Neutrino Astrophysics with the ANTARES Telescope by Vladimir Kulikovskiy

Author:Vladimir Kulikovskiy
Language: eng
Format: epub
Publisher: Springer International Publishing, Cham

6.All particles are tracked inside the can. Tracking assumes the energy losses calculation, interactions and light emission. For the events outside the can only muons with tracks intersecting the can are propagated till the can surface and then tracked.

7.For events which are kept the event weight is calculated.

Neutrino event weight calculation includes the probability of neutrino absorption in the Earth. This probability depends on the density of matter along its path and the neutrino interactions cross-section. To good approximation, the Earth may be regarded as a sphere with a complex internal structure consisting of a dense inner and outer core and a lower mantle of medium density, covered by a transition zone, lid, crust, and oceans. Density profile of the Earth is taken from the Preliminary Earth Model (Gandhi et al. 1996).

For , a charged-current interaction in the Earth far from the detector leads to the loss of the neutrino event. However, for the the situation is more complicated since the produced tau decays on the flight with a production of . This leads to the so-called regeneration chain thanks to which is never absorbed. The energy losses due to the propagation through the Earth lead to a pile-up of tau neutrinos at the energies lower than the neutrino’s energy at the Earth surface. Moreover, a tau can decay via muonic channel () or via electronic channel () with a production of secondary neutrinos. Neutral charged-current interaction cross-sections are lower than the charged-current cross-sections, however they can not be neglected, especially when searching for cascade-like events. These processes reduce the energy of the neutrinos passed through the Earth and increase the probability of this passage since the probability depends on the neutrino energy. All these processes are reproduced in GENHEN.

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