Type Ia supernovae from dark matter core collapse

Janish, Ryan; Narayan, Vijay; Riggins, Paul

doi:10.1103/physrevd.100.035008

Cited by 54 publications

(64 citation statements)

References 70 publications

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“…2. For dark matter masses in excess of 10 10 GeV, we believe our results differ from [63], because we have accounted for white dwarf structural suppression of dark matter-nuclear scattering at low momentum transfers, as given by Eq. (15) and surrounding text.…”

Section: Discussioncontrasting

confidence: 62%

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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: Discussioncontrasting

confidence: 62%

“…Note added: Shortly after this work appeared on the arxiv, another paper appeared [63] with some overlap, which identified a viscous dark matter thermalization regime. This version of our article has been updated to account for viscous thermalization, as discussed in Sec.…”

Section: Discussionmentioning

confidence: 99%

Supernovae sparked by dark matter in white dwarfs

Acevedo

Bramante

2019

Phys. Rev. D

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“…Our results will require the reinterpretation of a large and varied body of work, e.g., Refs. [43,46,48,49,[66][67][68][69][70][71][72][73][74][75][76][77][78][79][82][83][84][85][86][87][88][89][90][91][92].…”

Section: Introductionmentioning

confidence: 99%

Not as big as a barn: Upper bounds on dark matter-nucleus cross sections

et al. 2019

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Critical probes of dark matter come from tests of its elastic scattering with nuclei. The results are typically assumed to be model independent, meaning that the form of the potential need not be specified and that the cross sections on different nuclear targets can be simply related to the cross section on nucleons. For pointlike spin-independent scattering, the assumed scaling relation is σ χA ∝ A 2 μ 2 A σ χN ∝ A 4 σ χN , where the A 2 comes from coherence and the μ 2 A ≃ A 2 m 2 N from kinematics for m χ ≫ m A. Here we calculate where model independence ends, i.e., where the cross section becomes so large that it violates its defining assumptions. We show that the assumed scaling relations generically fail for dark matter-nucleus cross sections σ χA ∼ 10 −32-10 −27 cm 2 , significantly below the geometric sizes of nuclei and well within the regime probed by underground detectors. Last, we show on theoretical grounds, and in light of existing limits on light mediators, that pointlike dark matter cannot have σ χN ≳ 10 −25 cm 2 , above which many claimed constraints originate from cosmology and astrophysics. The most viable way to have such large cross sections is composite dark matter, which introduces significant additional model dependence through the choice of form factor. All prior limits on dark matter with cross sections σ χN > 10 −32 cm 2 with m χ ≳ 1 GeV must therefore be reevaluated and reinterpreted.

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“…Others have calculated the effect of this accumulated dark matter on cooling of celestial objects [34][35][36][37], or have compared the dark luminosity with the observed luminosity to provide stringent constraints on dark matter interactions with SM particles [35,38,39]. More recently, limits on DM-nucleon cross section have also been obtained from non-observation of collapse of massive white dwarfs [40] or from neutron star heating [41][42][43][44].…”

Section: Introductionmentioning

confidence: 99%

Dark matter capture in celestial objects: improved treatment of multiple scattering and updated constraints from white dwarfs

Dasgupta

Gupta

Ray

2019

J. Cosmol. Astropart. Phys.

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We revisit dark matter (DM) capture in celestial objects, including the impact of multiple scattering, and obtain updated constraints on the DM-proton cross section using observations of white dwarfs. Considering a general form for the energy loss distribution in each scattering, we derive an exact formula for the capture probability through multiple scatterings. We estimate the maximum number of scatterings that can take place, in contrast to the number required to bring a dark matter particle to rest. We employ these results to compute a "dark" luminosity L DM , arising solely from the thermalized annihilation products of the captured dark matter. Demanding that L DM not exceed the luminosity of the white dwarfs in the M4 globular cluster, we set a bound on the DM-proton cross section: σ p 10 −44 cm 2 , almost independent of the dark matter mass between 100 GeV and 1 PeV and mildly weakening beyond. This is a stronger constraint than those obtained by direct detection experiments in both large mass (M 5 TeV) and small mass (M 10 GeV) regimes. For dark matter lighter than 350 MeV, which is beyond the sensitivity of present direct detection experiments, this is the strongest available constraint.

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Type Ia supernovae from dark matter core collapse

Cited by 54 publications

References 70 publications

Supernovae sparked by dark matter in white dwarfs

Supernovae sparked by dark matter in white dwarfs

Not as big as a barn: Upper bounds on dark matter-nucleus cross sections

Dark matter capture in celestial objects: improved treatment of multiple scattering and updated constraints from white dwarfs

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