Baryogenesis and Leptogenesis

Dev, P. S. Bhupal

doi:10.1007/978-3-030-29622-3_40

Cited by 2 publications

(2 citation statements)

References 33 publications

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“…This superheavy dark matter [Khlopov & Chechetkin 1987, Chung, Kolb & Riotto 1998,Chung, Kolb & Riotto 1999,Covi et al 2010,Feldstein et al 2013 decays to another much lighter WIMPs χ and its lifetime is greater than the age of the Universe. This lead to a small but significant flux of UHE WIMPs [Li & Tao 2000,Bhattacharya, Gandhi & Gupta 2015,Esmaili, Ibarra & Peres 2012, Bai, Lu & Salvado 2016, Bhupal et al 2016].…”

Section: Introductionmentioning

confidence: 99%

Direct Detection of Ultrahigh-energy WIMPs with a Satellite Detector Like JEM-EUSO

2019

ApJ

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The possibility of directly detecting Ultra-high energy (UHE from now on) WIMPs are considered by the WIMPs interaction with the nuclei in the air. Since neutrinos dominate the events from the spherical crown near JEM-EUSO, all the events from this region are ignored in my work. Then the numbers of UHE WIMPs and neutrino detected by JEM-EUSO are evaluated at different energies (1 PeV < E < 100 EeV) in ten years, respectively. If the energy thresholds are taken to be 20 EeV, neutrino events can be almost rejected in the detection of UHE WIMPs. According to my evaluation, O(10-100) UHE WIMP events can be detected by JEM-EUSO at energies above 20 EeV in ten years.

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Section: Introductionmentioning

confidence: 99%

Direct Detection of Ultrahigh-energy WIMPs with a Satellite Detector Like JEM-EUSO

2019

ApJ

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“…This lead to a small but significant flux of UHE SM particles. In the present work, it is only focused on detection of the UHE neutrinos induced by the decay of superheavy dark matter φ (φ → ν ν) [16][17][18][19]. Although the fraction of these relativistic neutrinos is small in the Universe, their large interaction cross sections between them and other SM particles make it possible to find them.…”

Section: Introductionmentioning

confidence: 99%

Detection of Ultra-High Energy neutrinos skimming the Earth due to decay of superheavy dark matter at JEM-EUSO

2019

Physics of the Dark Universe

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The possibility of detecting Ultra-high energy (UHE from now on) neutrinos due to superheavy dark matter are considered by the neutrinos interaction with the nuclei in the air in the present paper. To reject other standard model particles, UHE neutrinos, from superheavy dark matter and astrophysical sources, skimming the Earth are detected at JEM-EUSO. Then the numbers of UHE neutrinos detected by JEM-EUSO are evaluated at different energies (1 EeV < E < 1 ZeV) in 5 years. If the energy thresholds are taken to be 100 EeV, the astrophysical neutrino contamination could be negligible in this detection. It is possible that UHE neutrinos from the decay of superheavy dark matter are detected at JEM-EUSO when O(10 27 )s < τ φ < O(10 31 )s. For example, O(10 4 ) UHE neutrino events could be detected by JEM-EUSO at 30 EeV in 5 years when τ φ = O(10 27 )s. If so, it may be confirmed that there may exist superheavy dark matter in the Universe.

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Baryogenesis and Leptogenesis

Cited by 2 publications

References 33 publications

Direct Detection of Ultrahigh-energy WIMPs with a Satellite Detector Like JEM-EUSO

Direct Detection of Ultrahigh-energy WIMPs with a Satellite Detector Like JEM-EUSO

Detection of Ultra-High Energy neutrinos skimming the Earth due to decay of superheavy dark matter at JEM-EUSO

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