The Three-dimensional Flow Field around Planets on Eccentric Orbits

We investigate the properties of hydrodynamic flow around eccentric protoplanets and compare them with often assumed case a circular orbit. To this end, we perform set 3D simulations small eccentricities ($e\leq 0.1$). adopt an isothermal equation state concentrate resolution on protoplanet to flows down scale protoplanet's circumplanetary disk (CPD). find enhanced prograde rotation exterior CPD for low planet masses undergoing subsonic motion. If eccentricity is made large enough develop bow shock, trend reverses becomes increasingly retrograde. The instantaneous field dramatically altered compared orbits. Whereas latter exhibit generic pattern polar inflow midplane outflow, geometry depends orbital phase in case. For even modest tested here, dominant source can come from instead poles. that amount outflow increases higher $e$ lower masses, thereby recycling more gas through planet's Bondi radius. These increased fluxes may increase pebble accretion rate planets up several times orbit rate. In response motion, structure bound remains unchanged. Because regulates eventual onto planet, predict little change rates between planets.