The spectroscopic binary eta Andromedae: Determination of the orbit by optical interferometry

Details The spectroscopic binary eta Andromedae: Determination of the orbit by optical interferometry The spectroscopic binary eta Andromedae: Determination of the orbit by optical interferometry

Dec 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aj....106.2486h&link_type=abstract

The Astronomical Journal (ISSN 0004-6256), vol. 106, no. 6, p. 2486-2492

Astronomy and Astrophysics

Astronomy

28

Astronomical Interferometry, Astronomical Spectroscopy, Binary Stars, Orbital Elements, Orbital Mechanics, Stellar Orbits, Computerized Simulation, Estimates, Monte Carlo Method

Scientific paper

We have determined the following orbital elements of the double-lined spectroscopic binary eta Andromedae (combined spectral class G8 IIIb) using measurments with the Mark III long baseline optical interferometer on Mt. Wilson: Period P = 115.72 +/- 0.02d, major axis a = 10.37 +/- 0.03 milliarcseonds, eccentricity e = 0.006 +/- 0.002, epoch of periastron T = JD 2448013 +/- 2, inclination i = 30.5 deg +/- 0.4 deg, argument of ascending node omega = 69.4 deg +/- 0.6 deg, and argument of periastron omega = 215 deg +/- 7 deg. The magnitude differences of the two components measured at lambda lambda 800 nm, 550 nm, and 500 nm are 0.50 mag +/- 0.06 mag, 0.55 mag +/- 0.08,ag, and 0.56 mag +/- 0.09 mag, respectively. Using orbital elements from spectroscopy by Gordon (1946) we derive component masses of (2.59 +/- 0.30) solar mass and (2.34 +/- 0.22) solar mass, and a distance of (76 +/- 2)pc. Monte-Carlo simulations have been performed to estimate parameter uncertainties. We discuss the evolutionary state of eta Andromedae.

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