Diffuse PeV neutrino emission from ultraluminous infrared galaxies
Diffuse PeV neutrino emission from ultraluminous infrared galaxies
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超亮红外星系的弥散 PeV 中微子发射
DOI：
10.1103/physrevd.87.063011
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发表时间：
2013-03
期刊：
影响因子：
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通讯作者：
Wei Da-Ming
中科院分区：
文献类型：
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作者：
He Hao-Ning;Wang Tao;Fan Yi-Zhong;Liu Si-Ming;Wei Da-Ming
超亮红外星系(ULIRG)是宇宙中最明亮、最强烈的星暴星系。它们的恒星形成率和气体表面质量密度都非常高，这意味着它们有很高的超新星速率和高能质子的有效能量转换。这些超新星中有一小部分是所谓的超新星，其典型动能类似于10(52)erg，激波速度>；=10(9)厘米S(-1)。超新星驱动的强激波能够将宇宙线质子加速到1017 eV。当这些高能质子被弹射到非常密集的星际介质中时，通过质子-质子的碰撞损失了很大一部分能量，结果产生了高能中微子(<；=5PeV)。最近的深红外探测对超新星红移范围0<；=z<；=2.3的超新星群的数密度提供了坚实的约束，使我们能够从超新星中得出弥散中微子的通量。我们发现，在PeV能量下，假设注入的宇宙线谱为dN(P)‘/d epsilon(P)’与epsilon(P)‘(-2)成正比，ULIRGs贡献的弥散中微子与通量为2×10(-9)GeV cm(-2)的S(-1)锶(-1)的大气中微子相当。DOI：10.1103/PhysRevD.87.063011
Ultraluminous infrared galaxies (ULIRGs) are the most luminous and intense starburst galaxies in the Universe. Both their star formation rates and their gas surface mass densities are very high, implying a high supernova rate and an efficient energy conversion of energetic protons. A small fraction of these supernovae are the so-called hypernovae, with a typical kinetic energy similar to 10(52) erg and a shock velocity >= 10(9) cm s(-1). The strong shocks driven by hypernovae are able to accelerate cosmic ray protons up to 1017 eV. These energetic protons lose a good fraction of their energy through proton-proton collision when ejected into very dense interstellar media, and as a result, produce high-energy neutrinos (<= 5 PeV). Recent deep infrared surveys provide solid constraints on the number density of ULIRGs across a wide redshift range 0 <= z <= 2.3, allowing us to derive the flux of diffuse neutrinos from hypernovae. We find that at PeV energies, the diffuse neutrinos contributed by ULIRGs are comparable to atmosphere neutrinos with the flux of 2 x 10(-9) GeV cm(-2) s(-1) sr(-1) by assuming the injected cosmic ray spectrum to be dN(p)'/d epsilon(p)' proportional to epsilon(p)'(-2). DOI: 10.1103/PhysRevD.87.063011