Erratum: Relativistic Bondi accretion for stiff equations of state

Richards, Chloe B; Baumgarte, Thomas W.; Shapiro, Stuart L.

doi:10.1093/mnras/stab2069

Cited by 6 publications

(4 citation statements)

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“…We see that the accretion rate increases rapidly as the sound speed a ∞ increases, and becomes divergent when approaching the sound barrier, see the middle panel of figure 1. This contrasts with the result of [65] in considering the relativistic Bondi accretion of the matter with polytropic EoS, for which the accretion rate remains finite as a ∞ increases. However, there is a trade-off between the accretion rate ( Ṁ ) and accretion range (r B ): The larger the accretion rate, the smaller the accretion range, see figure 1 (middle and bottom panels).…”

Section: Jcap08(2022)032contrasting

confidence: 78%

“…By solving the relativistic Bondi accretion problem, we find that the corresponding accretion rate, Ṁ ≥ 96πG 2 M 2 m 4 /λ 3 , is bounded from below, and can become divergently large when the initial sound speed approaches the sound barrier. This is quite different from the one for the polytropic type of matter [65]. Assuming this scalar field dominates the main component of DM around the BH, the shape of the density spike is determined by the model parameters of the DM model, i.e., mass and quartic coupling.…”

Section: Jcap08(2022)032 4 Conclusionmentioning

confidence: 81%

“…Inspired by the early works [59][60][61], there are recent studies on the spike or cusp profiles around a BH by quite different approaches for various DM models [62][63][64][65][66][67][68]. Our work can be seen as an extension along the same line but consider a nontrivial SIDM with a closed form of non-polytropic EoS.…”

Section: Jcap08(2022)032mentioning

confidence: 96%

“…On the other hand, we can fit some particular region over which γ remains constant. In such cases, the result shall take the limiting power-law form obtained in [65] (see (A.8) therein)…”

Section: Jcap08(2022)032mentioning

confidence: 99%

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Self-interacting dark scalar spikes around black holes via relativistic Bondi accretion

Feng

Parisi

Chen

et al. 2022

J. Cosmol. Astropart. Phys.

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We consider the spike mass density profile in a dark halo by self-consistently solving the relativistic Bondi accretion of dark matter onto a non-spining black hole of mass M. We assume that the dominant component of the dark matter in the halo is a Standard model gauge-singlet scalar. Its mass m ≃ 10-5 eV and quartic self-coupling λ ≲ 1019 are constrained to be compatible with the properties of galactic dark halos. In the hydrodynamic limit, we find that the accretion rate is bounded from below, M min = 96πG 2 M 2 m 4/λħ 3. Therefore, for M = 106 M⊙ we have M min ≃ 1.41 × 10-9 M ⊙ yr-1, which is subdominant compared to the Eddington accretion of baryons. The spike density profile ρ 0(r) within the self-gravitating regime cannot be fitted well by a single-power law but a double-power one. Despite that, we can fit ρ 0(r) piecewise and find that ρ 0(r) ∝ r -1.20 near the sound horizon, ρ 0(r) ∝ r -1.00 towards the Bondi radius and ρ 0(r) ∝ r -1.08 for the region in between. This contrasts with more cuspy ρ 0(r) ∝ r -1.75 for dark matter with Coulomb-like self-interaction.

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Section: Jcap08(2022)032contrasting

confidence: 78%

Section: Jcap08(2022)032 4 Conclusionmentioning

confidence: 81%

Section: Jcap08(2022)032mentioning

confidence: 96%

“…On the other hand, we can fit some particular region over which γ remains constant. In such cases, the result shall take the limiting power-law form obtained in [65] (see (A.8) therein)…”

Section: Jcap08(2022)032mentioning

confidence: 99%

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