Numerical simulations identify a sharp transition between runaway disruption and stable eccentric mass transfer in star-black hole binaries set by pericenter distance.
Title resolution pending
4 Pith papers cite this work. Polarity classification is still indexing.
4
Pith papers citing it
fields
astro-ph.HE 4verdicts
UNVERDICTED 4representative citing papers
Simulations identify black hole-giant collisions as the main formation channel for ultracompact black hole-white dwarf binaries in globular clusters, with mock catalogs suggesting order-one LISA-detectable sources in the Milky Way.
Reduces elliptic triple outcome model to one free parameter, matches N-body simulations except at low angular momentum, and finds observably eccentric merger fractions of 2.6-4.4% in 10^5-10^7 solar mass clusters.
Binary evolution simulations identify short (20-500 days) and long (2000-4000 days) orbital period ranges where massive star-black hole systems retain enough angular momentum for GRB jet production with negligible mass loss.
citing papers explorer
-
Bridging Roche Lobe Overflow and micro-TDEs: The Runaway Evolution of Eccentric Mass Transfer in Star-Black Hole Binaries
Numerical simulations identify a sharp transition between runaway disruption and stable eccentric mass transfer in star-black hole binaries set by pericenter distance.
-
Formation of Black Hole-White Dwarf X-ray Binaries in Globular Clusters
Simulations identify black hole-giant collisions as the main formation channel for ultracompact black hole-white dwarf binaries in globular clusters, with mock catalogs suggesting order-one LISA-detectable sources in the Milky Way.
-
Intermediate States in Chaotic Triple Evolution and Applications to Black Hole Merger Statistics
Reduces elliptic triple outcome model to one free parameter, matches N-body simulations except at low angular momentum, and finds observably eccentric merger fractions of 2.6-4.4% in 10^5-10^7 solar mass clusters.
-
Simulations of Interacting Binary Systems -- Pathways to Radio Bright GRB Progenitors
Binary evolution simulations identify short (20-500 days) and long (2000-4000 days) orbital period ranges where massive star-black hole systems retain enough angular momentum for GRB jet production with negligible mass loss.