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Black Holes in Astrophysics
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This article reviews the current status of black hole astrophysics, focusing on topics of interest to a physics audience. Astronomers have discovered dozens of compact objects with masses greater than 3 solar masses, the likely maximum mass of a neutron star. These objects are identified as black hole candidates. Some of the candidates have masses of 5 to 20 solar masses and are found in X-ray binaries, while the rest have masses from a million to a billion solar masses and are found in galactic nuclei. A variety of methods are being tried to estimate the spin parameters of the candidate black holes. There is strong circumstantial evidence that many of the objects have event horizons. Recent MHD simulations of magnetized plasma accreting on rotating black holes seem to hint that relativistic jets may be produced by a magnetic analog of the Penrose process.
Forward citations
Cited by 5 Pith papers
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Absorption spectrum and greybody factors of charged black holes in loop quantum gravity
The absorption cross section of massless scalar waves by a charged loop-quantum-gravity black hole increases with the quantum parameter in an intermediate frequency band, decreases with charge, and matches classical a...
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Establishing Compactness as a Population Observable in Gravitational-Wave Astronomy
Hierarchical analysis of GWTC-3 yields C_eff = 0.5^{+0.3}_{-0.1} consistent with black holes and limits low-compactness exotic binary merger rate to <0.7 Gpc^{-3} yr^{-1}.
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Tidal perturbations of an extreme mass ratio inspiral around a Kerr black hole
A closed-form Kerr metric under slow quadrupolar tides yields spin-dependent tidal shifts of the ISCO and light ring, with larger shifts for retrograde orbits around fast-spinning holes.
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Fate of scalar dark matter solitons around supermassive galactic black holes
A self-interacting scalar dark matter soliton around a supermassive black hole settles into a unique critical accretion flow with flux ~ r_s^2 m^4 / λ4 and survives for many Hubble times.
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Observational properties of regular black holes in Asymptotic Safety
As the asymptotic-safety parameter ξ grows, the shadow shrinks, the innermost orbit moves inward, and the accretion disk becomes brighter and more efficient than in Schwarzschild.
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