A Fully General, Non-Perturbative Treatment of Impulsive Heating

TL;DR

This paper introduces a comprehensive, non-perturbative method for analyzing impulsive encounters between astrophysical objects, accurately capturing close encounters and avoiding divergence issues inherent in traditional approximations.

Contribution

It develops a fully general analytical framework for impulsive encounters that works for any impact parameter and addresses limitations of the distant tide approximation.

Findings

Provides analytical expressions for velocity change in various profiles

Validates the formalism for straight-path and eccentric orbits

Discusses mass loss in galaxy encounters

Abstract

Impulsive encounters between astrophysical objects are usually treated using the distant tide approximation (DTA) for which the impact parameter, $b$, is assumed to be significantly larger than the characteristic radii of the subject, $r_{\mathrm{S}}$, and the perturber, $r_{\mathrm{P}}$. The perturber potential is then expanded as a multipole series and truncated at the quadrupole term. When the perturber is more extended than the subject, this standard approach can be extended to the case where $r_{\mathrm{S}} \ll b < r_{\mathrm{P}}$. However, for encounters with $b$ of order $r_{\mathrm{S}}$ or smaller, the DTA typically overpredicts the impulse, $\Delta \mathbf{v}$, and hence the internal energy change of the subject, $\Delta E_{\mathrm{int}}$. This is unfortunate, as these close encounters are the most interesting, potentially leading to tidal capture, mass stripping, or tidal disruption. Another drawback of the DTA is that $\Delta E_{\mathrm{int}}$ is proportional to the moment of inertia, which diverges unless the subject is truncated or has a density profile that falls off faster than $r^{-5}$. To overcome these shortcomings, this paper presents a fully general, non-perturbative treatment of impulsive encounters which is valid for any impact parameter, and not hampered by divergence issues, thereby negating the necessity to truncate the subject. We present analytical expressions for $\Delta \mathbf{v}$ for a variety of perturber profiles, apply our formalism to both straight-path encounters and eccentric orbits, and discuss the mass loss due to tidal shocks in gravitational encounters between equal mass galaxies.