Blocking the Hawking radiation

Autzen, Martin; Kouvaris, Chris

doi:10.1103/physrevd.89.123519

Cited by 5 publications

(4 citation statements)

References 48 publications

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“…At the temperatures relevant for ignition (53), all the particles present in the Standard Model are emitted relativistically. Each type of particle (where each helicity state counts as a separate particle) is emitted roughly equally up to percent level corrections [71,72], so long as each particle's mass is less than the black hole temperature. For the temperature indicated in Eq.…”

Section: Black Hole Evaporative Ignition Of White Dwarfsmentioning

confidence: 99%

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Supernovae sparked by dark matter in white dwarfs

Acevedo

Bramante

2019

Phys. Rev. D

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It was recently demonstrated that asymmetric dark matter can ignite supernovae by collecting and collapsing inside lone sub-Chandrasekhar mass white dwarfs, and that this may be the cause of Type Ia supernovae. A ball of asymmetric dark matter accumulated inside a white dwarf and collapsing under its own weight, sheds enough gravitational potential energy through scattering with nuclei, to spark the fusion reactions that precede a Type Ia supernova explosion. In this article we elaborate on this mechanism and use it to place new bounds on interactions between nucleons and asymmetric dark matter for masses m X = 10 6 − 10 16 GeV. Interestingly, we find that for dark matter more massive than 10 11 GeV, Type Ia supernova ignition can proceed through the Hawking evaporation of a small black hole formed by the collapsed dark matter. We also identify how a cold white dwarf's Coulomb crystal structure substantially suppresses dark matter-nuclear scattering at low momentum transfers, which is crucial for calculating the time it takes dark matter to form a black hole. Higgs and vector portal dark matter models that ignite Type Ia supernovae are explored.

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Section: Black Hole Evaporative Ignition Of White Dwarfsmentioning

confidence: 99%

“…( 53), we will only need to consider emitted particles that carry color charge. At these temperatures, more than half the black hole evaporation power is emitted in relativistic color-charged particles [71,72].…”

Section: Black Hole Evaporative Ignition Of White Dwarfsmentioning

confidence: 99%

Supernovae sparked by dark matter in white dwarfs

Acevedo

Bramante

2019

Phys. Rev. D

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“…• Hawking Evaporation: the last term in eq. (4.15) is the rate at which BH loses masses through hawking evaporation It is not impossible that these bounds may be slightly relaxed from the fact that when the BH evaporates there might be also at this stage a Fermi sea suppression effect at work [48], a possibility we will not look at.…”

Section: Jcap05(2019)035mentioning

confidence: 99%

New analysis of neutron star constraints on asymmetric dark matter

Garani

Génolini

Hambye

2019

J. Cosmol. Astropart. Phys.

113

165

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Due to their extreme density and low temperature, neutron stars (NS) are efficient probes to unveil interactions between standard model and dark matter (DM) particles. From elastic scatterings on NS material, DM can get gravitationally trapped by the star. The cooling of DM through further collisions may lead to the formation of a dense core which could collapse into a black hole, thus destroying the whole NS. From the observation of old NS, such a scenario leads to very stringent constraints on the parameter space of asymmetric DM. In this work we reexamine this possibility in detail. This includes: (a) a new detailed determination of the number of DM particles captured, properly taking into account the fact that neutrons form a highly degenerate Fermi material; (b) the determination of the time evolution of the DM density and energy profiles inside the NS, which allows us to understand how, as a function of time, DM thermalizes with NS material; (c) the determination of the corresponding constraints which hold on the DM-neutron cross section, including for the case where a large fraction of DM particles have not thermalized; (d) the first determination of the stringent constraints which also hold in a similar way on the DM-muon cross section, particularly relevant for leptophilic DM models; and (e) the use of realistic NS equations of state in determining these constraints. * Electronic address: rgaranir@ulb.ac.be † Electronic address: yoann.genolini@ulb.ac.be ‡ Electronic address: thambye@ulb.ac.be arXiv:1812.08773v1 [hep-ph] Note that small momentum dependence in the cross section has been ignored. For scalar interactions, i.e. L int ⊃the cross sections are dσ χ−f d cos θcm = G 2 S 8π m 2 f (mχ+m f ) 2 and dσ χ−f d cos θcm = G 2 S 2π m 2 χ m 2 f (mχ+m f ) 2 ,

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“…Thus far, the treatment of NS material accretion onto a BH at the core of a NS has followed the assumption that accretion proceeds through a spherical Bondi-Hoyle process, possibly including caveats from the NS rotation [14] or from Pauli blocking [15] (see also Ref. [16,17] for numerical studies of the full general relativistic problem of black hole evolution, but also assuming Bondi accretion).…”

Section: Introductionmentioning

confidence: 99%

Neutron Star Quantum Death by Small Black Holes

Giffin,

Lloyd,

McDermott

et al. 2021

Preprint

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Neutron stars can be destroyed by black holes at their center accreting material and eventually swallowing the entire star. Here we note that the accretion model adopted in the literature, based on Bondi accretion or variations thereof, is inadequate for small black holes -black holes whose Schwarzschild radius is comparable to, or smaller than, the neutron's de Broglie wavelength. In this case, quantum mechanical aspects of the accretion process cannot be neglected, and give rise to a completely different accretion rate. We show that for the case of black holes seeded by the collapse of bosonic dark matter, this is the case for electroweak-scale dark matter particles. In the case of fermionic dark matter, typically the black holes that would form at the center of a neutron star are more massive, unless the dark matter particle mass is very large, larger than about 10 10 GeV. We calculate the lifetime of neutron stars harboring a "small" black hole, and find that black holes lighter than ∼ 10 11 kg quickly evaporate, leaving no trace. More massive black holes destroy neutron stars via quantum accretion on time-scales much shorter than the age of observed neutron stars.

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Blocking the Hawking radiation

Cited by 5 publications

References 48 publications

Supernovae sparked by dark matter in white dwarfs

Supernovae sparked by dark matter in white dwarfs

New analysis of neutron star constraints on asymmetric dark matter

Neutron Star Quantum Death by Small Black Holes

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