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We use precise radial velocity measurements and photometric data to derivethe frequency spacing of the p-mode oscillation spectrum of the planet-hostingstar Beta Gem. This spacing along with the interferometric radius for this staris used to derive an accurate stellar mass. A long time series of over 60 hoursof precise stellar radial velocity measurements of Beta Gem were taken with aniodine absorption cell and the echelle spectrograph mounted on the 2m AlfredJensch Telescope. Complementary photometric data for this star were also takenwith the MOST microsatellite spanning 3.6 d. A Fourier analysis of the radialvelocity data reveals the presence of up to 17 significant pulsation modes inthe frequency interval 10-250 micro-Hz. Most of these fall on a grid ofequally-spaced frequencies having a separation of 7.14 +/- 0.12 micro-Hz. Ananalysis of 3.6 days of high precision photometry taken with the MOST spacetelescope shows the presence of up to 16 modes, six of which are consistentwith modes found in the spectral (radial velocity) data. This frequency spacingis consistent with high overtone radial pulsations; however, until thepulsation modes are identified we cannot be sure if some of these are nonradialmodes or even mixed modes. The radial velocity frequency spacing along withangular diameter measurements of Beta Gem via interferometry results in astellar mass of M = 1.91 +/- 0.09 solar masses. This value confirms theintermediate mass of the star determined using stellar evolutionary tracks.Beta Gem is confirmed to be an intermediate mass star. Stellar pulsations ingiant stars along with interferometric radius measurements can provide accuratedeterminations of the stellar mass of planet hosting giant stars. These canalso be used to calibrate stellar evolutionary tracks.

The Mass of the Planet-hosting Giant Star Beta Geminorum Determined from its p-mode Oscillation Spectrum