Radial Velocity Study of UZ Serpentis

Details Radial Velocity Study of UZ Serpentis Radial Velocity Study of UZ Serpentis

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007rmxaa..43..291e&link_type=abstract

Revista Mexicana de Astronomía y Astrofísica Vol. 43, pp. 291-296 (2007) (http://www.astroscu.unam.mx/~rmaa/)

Astronomy and Astrophysics

Astronomy

Binaries: Close, Stars: Dwarf Novae, Stars: Individual (Uz Serpentis)

Scientific paper

We present high dispersion time-resolved spectroscopic observations of the dwarf nova UZ. We find the radial velocity curve of the accretion disc, surrounding the primary star, with a semi-amplitude K_1 = 98 km s^{-1}. There is no spectral evidence of the secondary star. The orbital period, estimated from its velocity curve is 0.17589 days, slightly larger than that found by Echevarría (1988), from photometric observations. New ephemerides of the object are discussed from both results. An analysis of the masses and inclination angle of the binary, using the diagnostic M_1-M_2 diagram, favors a set of values with M_1 = 0.90+/-0.1M_&sun;; M_2 = 0.40+/-0.1M_&sun;; and i = 50°+/-0.1, which is consistent with the ultraviolet observations and models and also with the optical photometry.

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