BEGIN:VCALENDAR VERSION:2.0 PRODID:-//linuxsoftware.nz//NONSGML Joyous v1.4//EN BEGIN:VEVENT SUMMARY:Primordial Black Holes as laboratories for Physics beyond the stan dard scenarios DTSTART:20221018T143000Z DTEND:20221018T163000Z DTSTAMP:20260928T032144Z UID:c6a5f966-f224-43ce-bece-ff25667a87ba SEQUENCE:3 CREATED:20221014T131713Z DESCRIPTION:Abstract:We use the evaporation of primordial black holes (PBH s)\, of mass between 10^8 -10^12 kg\, as a laboratory to investigate Physi cs beyond the Standard Model of particles and to probe the structure of bl ack holes.We show that PBHs develop non-negligible spins through Hawking&# x27\;s emission of a large number of axion-like particles generically pres ent in string theory compactifications. This is because scalars can be emi tted in the monopole mode (l = 0)\, where no angular momentum is removed f rom the BH\, so a sufficiently large number of scalars can compensate for the spin-down produced by fermion\, gauge boson\, and graviton emission. T his yields a unique probe of the total number of light scalars in the fund amental theory\, independent of how weakly they interact with known matter .We propose a method to determine the mass and spin of PBHs based on measu ring the energy of specific features in the photon Hawking emission spectr um\, including both primary and secondary components. Since the proposed m ethod relies on the energy of the photons emitted by a given PBH\, rather than on the associated flux\, it is independent of the PBH-Earth distance and\, as a byproduct\, can also be used to infer the latter.We study a reg ular rotating black hole\, described by the Kerr-black-bounce metric\, eva porating under the Hawking emission of a single scalar field. We compare t he results with a Kerr black hole evaporating under the same conditions. T he Gray-body factors\, the asymptotic final spin\, the surface gravity\, a nd as a consequence temperature\, primary emissivity\, and lifetime\, are affected by the regularizing parameter. We briefly comment on the possibil ity of investigating the beyond-the-horizon structure of a black hole expl oiting its Hawking emission. LAST-MODIFIED:20221014T131808Z LOCATION:Sala de Seminários do DF\, Pavilhão de Física\, 2º piso URL:http://df.vps.tecnico.ulisboa.pt/pt/eventos/primordial-black-holes-as- laboratories-for-physics-beyond-the-standard-scenarios/ X-ALT-DESC;FMTTYPE=text/html:

Abstract:

We use the evaporation of primordial black hole s (PBHs)\, of mass between 10^8 -10^12 kg\, as a laboratory to investigate Physics beyond the Standard Model of particles and to probe the structure of black holes.


We show that PBHs develop non-negligible spins through Hawking'\;s emission of a large n umber of axion-like particles generically present in string theory compact ifications. This is because scalars can be emitted in the monopole mode (l = 0)\, where no angular momentum is removed from the BH\, so a sufficient ly large number of scalars can compensate for the spin-down produced by fe rmion\, gauge boson\, and graviton emission. This yields a unique probe of the total number of light scalars in the fundamental theory\, independent of how weakly they interact with known matter.


We propose a method to determine the mass and spin of PBHs bas ed on measuring the energy of specific features in the photon Hawking emis sion spectrum\, including both primary and secondary components. Since the proposed method relies on the energy of the photons emitted by a given PB H\, rather than on the associated flux\, it is independent of the PBH-Eart h distance and\, as a byproduct\, can also be used to infer the latter.


We study a regular rotating black hol e\, described by the Kerr-black-bounce metric\, evaporating under the Hawk ing emission of a single scalar field. We compare the results with a Kerr black hole evaporating under the same conditions.

The Gray-body factors\, the asymptotic final spin\, the surface gravity\, and as a conse quence temperature\, primary emissivity\, and lifetime\, are affected by t he regularizing parameter. We briefly comment on the possibility of invest igating the beyond-the-horizon structure of a black hole exploiting its Ha wking emission.

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