Determining the spin of light primordial black holes with Hawking radiation

Calzà, Marco; Rosa, João G.

doi:10.1007/jhep12(2022)090

Cited by 5 publications

(1 citation statement)

References 79 publications

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“…Another consideration is if the PBH initially rotates rapidly. While most past work argues for small PBH spins at formation (e.g., De Luca et al 2019), some calculations predict that PBHs near the classical evaporation limit may be spun up by emitting Hawking radiation, suggesting that the smallest PBHs may have large spins initially (Calzà & Rosa 2022).…”

Section: What Is the Growth Rate And Radiative Efficiency Of Amentioning

confidence: 99%

Solar Evolution Models with a Central Black Hole

Bellinger,

Caplan,

Ryu

et al. 2023

ApJ

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Hawking proposed that the Sun may harbor a primordial black hole (BH) whose accretion supplies some of the solar luminosity. Such an object would have formed within the first 1 s after the Big Bang with the mass of a moon or an asteroid. These light BHs are a candidate solution to the dark matter problem, and could grow to become stellar-mass BHs if captured by stars. Here we compute the evolution of stars having such a BH at their center. We find that such objects can be surprisingly long-lived, with the lightest BHs having no influence over stellar evolution, while more massive ones consume the star over time to produce a range of observable consequences. Models of the Sun born about a BH whose mass has since grown to approximately 10−6 M ⊙ are compatible with current observations. In this scenario, the Sun would first dim to half its current luminosity over a span of 100 Myr as the accretion starts to generate enough energy to quench nuclear reactions. The Sun would then expand into a fully convective star, where it would shine luminously for potentially several gigayears with an enriched surface helium abundance, first as a sub-subgiant star, and later as a red straggler, before becoming a subsolar-mass BH. We also present results for a range of stellar masses and metallicities. The unique internal structures of stars harboring BHs may make it possible for asteroseismology to discover them, should they exist. We conclude with a list of open problems and predictions.

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Section: What Is the Growth Rate And Radiative Efficiency Of Amentioning

confidence: 99%

Solar Evolution Models with a Central Black Hole

Bellinger,

Caplan,

Ryu

et al. 2023

ApJ

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Primordial black hole superradiance and evaporation in the string axiverse

Calzà,

Rosa,

Serrano

2024

J. High Energ. Phys.

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In the string axiverse scenario, light primordial black holes may spin up due to the Hawking emission of a large number of light (sub-MeV) axions. We show that this may trigger superradiant instabilities associated with a heavier axion during the black holes’ evolution, and study the coupled dynamics of superradiance and evaporation. We find, in particular, that the present black hole mass-spin distribution should follow the superradiance threshold condition for black hole masses below the value at which the superradiant cloud forms, for a given heavy axion mass. Furthermore, we show that the decay of the heavy axions within the superradiant cloud into photon pairs may lead to a distinctive line in the black hole’s emission spectrum, superimposed on its electromagnetic Hawking emission.

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Determining the spin of light primordial black holes with Hawking radiation. Part II. High spin regime

Calzà,

Rosa

2024

J. High Energ. Phys.

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We propose a method to determine the mass and spin of primordial black holes based on measuring the energy and emission rate at the dipolar and quadrupolar peaks in the primary photon Hawking spectrum, applicable for dimensionless spin parameters $$ \overset{\sim }{a} $$ a ~ ≳ 0.6. In particular, we show that the ratio between the energies of the two peaks is only a function of the black hole spin, while the ratio between their emission rates depends also on the line-of-sight inclination. The black hole mass and distance from the Earth may then be inferred from the absolute values of the peak energies and emission rates. This method is relevant for primordial black holes born with large spin parameters that are presently still in the early stages of their evaporation process. While Hawking radiation from such black holes is somewhat below the reach of planned gamma-ray telescopes, we expect the required sensitivity to be attained in the not too distant future.

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Determining the spin of light primordial black holes with Hawking radiation

Cited by 5 publications

References 79 publications

Solar Evolution Models with a Central Black Hole

Solar Evolution Models with a Central Black Hole

Primordial black hole superradiance and evaporation in the string axiverse

Determining the spin of light primordial black holes with Hawking radiation. Part II. High spin regime

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