Directly search for Ultra-High Energy WIMPs at IceCube. (arXiv:1811.09793v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Xu_Y/0/1/0/all/0/1">Ye Xu</a>
I study the possibility of directly detecting Ultra-high energy (UHE from now
on) WIMPs by the IceCube experiment, via the WIMPs interaction with the nuclei
in the ice. I evaluate galactic and extragalactic UHE WIMP and astrophysical
and atmospheric neutrino event rates at energy range of 10 TeV – 10 PeV. I
assume UHE WIMPs $chi$ are only from the decay of superheavy dark matter
$phi$, that is $phitochibar{chi}$. If the lifetime of superheavy dark
matter $tau_{phi}$ is taken to be $5times10^{21}$, WIMPs can be detected at
energies above $sim$50TeV in this detection. Since UHE WIMP fluxes are
actually depended on $tau_{phi}$, if superheavy dark matter can decay to
standard model particles (that is $tau_{phi}$ is constrained to be larger
than O($10^{26}$-$10^{28}$)s), according to my work, UHE WIMPs could not be
detected by IceCube.
I study the possibility of directly detecting Ultra-high energy (UHE from now
on) WIMPs by the IceCube experiment, via the WIMPs interaction with the nuclei
in the ice. I evaluate galactic and extragalactic UHE WIMP and astrophysical
and atmospheric neutrino event rates at energy range of 10 TeV – 10 PeV. I
assume UHE WIMPs $chi$ are only from the decay of superheavy dark matter
$phi$, that is $phitochibar{chi}$. If the lifetime of superheavy dark
matter $tau_{phi}$ is taken to be $5times10^{21}$, WIMPs can be detected at
energies above $sim$50TeV in this detection. Since UHE WIMP fluxes are
actually depended on $tau_{phi}$, if superheavy dark matter can decay to
standard model particles (that is $tau_{phi}$ is constrained to be larger
than O($10^{26}$-$10^{28}$)s), according to my work, UHE WIMPs could not be
detected by IceCube.
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