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Gamma Cephei - Rotation or planetary companion?
Walker, Gordon A. H.; Bohlender, David A.; Walker, Andrew R.; Irwin, Alan W.; Yang, Stephenson L. S.; Larson, Ana
AA(British Columbia, University, Vancouver, Canada), AB(British Columbia, University, Vancouver, Canada), AC(British Columbia, University, Vancouver, Canada), AD(Victoria, University, Canada), AE(Victoria, University, Canada), AF(Victoria, University, Canada)
Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 396, no. 2, Sept. 10, 1992, p. L91-L94. Research supported by NSERC. (ApJL Homepage)
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NASA/STI Keywords:
Binary Stars, Companion Stars, Radial Velocity, Stellar Rotation, Variable Stars, Chromosphere, Extrasolar Planets, G Stars, Rotational Spectra, Stellar Activity, Stellar Spectra
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In 1988 Gamma Cep was reported as a single-line, long-period spectroscopic binary with short-term periodic (P = 2.7 yr) residuals which might be caused by a Jupiter-mass companion. Eleven years of data now give a 2.52 yr (K = 27 m/s) period and an indeterminate spectroscopic binary period of not less than 30 yr. While binary motion induced by a Jupiter-mass companion could still explain the periodic residuals, Gamma Cep is almost certainly a velocity variable yellow giant because both the spetrum and (R - I) color indices are typical of luminosity class III. T eff and the trigonometric parallax give 5.8 solar radii independently.

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