Doppler-based planet surveys point to an increasing occurrence rate of giant planets with stellar mass .
Such surveys rely on evolved stars for a sample of intermediate-mass stars ( so-called retired A stars ) , which are more amenable to Doppler observations than their main-sequence progenitors .
However , it has been hypothesised that the masses of subgiant and low-luminosity red-giant stars targeted by these surveys — typically derived from a combination of spectroscopy and isochrone fitting — may be systematically overestimated .
Here , we test this hypothesis for the particular case of the exoplanet-host star HD 212771 using K2 asteroseismology .
The benchmark asteroseismic mass ( 1.45 ^ { +0.10 } _ { -0.09 } \ > \text { M } _ { \sun } ) is significantly higher than the value reported in the discovery paper ( 1.15 \pm 0.08 \ > \text { M } _ { \sun } ) , which has been used to inform the stellar mass-planet occurrence relation .
This result , therefore , does not lend support to the above hypothesis .
Implications for the fates of planetary systems are sensitively dependent on stellar mass .
Based on the derived asteroseismic mass , we predict the post-main-sequence evolution of the Jovian planet orbiting HD 212771 under the effects of tidal forces and stellar mass loss .