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.
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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.
citing papers explorer
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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.
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Stellar black hole binaries from two common envelope evolution phases in triple stellar systems
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.
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Building three-dimensional giant stellar models for common envelope simulations
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.
- Reproducing morphological features in the supernova remnant G11.2-0.3 by simulating jittering jets