The Magnetic Circuit

Gray, Andrew

doi:10.1038/057385a0

Cited by 1 publication

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“…A rotating magnetic region with a convective blueshift which somehow produces no photometric signature could be considered, but the more magnetically active Sun shows no spurious radial velocity variations as large as one-tenth the amplitude we observe on ρ CrB (see McMillan et al 1993). One might postulate a non-radial pulsation which does not produce any disk-integrated photometric modulation, as Gray (1997) has suggested to explain the 4.2-day periodicity observed in the radial velocity of 51 Pegasi (Mayor & Queloz 1995). However, the 40 day period of the radial-velocity variations in ρ CrB is extremely long compared to the dynamical timescales characterizing acoustic-gravity modes in Sun-like stars (roughly 1 hour).…”

Section: Discussionmentioning

confidence: 94%

A Planet Orbiting the Star ρ Coronae Borealis

Noyes

Korzennik

Krockenberger

et al. 1997

The Astrophysical Journal

160

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We report the discovery of near-sinusoidal radial velocity variations of the G0V star ρ CrB, with period 39.6 days and amplitude 67 m s −1 . These variations are consistent with the existence of an orbital companion in a circular orbit. Adopting a mass of 1.0 M ⊙ for the primary, the companion has minimum mass about 1.1 Jupiter masses, and orbital radius about 0.23 AU. Such an orbital radius is too large for tidal circularization of an initially eccentric orbit during the lifetime of the star, and hence we suggest that the low eccentricity is primordial, as would be expected for a planet formed in a dissipative circumstellar disk.

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Section: Discussionmentioning

confidence: 94%