On the Origin of Highest Energy Cosmic Rays
On the Origin of Highest Energy Cosmic Rays
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最高能量宇宙射线的起源
DOI：
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发表时间：
1990
期刊：
影响因子：
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通讯作者：
F. Takahara
中科院分区：
文献类型：
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作者：
F. Takahara
42毫克。S-r，占总光度的一小部分。到达方向的各向异性应该可以观测到附近的射电星系。近几十年来，宇宙射线的起源一直是一个广泛讨论的话题。最近，冲击波的统计加速已被广泛接受为宇宙射线最可行的加速机制。超新星残骸中的激波被认为为能量范围低于10 - 14 - 15 eV的宇宙射线的加速提供了可能的场所；然而，对于更高的能量，哪一种机制造成了加速度，这是一个悬而未决的问题。在最理想的情况下，星际隧道和银河风中的统计加速可以分别将质子加速到10 16 eV和10 1g eV；把它们加速到更高的能量似乎是不可能的。与来自Cyg X -3和Her X- 1的高能伽马射线有关，研究了具有强磁场的中子星周围的粒子加速。但是显著的辐射损失抑制了质子在10 - 17以上的加速
42 erg . s-r, which is a modest fraction of the total luminosity. Anisotropy in the arrival direction should be observable towards nearby radio galaxies. Origin of cosmic rays has been a topic of an extensive discussion in these decades. Recently statistical acceleration by shock waves has been widely accepted as the most viable acceleration mechanism of cosmic rays.!) Shocks in supernova remnants are believed to provide plausible places for the acceleration of cosmic rays for the energy range below 10 14 - 15 eV;2} For higher energies, however, it is an open question which mechanism is responsible for the acceleration. Statistical acceleration in interstellar tunnels 3 } and galactic winds 4 } may accelerate protons up to 10 16 eV and 10 1g eV, respectively, for most preferable cases; it seems to be improbable to accelerate them to higher energies. In relation to very high energy gamma rays from Cyg X -3 and Her X-I, particle acceleration around neutron stars with strong magnetic fields has been investigated. 5 } But significant radiation loss inhibits the acceleration of protons beyond 10 17