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Apparent orbit of the spectroscopic binary Beta ARIETIS with the time Mark III Stellar Interferometer
Pan, X. P.; Shao, M.; Colavita, M. M.; Mozurkewich, D.; Simon, R. S.; Johnston, K. J.
AA(California Institute of Technology, Pasadena), AB(JPL, Pasadena, CA), AC(JPL, Pasadena, CA), AD(U.S. Navy, E. O. Hulburt Center for Space Research, Washington, DC), AE(U.S. Navy, E. O. Hulburt Center for Space Research, Washington, DC)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 356, June 20, 1990, p. 641-645. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Binary Stars, Interferometry, Orbital Elements, Stellar Luminosity, Stellar Mass, Bessel Functions, Mass To Light Ratios, Spectrograms
Bibliographic Code:


The spectroscopic binary Beta Ari has been directly resolved with the Mark III Stellar Interferometer. Observations in 1988 were analyzed to determine the visual orbit of the system with the following results: eccentricity = 0.903 +/- 0.012, semimajor axis = 0.0361 +/- 0.0003 arcsec, inclination = 44.7 +/- 1.3 deg, longitude of periastron = 209.1 deg +/- 1.2 deg, position angle of ascending node = 79.1 deg +/- 0.8 deg. The measured magnitude difference between two components, Delta m = 2.63 +/- 0.22 at 800 nm, yields individual visual magnitudes of m(v1) = 2.70 +/- 0.02 and m(v2) = 5.80 +/- 0.20. Combined with data from spectroscopic observations, masses M1 = (2.34 +/- 0.10) solar masses, M2 = (1.34 +/- 0.07) solar masses, and geometrical parallax pi = 0.053 arcsec +/- 0.002 arcsec are derived. These results demonstrate that both components of Beta Ari agree well with the empirical mass-luminosity relation.

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