Radii and masses for beta Aurigae

Details Radii and masses for beta Aurigae Radii and masses for beta Aurigae

Nov 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...291..777n&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 291, no. 3, p. 777-785

Astronomy and Astrophysics

Astrophysics

23

A Stars, Eclipsing Binary Stars, Radii, Stellar Evolution, Stellar Mass, Stellar Models, Stellar Temperature, Chronology, Distance, Light Curve, Metallicity, Orbital Elements, Radial Velocity, Stellar Luminosity, Stellar Spectrophotometry

Scientific paper

Improved radii, masses and temperatures of the evolved early A-type binary beta Aurigae are determined through an analysis of the available light and radial velocity curves. A new spectroscopic determination of the luminosity ratio is used to constrain the ratio of the radii, k=rB/rA, which is indeterminate from the photometric light curves; we find k=0.95 +/- 0.015. The resulting physical parameters of the two stars, accurate to approximately 1%, are: masses: MA = 2.38 solar mass, MB = 2.31 solar mass; radii: RA = 2.77 solar radii, RB = 2.63 solar radii; log gA = 3.93, log gB = 3.96; effective temperatures: TA = 9350 K, TB = 9 200 K. Beta Aur has thus evolved into the upper part of the main sequence band. Our measured rotational velocities of 33 and 34 km/s for the two components correspond exactly to synchronous rotation in the circular orbit. Comparison with new stellar evolution models gives a very good fit at an age of 5.7 108 yr and indicates that beta Aur has a metal abundance that is close to solar or slightly below. Beta Aur is yet another system which is considerably younger than the Sun, but no richer in heavy elements. Recent optical interferometry of beta Aur yields an accurate distance to the system (24.8 +/- 0.8 pc) and allows an interesting cross-check of four different distance estimators. The results is a tighter constraint on the effective temperatures, rather than the masses and radii of the components.

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