Cosmic ray acceleration

Nevertheless, as has been emphasized by Ramaty et al. (2000), the kind of boost to the cosmic-ray flux per supernova implied by Eq. (9.57) is untenable on energetic grounds. From present-day abundances, one can estimate the quantity Q/W, the number of Be atoms per erg of cosmic-ray energy. Given an iron yield of 0.2 M per average supernova (of both types) today, and a Be/Fe ratio of 10-6, one finds a yield of 4 x 1048 Be atoms per supernova. If the typical supernova explosion energy is 1051 erg and the cosmic-ray acceleration efficiency is 10 per cent, this... 

Fig. 9.8. Trend of beryllium abundance with metallicity compared to predictions from two models (a) CRS denotes cosmic-ray acceleration in superbubbles rich in iron and oxygen as predicted from theoretical supernova yields (in this case those of Tsujimoto and Shigeyama 1998) and (b) CRI denoting cosmic rays accelerated from the general interstellar medium. The density dependence comes from its influence on the delay in the deposition of the synthesized Be. Virtually identical results were obtained using the yields from Woosley and Weaver (1995). After Ramaty et al. (2000).

The correction of observed at the Earth cosmic ray composition for nuclear fragmentation in the interstellar medium makes it possible to determine the initial elemental and isotopic composition of accelerated particles, to clarify the process of cosmic ray acceleration and the nature of cosmic ray sources. 

The entire pattern of cosmic ray acceleration at supernova shocks critically depends on the assumption that the energetic particles themselves produce the... 

Bell, A.R., and S.G. Lucek. (2001). Cosmic-ray acceleration to very high energie through the non-linear amplification by cosmic rays of the seed magnetic field44, MN-RAS 321,433. 

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