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_papers/Zenati:2024elj.md

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+---
+title: "Mass Transfer in Eccentric Black Hole–Neutron Star Mergers"
+authors:
+  - "Zenati, Yossef"
+  - "Rozner, Mor"
+  - "Krolik, Julian H."
+  - "Most, Elias R."
+jref: "Astrophys.J. 978, 126 (2025)"
+doi: "10.3847/1538-4357/ad9b87"
+date: 2024-10-07
+arxiv: "2410.05391"
+abstract: |
+  Black hole–neutron star binaries are of interest in many ways: they
+  are intrinsically 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 ≳\(10^{−2}\), 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 before merger that can be comparable in
+  mass to the debris remaining after merger, i.e., ~0.1 \(M_{⊙}\). 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 ≲ \(a_{0}/r_{g}\) ≲ 300 (\(r_{g}\) ≡ \(GM_{BH}/c^{2}\)),
+  and the eccentricity is large at \(e_{0}\) ≳ 0.8. Systems of this sort
+  may be generated through the dynamical evolution of a triple system,
+  as well as by other means.
+---