HR 7551 - A new supergiant eclipsing binary

Details HR 7551 - A new supergiant eclipsing binary HR 7551 - A new supergiant eclipsing binary

Oct 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981pasp...93..608m&link_type=abstract

Astronomical Society of the Pacific, Publications, vol. 93, Oct.-Nov. 1981, p. 608-613.

Astronomy and Astrophysics

Astronomy

6

Eclipsing Binary Stars, Stellar Motions, Stellar Spectrophotometry, Supergiant Stars, Variable Stars, Apsides, Eccentric Orbits, Line Spectra, Mass Transfer, Periodic Variations, Radial Velocity, Stellar Mass Accretion, Stellar Mass Ejection, Stellar Rotation, Ubv Spectra

Scientific paper

A photometric and spectroscopic investigation of the spectroscopic binary HR 7551, which belongs to spectral type B0.5 Ib and thus has an evolved primary component, is presented. Spectroscopic data taken from the measurements of Plaskett and Pearce (1931) made in the 1920s and spectrograms obtained with the 2-m telescope at Ondrejov from 1978-1980 are used to determine radial velocities which indicate a binary period of 13.374 days, and spectroscopic elements indicating a strongly eccentric orbit and the possible rotation of the line of apsides in the 50 year interval. UVB photometry has confirmed the existence of primary and secondary eclipses, with times in good agreement with the spectroscopy. The presence of secondary lines, which appears probable, would indicate a value of M1 sin i-cubed of 26.9 solar masses, M2 sin i-cubed of 13.5 solar masses, and a sin i of 56.6 x 10 to the 6th km, with an inclination close to 90 deg. The secondary thus appears to be of the same spectral type as the primary, and the system does not appear to be affected yet by mass transfer.

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