Chromospherically active stars. X - Spectroscopy and photometry of HD 212280

Details Chromospherically active stars. X - Spectroscopy and photometry of HD 212280 Chromospherically active stars. X - Spectroscopy and photometry of HD 212280

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aj....105.2265f&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 105, no. 6, p. 2265-2275.

Astronomy and Astrophysics

Astronomy

7

Binary Stars, Chromosphere, Stellar Spectrophotometry, Stellar Mass, Stellar Orbits, Stellar Rotation, Variable Stars

Scientific paper

The system HD 212280 is a chromospherically active double lined spectroscopic binary with an orbital period of 45.284 days and an eccentricity of 0.50. The spectrum is composite with spectral types of G8 IV and F5-8 V for the components. An estimated inclination of 78 +/- 8 deg results in masses of 1.7 and 1.4 solar mass for the G subgiant and mid-F star, respectively. The distance to the system is estimated to be 112 pc. Photometric observations obtained between 1987 November and 1992 June reveal that HD 212280 is a newly identified variable star with a V amplitude of about 0.15 mag and a mean period of 29.46 days. Our V data were divided into 11 sets and in all but one case two spots were required to fit the data. Lifetimes of 650 days and a minimum of 1350 days have been determined for two of the four spots. The differential rotation coefficient of 0.05 is relatively small. The age of the system is about 1.9 X 10 exp 9 yrs. The G subgiant is rotating slower than pseudosynchronously while the F-type star is rotating faster.

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