An effective model for the tidal disruption of satellites undergoing minor mergers with axisymmetric primaries

TL;DR

This paper introduces a new semi-analytic model for tidal stripping in minor galaxy mergers with axisymmetric primaries, validated against N-body simulations, improving efficiency in studying black hole binary evolution.

Contribution

The paper presents a novel, effective semi-analytic model for tidal stripping in axisymmetric potentials, validated against simulations, enhancing the study of galaxy mergers and black hole coalescence.

Findings

Model shows good agreement with N-body simulations across various conditions.

Moderate overestimation of mass loss for near-circular orbits.

Model's accuracy is robust despite orbit eccentricity variations.

Abstract

According to the hierarchical formation paradigm, galaxies form through mergers of smaller entities and massive black holes (MBHs), if lurking at their centers, migrate to the nucleus of the newly formed galaxy, where they form binary systems. The formation and evolution of MBH binaries, and in particular their coalescence timescale, is very relevant for current and future facilities aimed at detecting the gravitational-wave signal produced by the MBH close to coalescence. While most of the studies targeting this process are based on hydrodynamic simulations, the high computational cost makes a complete parameter space exploration prohibitive. Semi-analytic approaches represent a valid alternative, but they require ad-hoc prescriptions for the mass loss of the merging galaxies in minor mergers due to tidal stripping, which is not commonly considered or at most modelled assuming very idealised geometries. In this work, we propose a novel, effective model for the tidal stripping in axisymmetric potentials, to be implemented in semi-analytic models. We validate our semi-analytic approach against N-body simulations considering different galaxy sizes, inclinations, and eccentricities, finding only a moderate dependence on the orbit eccentricity. In particular, we find that, for almost circular orbits, our model mildly overestimates the mass loss, and this is due to the adjustment of the stellar distribution after the mass is removed. Nonetheless, the model exhibits a very good agreement with simulations in all the considered conditions, and thus represents an extremely powerful addition to semi-analytic calculations.