The close multiple system MU Orionis - Masses and the mass-luminosity relation

Details The close multiple system MU Orionis - Masses and the mass-luminosity relation The close multiple system MU Orionis - Masses and the mass-luminosity relation

Dec 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980pasp...92..785f&link_type=abstract

Astronomical Society of the Pacific, Publications, vol. 92, Dec. 1980-Jan. 1981, p. 785-789.

Astronomy and Astrophysics

Astronomy

15

Binary Stars, Orbital Elements, Stellar Luminosity, Stellar Mass, Stellar Spectrophotometry, Companion Stars, Dwarf Stars, F Stars, Mass Ratios, Radial Velocity, Stellar Magnitude

Scientific paper

The observations made of the secondary component B of the close visual binary mu Ori are described. The Reticon observations made at red wavelengths showed the secondary to be a double-lined spectroscopic binary with a period of 4.78 days and nearly identical components having minimum masses of 1.1 solar mass each. Previous estimates are corroborated by the large spectroscopic mass ratio of B to A and B. The discovery that B is a pair of late-F dwarfs solves the apparent mass-luminosity relation discrepancy noted in previous studies.

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