Photometric and spectroscopic observations of the eclipsing nova-like variable PG 1030 + 590 (DW Ursae Majoris)

Details Photometric and spectroscopic observations of the eclipsing nova-like variable PG 1030 + 590 (DW Ursae Majoris) Photometric and spectroscopic observations of the eclipsing nova-like variable PG 1030 + 590 (DW Ursae Majoris)

Apr 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988apj...327..248s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 327, April 1, 1988, p. 248-264.

Astronomy and Astrophysics

Astrophysics

73

Eclipsing Binary Stars, Novae, Stellar Spectra, Stellar Spectrophotometry, Variable Stars, White Dwarf Stars, Cataclysmic Variables, Emission Spectra, Line Spectra, Radial Velocity, Roche Limit, Stellar Mass

Scientific paper

The authors present high-speed photometric and time-resolved spectroscopic observations of the nova-like variable PG 1030+590 with eclipses which recur with a period of 0.13660653 (5) days. There is no evidence for a pronounced hump prior to eclipse. The spectrum exhibits strong, high-excitation lines in the optical. These high-excitation lines are greatly diminished in intensity during eclipse. They arise in a relatively hot, localized region. Radial velocity measurements show that the K-velocities of the Hα and Hβ emission lines are roughly 200 km s-1. Such a high amplitude requires a white dwarf mass below 0.2 M_sun; regardless of the orbital inclination or the evolutionary state of the secondary star. The K-velocity of the He II λ4686 line is about 110 km s-1. If one assumes that Kwd is the same as the K-velocity of the He II λ4686 line and assumes further that the secondary star is near the main sequence, then M2 ≈ 0.29 M_sun;, M1 ≈ 0.9 M_sun;, and i ≈ 80°.

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