Seasonal Variation of Atmospheric Muons. (arXiv:2107.12913v1 [astro-ph.HE])
<a href="http://arxiv.org/find/astro-ph/1/au:+Gaisser_T/0/1/0/all/0/1">Thomas Gaisser</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Verpoest_S/0/1/0/all/0/1">Stef Verpoest</a>

Competition between decay and re-interaction of charged pions and kaons
depends on the temperature/density profile of the upper atmosphere. The
amplitude and phase of the variations depend on the minimum muon energy
required to reach the detector and on muon multiplicity in the detector. Here
we compare different methods for characterizing the muon production profile and
the corresponding effective temperature. A muon production profile based on a
parameterization of simulations of muons as a function of primary energy is
compared with approximate analytic solutions of the cascade equation integrated
over primary energy. In both cases, we compare two definitions of effective
temperature. We emphasize applications to compact underground detectors like
MINOS and OPERA, while indicating how they relate to extended detectors like
IceCube.

Competition between decay and re-interaction of charged pions and kaons
depends on the temperature/density profile of the upper atmosphere. The
amplitude and phase of the variations depend on the minimum muon energy
required to reach the detector and on muon multiplicity in the detector. Here
we compare different methods for characterizing the muon production profile and
the corresponding effective temperature. A muon production profile based on a
parameterization of simulations of muons as a function of primary energy is
compared with approximate analytic solutions of the cascade equation integrated
over primary energy. In both cases, we compare two definitions of effective
temperature. We emphasize applications to compact underground detectors like
MINOS and OPERA, while indicating how they relate to extended detectors like
IceCube.

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