The orbital period of the polar MR Serpentis

Details The orbital period of the polar MR Serpentis The orbital period of the polar MR Serpentis

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...244..373s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 244, no. 2, April 1991, p. 373-377.

Astronomy and Astrophysics

Astronomy

18

Astronomical Spectroscopy, Binary Stars, Cataclysmic Variables, Light Curve, White Dwarf Stars, X Ray Astronomy, Ephemeris Time, Stellar Mass Accretion, Stellar Rotation

Scientific paper

The stability of spectroscopic features found in the AM Herculis binary MR Ser was used to derive a spectroscopic ephemeris of the narrow emission-line component which seems to originate from the secondary star. Published X-ray light curves displayed nonrepetitive features contrary to the 'standard' picture of these systems. These were explained in terms of multiple emission regions with variable accretion rates. The new orbital period was used to correctly phase these X-ray data. The resulting light curves display a relatively simple and stable pattern. The X-rays most probably originate from a single accretion spot on the white dwarf which is located within about 20 deg of the binary central meridian. From optical and X-ray photometry, there is no evidence for asynchronous rotation of the white dwarf over a 7-year base.

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