Preliminary results on the fundamental parameters of the eclipsing binary V398 Lacertae

Details Preliminary results on the fundamental parameters of the eclipsing binary V398 Lacertae Preliminary results on the fundamental parameters of the eclipsing binary V398 Lacertae

Jul 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007an....328..536c&link_type=abstract

Astronomische Nachrichten, Vol.328, Issue 6, p.536

Astronomy and Astrophysics

Astrophysics

1

Binaries: Eclipsing, Binaries: Spectroscopic, Stars: Fundamental Parameters, Stars: Variables, Stars: Individual: V398 Lacertae

Scientific paper

The Hipparcos Space Astrometry Mission photometric observations of V398 Lac, led to the discovery of its variability, allowing to classify it as an eclipsing binary with an orbital period of about 5.4 days. This prompted us to acquire high-resolution échelle spectra with the aim of performing accurate radial velocity measurements and to determine the main physical parameters of the system's components. We present, for the first time, a double-lined radial velocity curve and determine the orbital and physical parameters of the two components, that can be classified both as late B-type stars. In particular, we obtained an orbital inclination i ˜ 85°. With this value of the inclination, we deduced masses M_1=3.83±0.35 M&sun; and M_2=3.29±0.32 M&sun;, and radii R_1=4.89±0.18 R&sun; and R_2=2.45±0.11 R&sun; for the more massive and less massive components, respectively. Both components are well inside their own Roche lobes. The mass ratio is {M_2}/{M_1}˜ 0.86. We derived also the projected rotational velocities as v_1 sin i=79±2 km s-1 and v_2 sin i=19±2 km s-1. Our measurements indicate that the rotation of the primary star is essentially pseudo-synchronized with the orbital velocity at the periastron, while the secondary appears to rotate very slowly and has not yet attained synchronization.
Based on observations collected at Catania Astrophysical Observatory, Italy.

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