Orbital Period and Spectral Behavior of LS Peg (S193)

Details Orbital Period and Spectral Behavior of LS Peg (S193) Orbital Period and Spectral Behavior of LS Peg (S193)

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aas...19110913t&link_type=abstract

American Astronomical Society, 191st AAS Meeting, #109.13; Bulletin of the American Astronomical Society, Vol. 29, p.1387

Astronomy and Astrophysics

Astronomy

Scientific paper

We present time-resolved spectroscopy of the bright (V ~ 13.0 -- Szkody et al. 1997, AJ, 113, 2276) cataclysmic variable LS Peg (= S193), which has no formally published period. Our data are from five observing runs spanning July 1996 to June 1997, using both the McGraw-Hill 1.3 m and the Hiltner 2.4 m telescopes at the Michigan-Dartmouth-MIT Observatory. The Balmer lines exhibit broad Doppler-shifted wings (about 2000 km s(-1) at the edges) while the He 1 lines show phase-dependent absorption features similar to SW Sex stars, in addition to emission through most of the phase. The C 3/N 3 blend does not show any phase-dependence in velocity or intensity. Because of the confusion in the line cores, we determined the radial velocities of Hα by measuring by hand the bisector of the zero-intensity points of the broad emission wings. From the velocities measured in this way, we unambiguously determine an orbital period of 0.174774 +/- 0.000003 d (= 4.1946 h).

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