The cumulative background of high energy neutrinos from starburst galaxies
The cumulative background of high energy neutrinos from starburst galaxies
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DOI：
10.1088/1475-7516/2006/05/003
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发表时间：
2006-01
影响因子：
6.4
通讯作者：
A. Loeb;E. Waxman
中科院分区：
文献类型：
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作者：
A. Loeb;E. Waxman
我们表明，星爆星系有效地转换宇宙射线成π介子，这反过来又衰变成高能中微子和光子。GeV中微子的累积背景为Eν2Φν <$10 −7 GeV cm−2 s−1 sr−1，其外推到更高的中微子能量取决于注入宇宙射线的能谱，从Eν2Φν <$Eν- 0.15±0.1到Eν <$0.3 PeV，可能还有更高的中微子能量。这个通量，构成了高能量银河系外中微子通量的一个下限，可能会被即将到来的100倍中微子望远镜探测到。
We show that starburst galaxies efficiently convert cosmic rays into pions, which in turn decay into high energy neutrinos and photons. The cumulative background of GeV neutrinos is Eν2Φν ≈ 10−7 GeV cm−2 s−1 sr−1, and its extrapolation to higher neutrino energies depends on the energy spectrum of the injected cosmic rays, with Eν2Φν ∝ Eν- 0.15±0.1 up to Eν ∼ 0.3 PeV and possibly higher neutrino energies. This flux, which constitutes a lower limit to the high energy extra-Galactic neutrino flux, may be detectable with forthcoming kilometre-scale neutrino telescopes.