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arXiv 1605.01409hep-phastro-ph.HE
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粲对大气中微子通量的贡献

On the Charm Contribution to the Atmospheric Neutrino Flux

Francis Halzen, Logan Wille

备注：
arXiv admin note: text overlap with arXiv:1601.03044
发表信息：
Phys. Rev. D 94, 014014 (2016)
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摘要：

我们重新估计的魅力粒子贡献的大气中微子通量，预计将占主导地位的高能量，因为长寿命的高能π介子和K介子在大气中相互作用，然后衰变成中微子。我们专注于生产向前的魅力粒子进行了很大一部分的入射质子的动量。在奇异粒子的情况下，这样的成分是从大量产生的$K^{+} Λ$对中熟悉的。这些前向粲粒子可以在地下实验中主导高能大气中微子通量。现代对撞机实验没有覆盖在非常大的快度区，其中魅力向前对生产占主导地位。使用档案加速器数据以及IceCube测量的大气电子和μ子中微子通量，我们得到了上限的前向$\bar{D}^0 Λ_c$对生产和高能大气中微子的相关通量。我们的结论是，提示通量可能占主导地位的研究中心的组成部分，并代表了一个显着的贡献TeV的大气中微子通量。重要的是，它不能容纳高能宇宙中微子的PeV通量，也不能容纳IceCube在30- 200 TeV能量范围内观察到的过量事件，这表明宇宙加速器的通量中存在结构，或者观察到的宇宙通量中存在不止一种成分。

英文摘要：

We revisit the estimate of the charm particle contribution to the atmospheric neutrino flux that is expected to dominate at high energies because long-lived high-energy pions and kaons interact in the atmosphere before decaying into neutrinos. We focus on the production of forward charm particles which carry a large fraction of the momentum of the incident proton. In the case of strange particles, such a component is familiar from the abundant production of $K^{+} Λ$ pairs. These forward charm particles can dominate the high-energy atmospheric neutrino flux in underground experiments. Modern collider experiments have no coverage in the very large rapidity region where charm forward pair production dominates. Using archival accelerator data as well as IceCube measurements of atmospheric electron and muon neutrino fluxes, we obtain an upper limit on forward $\bar{D}^0 Λ_c$ pair production and on the associated flux of high-energy atmospheric neutrinos. We conclude that the prompt flux may dominate the much-studied central component and represent a significant contribution to the TeV atmospheric neutrino flux. Importantly, it cannot accommodate the PeV flux of high-energy cosmic neutrinos, nor the excess of events observed by IceCube in the 30--200 TeV energy range indicating either structure in the flux of cosmic accelerators, or a presence of more than one component in the cosmic flux observed.

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