Mass transfer in eccentric black hole - neutron star mergers

TL;DR

This paper shows that in certain eccentric black hole-neutron star mergers, mass transfer can significantly alter orbital evolution and reduce neutron star mass, affecting the merger dynamics and resulting debris.

Contribution

It introduces the role of mass transfer in eccentric BH/NS mergers, challenging the assumption that gravitational waves solely drive their evolution.

Findings

Mass transfer can reduce neutron star mass by order-unity.

Gas disks of ~0.1 solar masses form before merger.

Mass transfer effects are significant for specific mass ratios and eccentricities.

Abstract

Black hole - neutron star $(BH/NS)$ binaries are of interest in many ways: they are intrinsically multi-messenger systems, highly transient, radiate gravitational waves detectable by LIGO, and may produce $\gamma$-ray bursts. Although it has long been assumed that their late-stage orbital evolution is driven entirely by gravitational wave emission, we show here that in certain circumstances, mass transfer from the neutron star onto the black hole can both alter the binary's orbital evolution and significantly reduce the neutron star's mass when the fraction of its mass transferred per orbit is $\gtrsim 10^{-2}$, the neutron star's mass diminishes by order-unity, leading to mergers in which the neutron star mass is exceptionally small. The mass transfer creates a gas disk around the black hole ${\it before}$ merger that can be comparable in mass to the debris remaining after merger, i.e. $\sim 0.1 M_\odot$. These processes are most important when the initial neutron star/black hole mass ratio $q$ is in the range $\approx 0.2 - 0.8$, the orbital semimajor axis is $40 \lesssim a_0/r_g \lesssim 300 $ ($r_g \equiv GM_{\rm B}/c^2$), and the eccentricity is large, $e_0 \gtrsim 0.8$. Systems of this sort may be generated through the dynamical evolution of a triple system, as well as by other means.