Hydrodynamic simulations of the interaction between giant stars and planets

• DOI: 10.1093/mnras/stw331
• Publication Date: 2016-02-16T03:33:26Z
• Authors: Jan E. Staff; Orsola De Marco; Peter Wood; Pablo Galaviz; Jean-Claude Passy
• Keywords: Giant planet; Red giant; Jupiter mass

We present the results of hydrodynamic simulations interaction between a 10 Jupiter mass planet and red or asymptotic giant branch stars, both with zero-age main sequence 3.5 $M_\odot$. Dynamic in-spiral timescales are order few years decades for respectively. The planets will eventually be destroyed at separation from core giants smaller than resolution our simulations, either through evaporation tidal disruption. As in-spiral, stars' envelopes somewhat puffed up. Based on relatively long even considering fact that further should take place before destroyed, we predict merger would difficult to observe, only small, slow brightening. Very little is unbound in process. These conclusions may change if planet's orbit enhances star's pulsation modes. angular momentum transfer, also suspect this star-planet unable lead large scale outflows via rotation-mediated dynamo effect Nordhaus Blackman. Detectable pollution result lightest, lowest metallicity stars. furthermore find move outer stellar Mach-3 Mach-5, reaching Mach-1 towards end simulations. gravitational drag force decreases slows down sonic transition, as predicted analytically.