Primordial Black Holes: Observational characteristics of the final evaporation

Ukwatta, T. N.; Stump, Dan; Linnemann, J.; MacGibbon, Jane H.; Marinelli, S. S.; Yapici, T.; Tollefson, K.

doi:10.1016/j.astropartphys.2016.03.007

Cited by 60 publications

(80 citation statements)

References 50 publications

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“…Figure 3(a) is compatible with the equivalent figure in Ukwatta et al [17] but they are interested in the higher energies associated with the final black hole burst. q .…”

Section: B Instantaneous Primary and Secondary Emissionsupporting

confidence: 75%

“…However, this last step is smaller (a factor of 2 instead of 4) and it is not relevant to later considerations, so we neglect it below. An equivalent figure has been derived by Ukwatta et al [17]. …”

Section: Black Hole Gamma-ray Emissionmentioning

confidence: 99%

“…PBHs completing their evaporation today have m = 0 and therefore an initial mass 17) where the small correction 0.017 differs from the correction 0.020 in Eq. (2.12) by the factor 1 − α −1 ≈ 3/4.…”

Section: Black Hole Gamma-ray Emissionmentioning

confidence: 99%

See 2 more Smart Citations

Constraints on primordial black holes from the Galactic gamma-ray background

Carr¹,

Kohri²,

Sendouda³

et al. 2016

Phys. Rev. D

144

152

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The fraction of the Universe going into primordial black holes (PBHs) with initial mass M * ≈ 5 × 10 14 g , such that they are evaporating at the present epoch, is strongly constrained by observations of both the extragalactic and Galactic gamma-ray backgrounds. However, while the dominant contribution to the extragalactic background comes from the time-integrated emission of PBHs with initial mass M * , the Galactic background is dominated by the instantaneous emission of those with initial mass slightly larger than M * and current mass below M * . Also, the instantaneous emission of PBHs smaller than 0.4 M * mostly comprises secondary particles produced by the decay of directly emitted quark and gluon jets. These points were missed in the earlier analysis by Lehoucq et al. using EGRET data. For a monochromatic PBH mass function, with initial mass (1 + µ) M * and µ ≪ 1, the current mass is (3µ) 1/3 M * and the Galactic background constrains the fraction of the Universe going into PBHs as a function of µ . However, the initial mass function cannot be precisely monochromatic and even a tiny spread of mass around M * would generate a current lowmass tail of PBHs below M * . This tail would be the main contributor to the Galactic background, so we consider its form and the associated constraints for a variety of scenarios with both extended and nearly-monochromatic initial mass functions. In particular, we consider a scenario in which the PBHs form from critical collapse and have a mass function which peaks well above M * . In this case, the largest PBHs could provide the dark matter without the M * ones exceeding the gamma-ray background limits.

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“…Figure 3(a) is compatible with the equivalent figure in Ukwatta et al [17] but they are interested in the higher energies associated with the final black hole burst. q .…”

Section: B Instantaneous Primary and Secondary Emissionsupporting

confidence: 75%

Section: Black Hole Gamma-ray Emissionmentioning

confidence: 99%

See 1 more Smart Citation

Constraints on primordial black holes from the Galactic gamma-ray background

Carr¹,

Kohri²,

Sendouda³

et al. 2016

Phys. Rev. D

144

152

View full text Add to dashboard Cite

show abstract

“…lower black hole mass), the temperature of black hole is still higher and the tabulated data in [57] is sufficient. We have used the primary black hole spectrum with the absorption coefficient Γ s (E, s, M BH ) provided in [56]. We have taken into account the change in the mass of the black hole (and therefore its evolving temperature and emitted instantaneous power) as it evaporates.…”

Section: Calculations and Resultsmentioning

confidence: 99%

CMB spectral distortions constraints on primordial black holes, cosmic strings and long lived unstable particles revisited

Acharya

Khatri

2020

J. Cosmol. Astropart. Phys.

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We calculate the spectral distortions from Hawking evaporation of primordial black holes before the epoch of recombination, taking into account emission of all standard model particles, including quark and gluons, and evolving the resulting particle cascades in the expanding Universe. We show that the constraints on the abundance of primordial black holes are stronger by more than an order of magnitude compared to the previous calculations which take only the primary photon emission into account. We also show that the shapes of the spectral distortions is different from the y or i-type distortions and are sensitive to the mass of the primordial black holes. We also extend previous constraints on the decay of long lived unstable particles before recombination to additional decay channels. We show that for dark matter mass 1 GeV, the spectral distortion shape is a function of the dark matter mass as well as the decay channel to standard model particles. We also provide new spectral distortion constraints on superconducting cosmic string decay. We explicitly show that consideration of emitted photon spectrum from string decay is not only important for the future experiments but also for already available COBE-FIRAS data.

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“…Detailed calculation [57] finds α ≈ 2.8 · 10 −4 for T BH MeV, accounting for emission of photons, gravitons, and three neutrino species. Counting only experimentally verified SM degrees of freedom, the emission rate effectively asymptotes to α ≈ 4.1 · 10 −3 for T BH 100 GeV [58]. Thus an evaporating BH (by this we mean a BH which only Hawking radiates without any accretion) 5 has a lifetime less than τ WD ≈ 5 Gyr if:…”

Section: A Fate Of a Bhmentioning

confidence: 98%

Type Ia supernovae from dark matter core collapse

2019

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Dark matter (DM) which sufficiently heats a local region in a white dwarf will trigger runaway fusion, igniting a type Ia supernova (SN). In a companion paper, this instability was used to constrain DM heavier than 10 16 GeV which ignites SN through the violent interaction of one or two individual DM particles with the stellar medium. Here we study the ignition of supernovae by the formation and self-gravitational collapse of a DM core containing many DM particles. For non-annihilating DM, such a core collapse may lead to a mini black hole that can ignite SN through the emission of Hawking radiation, or possibly as a by-product of accretion. For annihilating DM, core collapse leads to an increasing annihilation rate and can ignite SN through a large number of rapid annihilations. These processes extend the previously derived constraints on DM to masses as low as 10 5 GeV.

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Primordial Black Holes: Observational characteristics of the final evaporation

Cited by 60 publications

References 50 publications

Constraints on primordial black holes from the Galactic gamma-ray background

Constraints on primordial black holes from the Galactic gamma-ray background

CMB spectral distortions constraints on primordial black holes, cosmic strings and long lived unstable particles revisited

Type Ia supernovae from dark matter core collapse

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