Radial velocity studies of cataclysmic binaries. II - The ultrashort period dwarf nova T Leonis

Details Radial velocity studies of cataclysmic binaries. II - The ultrashort period dwarf nova T Leonis Radial velocity studies of cataclysmic binaries. II - The ultrashort period dwarf nova T Leonis

Jan 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...276..305s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 276, Jan. 1, 1984, p. 305-315.

Astronomy and Astrophysics

Astrophysics

74

Angular Velocity, Dwarf Novae, Stellar Rotation, Stellar Spectrophotometry, Binary Stars, H Alpha Line, Red Dwarf Stars, Spectral Energy Distribution, Stellar Evolution, Stellar Mass Accretion, Stellar Models, White Dwarf Stars

Scientific paper

Spectroscopic and photometric observations of T Leo which reveal the object to be an ultrashort period dwarf nova are presented. In particular, the analysis indicates that T Leo has an orbital period of 84.69936 (plus or minus 0.00068) minutes, which is the third shortest orbital period of any known cataclysmic variable and the shortest known for any U Gem type dwarf nova. These observations enable the placement of upper limits of 0.19 and 0.4 solar mass on the mass of the red dwarf and white dwarf, respectively. The overall energy distribution is relatively flat (f-sub-lambda approximately constant) which is consistent with a low mass accretion rate. The models of Williams and Ferguson (1982) suggest that the mass accretion rate is about 10 to the -10th solar mass/yr. A narrow peak component of H-alpha is observed, the phasing of which cannot be explained by the canonical hot spot model. Possible explanations for its origin are presented and discussed. It is predicted that future observations of T Leo may reveal the object to be a SU UMa type dwarf nova.

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