A 4.46 solar-mass black hole is found in a 94-year eccentric orbit with a main-sequence turnoff star in ω Centauri via 23-year astrometric monitoring.
Title resolution pending
5 Pith papers cite this work. Polarity classification is still indexing.
5
Pith papers citing it
years
2026 5verdicts
UNVERDICTED 5representative citing papers
A triple-star channel with two common envelope evolution phases produces merging black hole binaries with positive average χ_eff and a tail of negative values.
Depositing stellar luminosity in an inner shell and cooling low-density outer cells produces a stable pulsating 3D red supergiant model for common envelope simulations without relaxation.
A more efficient 12C+12C rate extends carbon burning, produces less compact pre-supernova structures, and enhances s-process yields of elements heavier than Fe in supernova ejecta from 15-40 solar mass stars.
Hydrodynamic simulations of three pairs of jittering jets in a CCSN reproduce the ring-and-bar morphology of SNR G11.2-0.3.
citing papers explorer
-
A Long Period Stellar-Mass Black Hole Binary in $\omega$ Centauri
A 4.46 solar-mass black hole is found in a 94-year eccentric orbit with a main-sequence turnoff star in ω Centauri via 23-year astrometric monitoring.