A Clinical Application of Fuzzy Logic

Torshabi, Ahmad Esmaili; Riboldi, Marco; Pella, Andera; Negarestani, Ali; Rahnema, Mohamad; Baroni, Guido

doi:10.5772/35737

Cited by 3 publications

(3 citation statements)

References 40 publications

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“…And χ comprises the bulk of present-day dark matter. The lifetime for the decay of heavy dark matter to standard model (SM from now on) particles is strongly constrained (τ ≥ O(10 26 − 10 29 )s) by diffuse gamma and neutrino observations [Esmaili, Ibarra & Peres 2012, Murase & Beacom 2012, Rott,Kohri & Park 2015, Kachelriess,Kalashev & Kuznetsov 2018. In the present work, it is considered an assumption that superheavy dark matter could not decay to SM particles.…”

Section: Uhe Wimps Flux In the Galaxymentioning

confidence: 99%

“…And τ φ is taken to be 10 25 s. Since the WIMP flux only depends on the two-body decay of superheavy dark matter and the dark matter distribution in the galactic halo, it is the same as the neutrino flux due to the decay of superheavy dark matter in Ref. [Esmaili, Ibarra & Peres 2012, Bai, Lu & Salvado 2016:…”

Section: Uhe Wimps Flux In the Galaxymentioning

confidence: 99%

“…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%

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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: Uhe Wimps Flux In the Galaxymentioning

confidence: 99%

Section: Uhe Wimps Flux In the Galaxymentioning

confidence: 99%