2024/10/07 by Yossef Zenati, Zenati, Yossef, Mor Rozner +5 · 2 citations
Physics and Astronomy · #FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE) #Pulsars and Gravitational Waves Research
paper · pdf · doi:10.48550/arxiv.2410.05391
openalex publication_date 2024/10/07 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/01
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 γ-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. ∼ 0.1 M_\odot. These processes are most important when the initial neutron star/black hole mass ratio q is in the range ≈ 0.2 - 0.8, the orbital semimajor axis is 40 \lesssim a0/rg \lesssim 300 (rg ≡ GM\rm B/c2), and the eccentricity is large, e0 \gtrsim 0.8. Systems of this sort may be generated through the dynamical evolution of a triple system, as well as by other means.