Eccentricity Evolution in Gaseous Dynamical Friction

TL;DR

This paper investigates how different gaseous drag forces influence the evolution of orbital eccentricity, revealing a critical density gradient that determines whether orbits become more circular or eccentric, with applications to planetary infall and binary systems.

Contribution

It introduces a semi-analytic model to predict eccentricity changes due to hydrodynamic and dynamical friction forces in gaseous environments, highlighting a critical density gradient threshold.

Findings

Hydrodynamic drag circularizes orbits in gaseous media.

Dynamical friction can increase orbital eccentricity.

A critical density gradient at $ ho o r^{- ext{3}}$ separates these regimes.

Abstract

We analyse how drag forces modify the orbits of objects moving through extended gaseous distributions. We consider how hydrodynamic (surface area) drag forces and dynamical friction (gravitational) drag forces drive the evolution of orbital eccentricity. While hydrodynamic drag forces cause eccentric orbits to become more circular, dynamical friction drag can cause orbits to become more eccentric. We develop a semi-analytic model that accurately predicts these changes by comparing the total work and torque applied to the orbit at periapse and apoapse. We use a toy model of a radial power-law density profile, $\rho \propto r^{-\gamma}$, to determine that there is a critical $\gamma = 3$ power index which separates the eccentricity evolution in dynamical friction: orbits become more eccentric for $\gamma < 3$ and circularize for $\gamma > 3$. We apply these findings to the infall of a Jupiter-like planet into the envelope of its host star. The hydrostatic envelopes of stars are defined by steep density gradients near the limb and shallower gradients in the interior. Under the influence of gaseous dynamical friction, an infalling object's orbit will first decrease in eccentricity, then increase. The critical separation that delineates these regimes is predicted by the local density slope and is linearly dependent on polytropic index. More broadly, our findings indicate that binary systems may routinely emerge from common envelope phases with non-zero eccentricities that were excited by the dynamical friction forces that drove their orbital tightening.