论文标题
关于产生非常高能天体物理中微子的质子的能量
On the energy of the protons producing the very high-energy astrophysical neutrinos
论文作者
论文摘要
我们研究质子的能量的分布，可以通过$ pp $或$pγ$相互作用在TEV-PEV范围内产生带有观察到的能量的天体中微子。由于高质量能量中心产生的多样性增加，因此由此产生的平均质子能量可能比经常使用的近似值$ e_p \ simeq20E_ν$大得多。同样，$pγ$过程的阈值可能会导致$ \ langle e_p \ rangle /e_ν$的明显增加，以减少中微子的能量。结果敏感地取决于假定的质子光谱，因为较陡的光谱给出的较低的能量中微子的尾巴的重量较小，这是由于丰富的低能硫酸盐的衰变而导致的。在$Pγ$的情况下，它们也敏感地取决于目标光子的光谱。结果特别与将中微子光谱与产生它们的相应宇宙射线的可能特征相关联。我们还讨论了来源的伽马射线的相关生产。
We study the distribution of the energy of the protons that can produce an astrophysical neutrino with a given observed energy, in the TeV--PeV range, both through $pp$ or $pγ$ interactions. Due to the increasing multiplicity of the pion production at high center of mass energies, the resulting average proton energies can be much larger than the often used approximate value $E_p\simeq 20E_ν$. Also the threshold of the $pγ$ process can lead to a pronounced increase in the values of $\langle E_p\rangle /E_ν$ for decreasing neutrino energies. The results depend sensitively on the assumed proton spectrum, since steeper spectra give less weight to the lower energy neutrino tail resulting from the decays of the abundant low-energy pions. In the $pγ$ scenarios they also depend sensitively on the spectrum of the target photons. The results are in particular relevant to relate possible characteristics of the neutrino spectrum to those of the corresponding cosmic rays that generated them. We also discuss the associated production of gamma rays at the sources.
