Morphology and Mach number dependence of subsonic Bondi-Hoyle accretion
We carry out three-dimensional computations of the accretion rate onto an object (of size R sink and mass m) as it moves through a uniform medium at a subsonic speed v ∞. The object is treated as a fully absorbing boundary (e.g., a black hole). In contrast to early conjectures, we show that for an a...
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| Hauptverfasser: | , , , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
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2024, May 1
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| In: |
The astrophysical journal
Year: 2024, Jahrgang: 966, Heft: 1, Pages: 1-11 |
| ISSN: | 1538-4357 |
| DOI: | 10.3847/1538-4357/ad3732 |
| Online-Zugang: | Verlag, kostenfrei, Volltext: https://doi.org/10.3847/1538-4357/ad3732 Verlag, kostenfrei, Volltext: https://dx.doi.org/10.3847/1538-4357/ad3732 
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| Verfasserangaben: | Logan J. Prust, Hila Glanz, Lars Bildsten, Hagai B. Perets and Friedrich K. Röpke |
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| 245 | 1 | 0 | |a Morphology and Mach number dependence of subsonic Bondi-Hoyle accretion |c Logan J. Prust, Hila Glanz, Lars Bildsten, Hagai B. Perets and Friedrich K. Röpke |
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| 520 | |a We carry out three-dimensional computations of the accretion rate onto an object (of size R sink and mass m) as it moves through a uniform medium at a subsonic speed v ∞. The object is treated as a fully absorbing boundary (e.g., a black hole). In contrast to early conjectures, we show that for an accretor with in a gaseous medium with adiabatic index γ = 5/3, the accretion rate is independent of Mach number and is determined only by m and the gas entropy. Our numerical simulations are conducted using two different numerical schemes via the Athena++ and Arepo hydrodynamics solvers, which reach nearly identical steady-state solutions. We find that pressure gradients generated by the isentropic compression of the flow near the accretor are sufficient to suspend much of the surrounding gas in a near-hydrostatic equilibrium, just as predicted from the spherical Bondi-Hoyle calculation. Indeed, the accretion rates for steady flow match the Bondi-Hoyle rate, and are indicative of isentropic flow for subsonic motion where no shocks occur. We also find that the accretion drag may be predicted using the Safronov number, Θ = R A /R sink, and is much less than the dynamical friction for sufficiently small accretors (R sink ≪ R A ). | ||
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