Nucleus capture by macroscopic dark matter

Bai, Y.; Berger, Joshua

doi:10.1007/jhep05(2020)160

Cited by 29 publications

(34 citation statements)

References 30 publications

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“…For a white dwarf, the situation is simpler as they are not expected to be superconducting. Similar to the case for the Sun or a color superconducting neutron star core, annihilation quickly equilibrates with capture at N crit * • , with 17) taking the white dwarf magnetic field to be B 6 × 10 6 gauss and the density to be ρ c ∼ 10 6 g/cm 3 . The annihilation rate is then…”

Section: Jhep10(2020)210mentioning

confidence: 93%

“…As discussed in appendix A, baryons that enter an EWS corona become 2d modes and can be easily captured by the PMBH. For example, if R EW 1 GeV −1 corresponding to Q 10 4 , then baryon bound states are expected [17]. The PMBH can then reemit energy as Hawking radiation, which need not have the same baryon number.…”

Section: Non-extremal Magnetic Black Holesmentioning

confidence: 99%

“…[11][12][13][14][15]. Other objects with macroscopic EW-symmetric (EWS) regions have been studied in [16][17][18].…”

Section: Introductionmentioning

confidence: 99%

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Phenomenology of magnetic black holes with electroweak-symmetric coronas

Bai

Berger

Korwar

et al. 2020

J. High Energ. Phys.

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Magnetically charged black holes (MBHs) are interesting solutions of the Standard Model and general relativity. They may possess a “hairy” electroweak-symmetric corona outside the event horizon, which speeds up their Hawking radiation and leads them to become nearly extremal on short timescales. Their masses could range from the Planck scale up to the Earth mass. We study various methods to search for primordially produced MBHs and estimate the upper limits on their abundance. We revisit the Parker bound on magnetic monopoles and show that it can be extended by several orders of magnitude using the large-scale coherent magnetic fields in Andromeda. This sets a mass-independent constraint that MBHs have an abundance less than 4 × 10−4 times that of dark matter. MBHs can also be captured in astrophysical systems like the Sun, the Earth, or neutron stars. There, they can become non-extremal either from merging with an oppositely charged MBH or absorbing nucleons. The resulting Hawking radiation can be detected as neutri- nos, photons, or heat. High-energy neutrino searches in particular can set a stronger bound than the Parker bound for some MBH masses, down to an abundance 10−7 of dark matter.

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Section: Jhep10(2020)210mentioning

confidence: 93%

Section: Non-extremal Magnetic Black Holesmentioning

confidence: 99%

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Phenomenology of magnetic black holes with electroweak-symmetric coronas

Bai

Berger

Korwar

et al. 2020

J. High Energ. Phys.

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“…Concrete charged macro formation models include macros formed from the mechanisms described for neutral macros, e.g. thos described in references [6,7,35], that then acquire a charged by absorbing nuclei during their lifetime. Such a possible mechanism for absorbing additional nuclei is described in reference [35].…”

Section: Introductionmentioning

confidence: 99%

“…thos described in references [6,7,35], that then acquire a charged by absorbing nuclei during their lifetime. Such a possible mechanism for absorbing additional nuclei is described in reference [35]. Indeed, if a macro consists of a bound state of nuclei, it is plausible that a collision with a nucleus could result in the absorption of that nucleus, thus increasing the net charge of the macro.…”

Section: Introductionmentioning

confidence: 99%

Charge constraints of macroscopic dark matter

Sidhu

2020

Phys. Rev. D

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Macroscopic dark matter (macros) refers to a broad class of alternative candidates to particle dark matter with still unprobed regions of parameter space. Prior work on macros has considered elastic scattering to be the dominant energy transfer mechanism in deriving constraints on the abundance of macros for some range of masses Mx and (geometric) cross-sections σx However, macros with a significant amount of electric charge would, through Coulomb interactions, interact strongly enough to have produced observable signals on terrestrial, galactic and cosmological scales. We determine the expected phenomenological signals and constrain the corresponding regions of parameter space, based on the lack of these signals in observations.

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Q-monopole-ball: a topological and nontopological soliton

Bai

Orlofsky

2022

J. High Energ. Phys.

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Magnetic monopoles and Q-balls are examples of topological and nontopological solitons, respectively. A new soliton state with both topological and nontopological charges is shown to also exist, given a monopole sector with a portal coupling to an additional scalar field S with a global U(1) symmetry. This new state, the Q-monopole-ball, is more stable than an isolated Q-ball made of only S particles, and it could be stable against fissioning into monopoles and free S particles. Stable Q-monopole-balls can contain large magnetic charges, providing a novel nongravitational mechanism for binding like-charged monopoles together. They could be produced from a phase transition in the early universe and account for all dark matter.

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Nucleus capture by macroscopic dark matter

Cited by 29 publications

References 30 publications

Phenomenology of magnetic black holes with electroweak-symmetric coronas

Phenomenology of magnetic black holes with electroweak-symmetric coronas

Charge constraints of macroscopic dark matter

Q-monopole-ball: a topological and nontopological soliton

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