be present during outburst. The observed spectrum in quiescence is fairly typical for a dwarf nova. However, we find that the He I line at 5876 A is much stronger relative to H-alpha than is the case in other cataclysmic variables. We discuss the nature of the 59 m period in terms of (i) the rotation period of the white dwarf; (ii) the orbital period of the system.

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