A spectroscopic study of the dwarf nova CN Orionis

Details A spectroscopic study of the dwarf nova CN Orionis A spectroscopic study of the dwarf nova CN Orionis

Aug 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...220...99b&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 220, no. 1-2, Aug. 1989, p. 99-104. Research supported by the Pontificia Unive

Astronomy and Astrophysics

Astrophysics

11

Cataclysmic Variables, Dwarf Novae, Stellar Spectra, Balmer Series, Radial Velocity, Stellar Spectrophotometry, Visible Spectrum

Scientific paper

Time-resolved spectroscopy of CN Ori in the quiescent state has been obtained in the wavelength range of 3500-7000 A with a resolution of 3 A. An improved orbital period of 0.163199 + or - 0.000007 d is proposed for the dwarf nova. The radial velocity amplitude K1 = 180 + or - 15 km/s derived suggests a rather high orbital inclination and moderate masses for both M1 and M2 of about 0.45 solar masses. The Balmer emission lines H-alpha, H-beta, H-gamma, and H-delta are shown to modulate with the orbital phase, amounting to 70-100 percent of the equivalent width. Unlike most other CVs, the maximal equivalent width and FWHM are found to coincide roughly with the photometric hump maximum.

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