《Table 4 Fitting parameters of the injection spectra》

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《Implications on cosmic ray injection and propagation parameters from Voyager/ACE/AMS-02 nucleus data》

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a) Source abundance relative to Hydrogen；b) χ2Σhas been included.

whereθrepresents the propagation parameter set，ˉθis the vector of the mean propagation parameters given in Table 3，andΣis the covariance matrix of these parameters which has been derived in the previous subsection.We re-fit the fluxes of protons，helium，carbon，and oxygen to derive the injection spectral parameters of these species.Slightly different from eq.（1），we introduce an additional spectral break at Rbr，2，which is around a few hundred GV，to describe the spectral hardenings.Besides the Voyager and AMS-02 data，for protons and helium nuclei，the CREAM I+III data at higher energies are also used[41].For carbon and oxygen nuclei，the ACE data given in Table 2 are used.Since the observed helium，carbon，and oxygen spectra by AMS-02 show similarities among each other[13]，we first do the fit with all these three compositions together.The injection parameters of them are assumed to be the same，with only differences of the normalizations.However，we find that in both DC2and DR2 models，the goodness-of-fit is very poor.The propagated spectra of these nuclei differ mainly at low energies，perhaps due to different cooling rates of them in the interstellar medium.This result suggests that the injection spectra of helium，carbon，and oxygen might be different.The similar result has also been obtained in a recent work[42].