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arxiv: 2606.02726 · v1 · pith:2BU6AEFQnew · submitted 2026-06-01 · 🌌 astro-ph.HE · astro-ph.SR

Accretion of Primordial Black Holes in Stellar Interiors

Matteo Cantiello , Ore Gottlieb , Cameron Norton , Matthew Kleban , Ken Van Tilburg This is my paper

Pith reviewed 2026-06-28 12:55 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.SR
keywords primordial black holesstellar accretionBondi accretionradiative efficiencybremsstrahlung coolingphoton trappingaccretion regimes
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The pith

Cooling near the event horizon lets primordial black holes as light as 10^{-16} solar masses consume a solar-mass star within a Hubble time.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper computes how small primordial black holes accrete gas while embedded in the core of a sun-like star, solving the flow equations with self-consistent cooling for the first time. It shows that bremsstrahlung radiation at temperatures near 10^{11} K near the black hole changes the accretion from the classical adiabatic case, raising the mass inflow rate by a factor of 2 to 7 and dropping the fraction of rest-mass energy radiated away by roughly ten times. These changes keep the growth super-exponential across three identified regimes and lower the starting mass needed for the black hole to swallow the entire star in cosmic time to about 10^{-16} solar masses. A reader would care because the result revises how dangerous or detectable such black holes could be inside ordinary stars.

Core claim

We solve the time-dependent spherical Euler equations with an implicit cooling source term to determine accretion rate, radiative efficiency, and flow structure self-consistently across the optically thin range. This yields three regimes: a Hot Bondi regime below 10^{-14} solar masses where cooling is negligible; a bremsstrahlung-cooling regime from 10^{-14} to 5 times 10^{-13} solar masses that drives the flow toward isothermal with efficiency near 10^{-2}; and a photon-trapping regime above that mass where the Bondi sphere is optically thick and the rate stays near the classical Bondi value. Cooling therefore enhances the accretion rate by a factor of roughly 2-7 throughout the spherical r

What carries the argument

Time-dependent spherical Euler equations with an implicit cooling source term that self-consistently sets the accretion rate and radiative efficiency in three regimes from Hot Bondi through bremsstrahlung cooling to photon trapping.

If this is right

  • Growth of the black hole remains super-exponential while the flow stays spherical.
  • Radiative efficiency falls to approximately 10^{-2} once bremsstrahlung cooling becomes important.
  • Above 5 times 10^{-13} solar masses the accretion rate stays close to the classical Bondi value because of photon trapping.
  • The threshold mass for destroying a solar-mass star drops to roughly 10^{-16} solar masses.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Stellar lifetimes could place new upper limits on the abundance of primordial black holes if the cooling-enhanced growth holds.
  • The same cooling physics might alter accretion estimates for other compact objects embedded in dense gas.
  • Observing unusually rapid stellar evolution or sudden disappearance of stars could test the predicted growth rates.

Load-bearing premise

Microphysical cooling at temperatures around 10^{11} K can be captured by an implicit source term in the spherical Euler equations without needing full radiation transport or magnetic fields.

What would settle it

A simulation of the same mass range that includes explicit radiative transfer and shows the accretion rate or efficiency differing by more than a factor of two from the values reported for masses near 10^{-16} solar masses.

Figures

Figures reproduced from arXiv: 2606.02726 by Cameron Norton, Ken Van Tilburg, Matteo Cantiello, Matthew Kleban, Ore Gottlieb.

Figure 1
Figure 1. Figure 1: Schematic of the radiative feedback mechanism on the Bondi boundary conditions. Accretion luminosity Lacc produced near the PBH (central black circle) escapes the Bondi sphere (blue circle, radius rB) and is absorbed by the ambient stellar plasma just outside it, raising the local temperature from T∞ to T∞ + ∆T (or￾ange shading). The deposited energy is transported outward by pho￾ton diffusion (brown dashe… view at source ↗
Figure 2
Figure 2. Figure 2: Schematic overview of the three spherical-accretion regimes and the disk-accretion regime onto a PBH embedded in a stellar interior, ordered by increasing MBH. Hot Bondi (MBH ≲ 10−14 M⊙): the Bondi sphere is optically thin (τ < 1); bremsstrahlung photons (orange wavy arrows) escape freely without interacting with the infalling gas (grey arrows), yielding η ≈ 10−2 . Bremsstrahlung cooling (10−14–5×10−13 M⊙)… view at source ↗
Figure 3
Figure 3. Figure 3: Physical length scales controlling the accretion regime as a function of PBH mass, for solar core conditions. The Bondi ra￾dius rB (blue) defines the gravitational sphere of influence. The vertical dotted line marks τ(rB) = 1, where the Bondi sphere becomes optically thick (M ∼ 5 × 10−13 M⊙). The photon trapping radius rtrap (red) exceeds rB at M ∼ 10−9 M⊙. Two circularization radii rcirc (or￾ange) are sho… view at source ↗
Figure 4
Figure 4. Figure 4: Steady-state radial profiles from the time-dependent Euler solver for MBH = 10−16, 10−13, and 10−11 M⊙. (a) Temperature, (b) infall velocity, (c) density, and (d) Mach number as a function of r/rS. Dashed grey lines show the adiabatic Bondi solution. The vertical dashed line marks rB. The transition from near-adiabatic (low mass) to nearly isothermal (high mass) flow is evident in the temperature panel, wh… view at source ↗
Figure 5
Figure 5. Figure 5: Opacity (top) and cumulative optical depth (bottom) as a function of r/rS for MBH = 10−16, 10−13, and 10−11 M⊙. Thick translucent lines show the total opacity; dashed lines show Klein–Nishina–corrected scattering; dotted lines show Kramers free–free absorption. The vertical dotted line marks the θe = 1 boundary separating the KN-suppressed and Thomson regimes. The horizontal dashed line in the lower panel … view at source ↗
Figure 7
Figure 7. Figure 7: Accretion luminosity as a function of BH mass. The solid blue line shows the locally emitted luminosity Lemitted = η M c ˙ 2 evaluated with the cooling-enhanced accretion rate; the dotted blue line shows the bare-Bondi reference η M˙Bc 2 without the cool￾ing enhancement. The black dashed line is LEdd ∝ M, the dotted black line is the M. C. Begelman (1979) cap 0.6LEdd, and the green dash-dotted line is the … view at source ↗
Figure 8
Figure 8. Figure 8: Top panel: Accretion rate onto a PBH in the solar core as a function of BH mass. The gray solid line shows the adiabatic Bondi rate M˙B ∝ M2 ; the blue dashed line shows the isothermal-limit cooling-enhanced rate f(M)M˙B; the red dotted line shows the legacy Eddington cap LEdd/(ηEddc 2 ) for reference (not applied in our prescription); and the thick black line shows the physical accretion rate of Equation … view at source ↗
Figure 9
Figure 9. Figure 9: Growth trajectories MBH(t) for PBHs with initial masses M0 = 10−17–10−10 M⊙ embedded in the solar core (color scale, from light to dark green). Trajectories are trimmed at 0.01M⊙. PBHs with M0 ≳ 10−16 M⊙ reach this threshold within a Hubble time; lighter PBHs stall in the Hot Bondi regime. Horizontal colored bands indicate the accretion regimes from Section 3.1. Vertical lines mark the solar age (t⊙ = 4.6 … view at source ↗
Figure 10
Figure 10. Figure 10: Schematic of the recycling/pile-up geometry inside the collisionless region. The flow is hydrodynamic near rB and becomes collisionless below rcoll. Most particles miss the GR loss cone on a single inward pass, return to rcoll, re-thermalize, and either are recaptured or circularize after losing orbital energy to bremsstrahlung. Direct GR capture (loss cone) accounts for ∼ 0.2% of entrants; ∼ 33% are refl… view at source ↗
Figure 11
Figure 11. Figure 11: Effective Knudsen number at the circularization radius as a function of specific angular momentum, for MBH = 10−16 M⊙. The hatched bands mark the excluded loss-cone (ℓ < ℓcrit) and reflected (ℓ > ℓmax) populations. The pile-up enhancement ξ (ℓ) is sufficient to make Kneff < 1 for the bulk of the recycling population (ℓ ≳ ℓ⋆ ≃ 12ℓcrit), so most circularization radii are self-collisionalized. Only a low-ℓ t… view at source ↗
read the original abstract

We study spherical accretion onto primordial black holes (PBHs) embedded in the core of a solar-type star. We compute the radiative efficiency self-consistently for the first time across the optically thin range ($10^{-16.5}$-$10^{-10}M_\odot$) with time-dependent simulations, and follow the growth up to $10^{-2}M_\odot$ using an analytical photon-trapping prescription above $5\times 10^{-13}M_\odot$. Near the Schwarzschild radius ($r_{\rm S}\sim 10^{-11}$cm for a $10^{-16}M_\odot$ PBH), gas compressed to $T\sim 10^{11}$K radiates through microphysical processes that fundamentally alter the classical adiabatic Bondi solution. We solve the time-dependent spherical Euler equations with an implicit cooling source term, determining $\dot M$, $\eta = L/\dot M c^2$, and the flow structure self-consistently. We identify three regimes for spherical accretion: a Hot Bondi regime ($M_{\rm BH}\lesssim 10^{-14}M_\odot$) in which bremsstrahlung cooling is dynamically negligible; a bremsstrahlung-cooling regime ($10^{-14}$-$5\times 10^{-13}M_\odot$) driving the flow toward isothermal with $\eta\approx 10^{-2}$; and a photon-trapping regime above $5\times 10^{-13}M_\odot$, in which the Bondi sphere is optically thick and the accretion rate remains close to the Bondi value. Cooling enhances $\dot M$ by a factor of $\sim$2-7, keeping growth super-exponential throughout the spherical regime. The radiative efficiency is an order of magnitude lower than previously assumed, and the critical initial PBH mass required to consume a solar-mass star within a Hubble time is $M_{\rm 0,crit}\sim 10^{-16}M_\odot$.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The paper studies spherical accretion of primordial black holes (PBHs) in solar-type stellar cores. It solves the time-dependent spherical Euler equations with an implicit cooling source term to compute radiative efficiency self-consistently in the optically thin regime (10^{-16.5} to 10^{-10} M_⊙), then switches to an analytical photon-trapping prescription above 5×10^{-13} M_⊙. The work identifies three regimes (Hot Bondi, bremsstrahlung-cooling, photon-trapping), finds cooling enhances \dot M by a factor of ~2-7 with η≈10^{-2}, and concludes the critical initial PBH mass to consume a solar-mass star in a Hubble time is M_{0,crit}∼10^{-16} M_⊙.

Significance. If the numerical results hold, the self-consistent treatment of cooling and efficiency across regimes strengthens constraints on PBH masses that could disrupt stars, with implications for PBH dark matter searches. The time-dependent simulations determining \dot M and η without post-hoc fitting are a methodological strength relative to prior analytic Bondi assumptions.

major comments (2)
  1. [description of bremsstrahlung-cooling regime and implicit cooling implementation] The bremsstrahlung-cooling regime (10^{-14} to 5×10^{-13} M_⊙) relies on an implicit cooling source term in the Euler equations to produce the factor of 2-7 enhancement in \dot M and the drop in η to ~10^{-2}; this term replaces full radiation transport near r_S at T~10^{11} K where optical depth nears unity, but the manuscript provides no quantitative test (e.g., comparison to diffusion approximation or optical-depth calculation) showing the net cooling rate is accurate to better than the reported enhancement factor.
  2. [transition to photon-trapping regime] The switch to the analytical photon-trapping prescription at exactly 5×10^{-13} M_⊙ is presented as the point where the Bondi sphere becomes optically thick, yet this threshold is listed among the free parameters and lacks an explicit derivation from the simulated optical depth or trapping condition; altering it would directly rescale the integrated growth and shift M_{0,crit}.
minor comments (2)
  1. Notation for the three regimes should be defined once with explicit mass boundaries and referenced consistently when quoting the enhancement factor.
  2. The abstract states the enhancement keeps growth 'super-exponential throughout the spherical regime'; a brief quantitative comparison of the integrated growth timescale with and without cooling would clarify this claim.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful review and for recognizing the methodological value of our time-dependent simulations. We respond to the major comments below and will revise the manuscript to address the identified gaps in validation and derivation.

read point-by-point responses

  1. Referee: The bremsstrahlung-cooling regime (10^{-14} to 5×10^{-13} M_⊙) relies on an implicit cooling source term in the Euler equations to produce the factor of 2-7 enhancement in \dot M and the drop in η to ~10^{-2}; this term replaces full radiation transport near r_S at T~10^{11} K where optical depth nears unity, but the manuscript provides no quantitative test (e.g., comparison to diffusion approximation or optical-depth calculation) showing the net cooling rate is accurate to better than the reported enhancement factor.

    Authors: We agree that a quantitative validation of the implicit cooling term would strengthen the results. The term is used because the cooling timescale is much shorter than the dynamical timescale in this regime, but we will add to the revised manuscript an explicit optical-depth calculation using the simulated density and temperature profiles near r_S, together with a comparison of the cooling rate to the diffusion approximation. This will confirm that the reported enhancement remains robust. revision: yes

  2. Referee: The switch to the analytical photon-trapping prescription at exactly 5×10^{-13} M_⊙ is presented as the point where the Bondi sphere becomes optically thick, yet this threshold is listed among the free parameters and lacks an explicit derivation from the simulated optical depth or trapping condition; altering it would directly rescale the integrated growth and shift M_{0,crit}.

    Authors: The threshold marks the mass at which the simulated Bondi sphere reaches optical depth of order unity. While the original text did not include the explicit derivation, the value is physically motivated rather than arbitrary. In revision we will add the optical-depth calculation versus black-hole mass extracted from the simulations to derive the transition point, and we will include a sensitivity test showing the effect of varying the threshold on the integrated growth and on M_{0,crit}. revision: yes

Circularity Check

0 steps flagged

No significant circularity; central results from self-consistent simulations

full rationale

The paper computes radiative efficiency, accretion rates, and the critical PBH mass M_{0,crit} via time-dependent spherical Euler simulations with an implicit cooling term across the optically thin regime, followed by an analytic photon-trapping model above 5e-13 M_sun. These steps determine \dot M and \eta directly from the equations without any reduction to a fitted parameter defined from the target result, self-citation load-bearing the central claim, or ansatz smuggled via prior work. The derivation chain remains independent of the final M_{0,crit} value.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard hydrodynamics plus specific microphysical cooling rates at extreme temperatures; no new particles or forces are introduced, but several modeling choices function as effective free parameters.

free parameters (2)
  • transition mass for photon-trapping prescription
    The switch at 5e-13 M_sun from simulation to analytic treatment is chosen to match optical depth; its exact value affects the quoted growth factor.
  • implicit cooling implementation details
    The precise form of the cooling function (bremsstrahlung coefficient, temperature dependence) is not stated and must be assumed from standard tables.
axioms (2)
  • domain assumption Spherical symmetry and absence of magnetic fields or angular momentum remain valid throughout the accretion flow
    Invoked when the authors restrict the problem to the time-dependent spherical Euler equations.
  • domain assumption Microphysical radiative processes at T~10^11 K near r_S can be treated as an optically thin cooling term without full radiative transfer
    Required for the self-consistent eta calculation in the optically thin regime.

pith-pipeline@v0.9.1-grok · 5907 in / 1790 out tokens · 32395 ms · 2026-06-28T12:55:45.155277+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

297 extracted references · 264 canonical work pages · 108 internal anchors

  1. [1]

    The Internal Constitution of the Stars

  2. [2]

    , year = 1957, month = jan, volume =

    Statistical dynamics and accretion. , year = 1957, month = jan, volume =. doi:10.1093/mnras/117.1.50 , adsurl =

    work page doi:10.1093/mnras/117.1.50 1957

  3. [3]

    , keywords =

    Nearly collisionless spherical accretion. , keywords =. doi:10.1093/mnras/181.2.347 , adsurl =

    work page doi:10.1093/mnras/181.2.347

  4. [4]

    Improved angular momentum evolution model for solar-like stars

    Improved angular momentum evolution model for solar-like stars. , keywords =. doi:10.1051/0004-6361/201321302 , archivePrefix =. 1306.2130 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201321302

  5. [5]

    , year = 1959, month = feb, volume =

    Spontaneously Growing Transverse Waves in a Plasma Due to an Anisotropic Velocity Distribution. , year = 1959, month = feb, volume =. doi:10.1103/PhysRevLett.2.83 , adsurl =

    work page doi:10.1103/physrevlett.2.83 1959

  6. [6]

    , keywords =

    Nonadiabatic self-consistent spherical accretion as a model for quasars and active galactic nuclei. , keywords =. doi:10.1086/162175 , adsurl =

    work page doi:10.1086/162175

  7. [7]

    , keywords =

    Stationary spherical accretion into black holes - The transition from the optically thin to the optically thick regime. , keywords =

  8. [8]

    , keywords =

    Resonant Enhancements in Weakly Interacting Massive Particle Capture by the Earth. , keywords =. doi:10.1086/165653 , adsurl =

    work page doi:10.1086/165653

  9. [9]

    , keywords =

    Capture by the sun of a galactic population of weakly interacting, massive particles. , keywords =. doi:10.1086/163485 , adsurl =

    work page doi:10.1086/163485

  10. [10]

    , keywords =

    Accretion of Matter by Condensed Objects. , keywords =. doi:10.1007/BF00649949 , adsurl =

    work page doi:10.1007/bf00649949

  11. [11]

    , keywords =

    Radiation from spherical accretion onto black holes. , keywords =

  12. [12]

    , year = 1973, month = mar, volume =

    Accretion onto Black Holes: the Emergent Radiation Spectrum. , year = 1973, month = mar, volume =. doi:10.1086/151982 , adsurl =

    work page doi:10.1086/151982 1973

  13. [13]

    , keywords =

    Super-Eddington Accretion onto Black Holes and Its Application to Fallback Accretion. , keywords =. doi:10.3847/1538-4357/ae30dc , archivePrefix =. 2507.16893 , primaryClass =

    work page doi:10.3847/1538-4357/ae30dc

  14. [14]

    , keywords =

    Black holes in radiation-dominated gas: an analogue of the Bondi accretion problem. , keywords =. doi:10.1093/mnras/184.1.53 , adsurl =

    work page doi:10.1093/mnras/184.1.53

  15. [15]

    I - Equations and numerical methods

    Optically thick, time-dependent spherical accretion onto a black hole. I - Equations and numerical methods. , keywords =. doi:10.1086/162419 , adsurl =

    work page doi:10.1086/162419

  16. [16]

    III Optically thick accretion in particular cases

    Stationary spherical accretion into black holes. III Optically thick accretion in particular cases. , keywords =. doi:10.1093/mnras/206.3.589 , adsurl =

    work page doi:10.1093/mnras/206.3.589

  17. [17]

    Self-consistent Models of Spherical Accretion onto Black Holes. II. Two-Temperature Solutions with Pairs. , keywords =. doi:10.1086/168669 , adsurl =

    work page doi:10.1086/168669

  18. [18]

    , keywords =

    Spherical Accretion onto Black Holes: A Complete Analysis of Stationary Solutions. , keywords =. doi:10.1086/170781 , adsurl =

    work page doi:10.1086/170781

  19. [19]

    Rubin, S. G. and Khlopov, M. Yu. and Sakharov, A. S. Primordial black holes from nonequilibrium second order phase transition. Grav. Cosmol. 2000. arXiv:hep-ph/0005271

    Pith/arXiv arXiv 2000

  20. [20]

    Black holes and the multiverse , volume=

    Garriga, Jaume and Vilenkin, Alexander and Zhang, Jun , year=. Black holes and the multiverse , volume=. Journal of Cosmology and Astroparticle Physics , publisher=. doi:10.1088/1475-7516/2016/02/064 , number=

    work page doi:10.1088/1475-7516/2016/02/064 2016

  21. [21]

    Spontaneous Generation of Density Perturbations in the Early Universe

    Crawford, Matt and Schramm, David N. Spontaneous Generation of Density Perturbations in the Early Universe. Nature. 1982. doi:10.1038/298538a0

    work page doi:10.1038/298538a0 1982

  22. [22]

    Monochromatic mass spectrum of primordial black holes

    Kleban, Matthew and Norton, Cameron E. Monochromatic mass spectrum of primordial black holes. Phys. Rev. D. 2025. doi:10.1103/PhysRevD.111.023538. arXiv:2310.09898

    work page doi:10.1103/physrevd.111.023538 2025

  23. [24]

    , year = 1982, month = jul, volume =

    Electron-Positron Pair Equilibria in Relativistic Plasmas. , year = 1982, month = jul, volume =. doi:10.1086/160082 , adsurl =

    work page doi:10.1086/160082 1982

  24. [25]

    , keywords =

    Magnetic Hair and Reconnection in Black Hole Magnetospheres. , keywords =. doi:10.1103/PhysRevLett.127.055101 , archivePrefix =. 2109.14620 , primaryClass =

    work page doi:10.1103/physrevlett.127.055101

  25. [26]

    High resolution schemes for hyperbolic conservation laws , journal =

    Ami Harten , abstract =. High resolution schemes for hyperbolic conservation laws , journal =. 1983 , issn =. doi:https://doi.org/10.1016/0021-9991(83)90136-5 , url =

    work page doi:10.1016/0021-9991(83)90136-5 1983

  26. [27]

    , keywords =

    Numerical fits to important rates in high temperature astrophysical plasmas. , keywords =. doi:10.1093/mnras/204.4.1269 , adsurl =

    work page doi:10.1093/mnras/204.4.1269

  27. [28]

    Radiative processes in astrophysics

  28. [29]

    Introduction to Stellar Astrophysics

  29. [30]

    , year = 1974, month = aug, volume =

    Black holes in the early Universe. , year = 1974, month = aug, volume =. doi:10.1093/mnras/168.2.399 , adsurl =

    work page doi:10.1093/mnras/168.2.399 1974

  30. [31]

    The end of the MACHO era- revisited: new limits on MACHO masses from halo wide binaries

    The End of the MACHO Era, Revisited: New Limits on MACHO Masses from Halo Wide Binaries. , keywords =. doi:10.1088/0004-637X/790/2/159 , archivePrefix =. 1406.5169 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/790/2/159

  31. [32]

    , keywords =

    Massive black holes in galactic halos ?. , keywords =. doi:10.1086/163729 , adsurl =

    work page doi:10.1086/163729

  32. [33]

    Constraints on MACHO Dark Matter from Compact Stellar Systems in Ultra-Faint Dwarf Galaxies

    Constraints on MACHO Dark Matter from Compact Stellar Systems in Ultra-faint Dwarf Galaxies. , keywords =. doi:10.3847/2041-8205/824/2/L31 , archivePrefix =. 1605.03665 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8205/824/2/l31 2041

  33. [34]

    Black Holes in the Era of Gravitational-Wave Astronomy , year = 2024, editor =

    Primordial black holes. Black Holes in the Era of Gravitational-Wave Astronomy , year = 2024, editor =. doi:10.1016/B978-0-32-395636-9.00012-8 , adsurl =

    work page doi:10.1016/b978-0-32-395636-9.00012-8 2024

  34. [35]

    Primordial Black Holes - Perspectives in Gravitational Wave Astronomy -

    Primordial black holes perspectives in gravitational wave astronomy. Classical and Quantum Gravity , keywords =. doi:10.1088/1361-6382/aaa7b4 , archivePrefix =. 1801.05235 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1361-6382/aaa7b4

  35. [36]

    , year = 1931, month = jul, volume =

    The Maximum Mass of Ideal White Dwarfs. , year = 1931, month = jul, volume =. doi:10.1086/143324 , adsurl =

    work page doi:10.1086/143324 1931

  36. [37]

    , keywords =

    Revisiting constraints on asteroid-mass primordial black holes as dark matter candidates. , keywords =. doi:10.1088/1475-7516/2019/08/031 , archivePrefix =. 1906.05950 , primaryClass =

    work page doi:10.1088/1475-7516/2019/08/031 2019

  37. [38]

    , keywords =

    Primordial black holes capture by stars and induced collapse to low-mass stellar black holes. , keywords =. doi:10.1093/mnras/stac2647 , archivePrefix =. 2205.13003 , primaryClass =

    work page doi:10.1093/mnras/stac2647

  38. [39]

    , keywords =

    Dark matter capture in celestial objects: improved treatment of multiple scattering and updated constraints from white dwarfs. , keywords =. doi:10.1088/1475-7516/2019/08/018 , archivePrefix =. 1906.04204 , primaryClass =

    work page doi:10.1088/1475-7516/2019/08/018 2019

  39. [40]

    Dark Matter Triggers of Supernovae

    Dark matter triggers of supernovae. , keywords =. doi:10.1103/PhysRevD.92.063007 , archivePrefix =. 1505.04444 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.92.063007

  40. [41]

    , keywords =

    Primordial black holes captured by neutron stars: Simulations in general relativity. , keywords =. doi:10.1103/PhysRevD.110.023021 , archivePrefix =. 2405.10365 , primaryClass =

    work page doi:10.1103/physrevd.110.023021

  41. [42]

    , keywords =

    Primordial black holes captured by neutron stars: Relativistic point-mass treatment. , keywords =. doi:10.1103/PhysRevD.109.123012 , archivePrefix =. 2404.08735 , primaryClass =

    work page doi:10.1103/physrevd.109.123012

  42. [43]

    , keywords =

    Fate of a neutron star with an endoparasitic black hole and implications for dark matter. , keywords =. doi:10.1103/PhysRevD.100.124026 , archivePrefix =. 1909.07968 , primaryClass =

    work page doi:10.1103/physrevd.100.124026 1909

  43. [44]

    , keywords =

    Accretion onto black holes inside neutron stars with piecewise-polytropic equations of state: Analytic and numerical treatments. , keywords =. doi:10.1103/PhysRevD.104.123021 , archivePrefix =. 2110.08285 , primaryClass =

    work page doi:10.1103/physrevd.104.123021

  44. [45]

    , keywords =

    Accretion onto a small black hole at the center of a neutron star. , keywords =. doi:10.1103/PhysRevD.103.104009 , archivePrefix =. 2102.09574 , primaryClass =

    work page doi:10.1103/physrevd.103.104009

  45. [46]

    , keywords =

    Neutron stars harboring a primordial black hole: Maximum survival time. , keywords =. doi:10.1103/PhysRevD.103.L081303 , archivePrefix =. 2101.12220 , primaryClass =

    work page doi:10.1103/physrevd.103.l081303

  46. [47]

    Growth of Black Holes in the interior of Rotating Neutron Stars

    Growth of black holes in the interior of rotating neutron stars. , keywords =. doi:10.1103/PhysRevD.90.043512 , archivePrefix =. 1312.3764 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.90.043512

  47. [48]

    , keywords =

    Evolution of a primordial black hole inside a rotating solar-type star. , keywords =. doi:10.1093/mnras/277.1.25 , adsurl =

    work page doi:10.1093/mnras/277.1.25

  48. [49]

    , keywords =

    Mind the Gap: The Location of the Lower Edge of the Pair-instability Supernova Black Hole Mass Gap. , keywords =. doi:10.3847/1538-4357/ab518b , archivePrefix =. 1910.12874 , primaryClass =

    work page doi:10.3847/1538-4357/ab518b 1910

  49. [50]

    , keywords =

    Fragmentation in Gravitationally Unstable Collapsar Disks and Subsolar Neutron Star Mergers. , keywords =. doi:10.3847/2041-8213/ad6990 , archivePrefix =. 2407.07955 , primaryClass =

    work page doi:10.3847/2041-8213/ad6990 2041

  50. [51]

    Black hole growth through hierarchical black hole mergers in dense star clusters: implications for gravitational wave detections

    Black hole growth through hierarchical black hole mergers in dense star clusters: implications for gravitational wave detections. , keywords =. doi:10.1093/mnras/stz1149 , archivePrefix =. 1811.03640 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz1149

  51. [52]

    , keywords =

    Black holes: The next generation repeated mergers in dense star clusters and their gravitational-wave properties. , keywords =. doi:10.1103/PhysRevD.100.043027 , archivePrefix =. 1906.10260 , primaryClass =

    work page doi:10.1103/physrevd.100.043027 1906

  52. [53]

    , keywords =

    Spinning into the Gap: Direct-horizon Collapse as the Origin of GW231123 from End-to-end General-relativistic Magnetohydrodynamic Simulations. , keywords =. doi:10.3847/2041-8213/ae0d81 , archivePrefix =. 2508.15887 , primaryClass =

    work page doi:10.3847/2041-8213/ae0d81 2041

  53. [54]

    Gravitational Waves from Primordial Black Hole Mergers

    Gravitational waves from primordial black hole mergers. , keywords =. doi:10.1088/1475-7516/2017/09/037 , archivePrefix =. 1707.01480 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2017/09/037 2017

  54. [55]

    Gravitational Wave signatures of inflationary models from Primordial Black Hole Dark Matter

    Gravitational wave signatures of inflationary models from Primordial Black Hole dark matter. , keywords =. doi:10.1088/1475-7516/2017/09/013 , archivePrefix =. 1707.02441 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1475-7516/2017/09/013 2017

  55. [56]

    The clustering of massive Primordial Black Holes as Dark Matter: measuring their mass distribution with Advanced LIGO

    The clustering of massive Primordial Black Holes as Dark Matter: Measuring their mass distribution with advanced LIGO. Physics of the Dark Universe , keywords =. doi:10.1016/j.dark.2016.10.002 , archivePrefix =. 1603.05234 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.dark.2016.10.002 2016

  56. [57]

    , keywords =

    Consistency of Primordial Black Hole Dark Matter with LIGO/Virgo Merger Rates. , keywords =. doi:10.1103/PhysRevLett.126.051302 , archivePrefix =. 2007.03565 , primaryClass =

    work page doi:10.1103/physrevlett.126.051302 2007

  57. [58]

    , year = 1971, month = jan, volume =

    Gravitationally collapsed objects of very low mass. , year = 1971, month = jan, volume =. doi:10.1093/mnras/152.1.75 , adsurl =

    work page doi:10.1093/mnras/152.1.75 1971

  58. [59]

    Dynamics of dwarf galaxies disfavor stellar-mass black hole dark matter

    Dynamics of Dwarf Galaxies Disfavor Stellar-Mass Black Holes as Dark Matter. , keywords =. doi:10.1103/PhysRevLett.119.041102 , archivePrefix =. 1704.01668 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevlett.119.041102

  59. [60]

    , keywords =

    On the reported death of the MACHO era. , keywords =. doi:10.1111/j.1745-3933.2009.00652.x , archivePrefix =. 0903.1644 , primaryClass =

    work page doi:10.1111/j.1745-3933.2009.00652.x 2009

  60. [61]

    The End of the MACHO Era: Limits on Halo Dark Matter from Stellar Halo Wide Binaries

    The End of the MACHO Era: Limits on Halo Dark Matter from Stellar Halo Wide Binaries. , keywords =. doi:10.1086/380562 , archivePrefix =. astro-ph/0307437 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/380562

  61. [62]

    Microlensing constraints on primordial black holes with the Subaru/HSC Andromeda observation

    Microlensing constraints on primordial black holes with Subaru/HSC Andromeda observations. Nature Astronomy , keywords =. doi:10.1038/s41550-019-0723-1 , archivePrefix =. 1701.02151 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1038/s41550-019-0723-1

  62. [63]

    Constraints on Earth-mass primordial black holes from OGLE 5-year microlensing events

    Constraints on Earth-mass primordial black holes from OGLE 5-year microlensing events. , keywords =. doi:10.1103/PhysRevD.99.083503 , archivePrefix =. 1901.07120 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.99.083503 1901

  63. [64]

    Microlensing and dynamical constraints on primordial black hole dark matter with an extended mass function

    Microlensing and dynamical constraints on primordial black hole dark matter with an extended mass function. , keywords =. doi:10.1103/PhysRevD.94.063530 , archivePrefix =. 1609.01143 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.94.063530

  64. [65]

    Communications in Mathematical Physics , year = 1975, month = aug, volume =

    Particle creation by black holes. Communications in Mathematical Physics , year = 1975, month = aug, volume =. doi:10.1007/BF02345020 , adsurl =

    work page doi:10.1007/bf02345020 1975

  65. [66]

    , keywords =

    Gamma rays from primordial black holes. , keywords =. doi:10.1086/154350 , adsurl =

    work page doi:10.1086/154350

  66. [67]

    New cosmological constraints on primordial black holes

    New cosmological constraints on primordial black holes. , keywords =. doi:10.1103/PhysRevD.81.104019 , archivePrefix =. 0912.5297 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.81.104019

  67. [68]

    Primordial Black Holes as a dark matter candidate

    Primordial black holes as a dark matter candidate. Journal of Physics G Nuclear Physics , keywords =. doi:10.1088/1361-6471/abc534 , archivePrefix =. 2007.10722 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1361-6471/abc534 2007

  68. [69]

    , keywords =

    Inflation and primordial black holes as dark matter. , keywords =. doi:10.1103/PhysRevD.50.7173 , adsurl =

    work page doi:10.1103/physrevd.50.7173

  69. [70]

    Massive Primordial Black Holes from Hybrid Inflation as Dark Matter and the seeds of Galaxies

    Massive primordial black holes from hybrid inflation as dark matter and the seeds of galaxies. , keywords =. doi:10.1103/PhysRevD.92.023524 , archivePrefix =. 1501.07565 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.92.023524

  70. [71]

    Primordial Black Holes as Dark Matter: Recent Developments

    Primordial Black Holes as Dark Matter: Recent Developments. Annual Review of Nuclear and Particle Science , keywords =. doi:10.1146/annurev-nucl-050520-125911 , archivePrefix =. 2006.02838 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev-nucl-050520-125911 2006

  71. [72]

    Peculiar Relics from Primordial Black Holes in the Inflationary Paradigm

    Peculiar relics from Primordial Black Holes in the inflationary paradigm. Annalen der Physik , keywords =. doi:10.1002/andp.200310067 , archivePrefix =. astro-ph/0303330 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1002/andp.200310067

  72. [73]

    , keywords =

    The primordial black hole mass spectrum. , keywords =. doi:10.1086/153853 , adsurl =

    work page doi:10.1086/153853

  73. [74]

    Constraints on Primordial Black Holes

    Constraints on primordial black holes. Reports on Progress in Physics , keywords =. doi:10.1088/1361-6633/ac1e31 , archivePrefix =. 2002.12778 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/1361-6633/ac1e31 2002

  74. [75]

    Primordial Black Holes as Dark Matter

    Primordial black holes as dark matter. , keywords =. doi:10.1103/PhysRevD.94.083504 , archivePrefix =. 1607.06077 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1103/physrevd.94.083504

  75. [76]

    , year = 1999, month = aug, volume =

    A compilation of charged-particle induced thermonuclear reaction rates. , year = 1999, month = aug, volume =. doi:10.1016/S0375-9474(99)00030-5 , adsurl =

    work page doi:10.1016/s0375-9474(99)00030-5 1999

  76. [77]

    1969 , institution =

    1969

  77. [78]

    Rosseland and flux mean opacities for Compton scattering

    Rosseland and Flux Mean Opacities for Compton Scattering. , keywords =. doi:10.3847/1538-4357/835/2/119 , archivePrefix =. 1606.09466 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-4357/835/2/119

  78. [79]

    arXiv e-prints , keywords =

    High Metal Content of Highly Accreting Quasars: Analysis of an Extended Sample. arXiv e-prints , keywords =

  79. [80]

    Journal of High Energy Physics , keywords =

    Orbital dynamics of the solar basin. Journal of High Energy Physics , keywords =. doi:10.1007/JHEP12(2024)007 , archivePrefix =. 2408.16041 , primaryClass =

    work page doi:10.1007/jhep12(2024)007 2024

  80. [81]

    doi:10.1007/978-3-642-30304-3 , adsurl =

    Stellar Structure and Evolution. doi:10.1007/978-3-642-30304-3 , adsurl =

    work page doi:10.1007/978-3-642-30304-3

Showing first 80 references.