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Cosmic Rays below Z=30 in a diffusion model: new constraints on propagation parameters | | D.Maurin
; F.Donato
; R.Taillet
; P.Salati
; | | Date: |
15 Dec 2000 | | Journal: | Astrophys.J. 555 (2001) 585-596 | | Subject: | astro-ph | | Affiliation: | LAPTH Annecy, Universite de Savoie), F.Donato (LAPTH Annecy), R.Taillet (LAPTH Annecy, Universite de Savoie), P.Salati (LAPTH Annecy, Universite de Savoie | | Abstract: | Cosmic ray nuclei fluxes are expected to be measured with high precision in the near future. For instance, high quality data on the antiproton component could give important clues about the nature of the astronomical dark matter. A very good understanding of the different aspects of cosmic ray propagation is therefore necessary. In this paper, we use cosmic ray nuclei data to give constraints on the diffusion parameters. Propagation is studied with semi-analytical solutions of a diffusion model, and we give new analytical solutions for radioactively produced species. Our model includes convection and reacceleration as well as the standard energy losses. We perform a $chi^2$ analysis over B/C data for a large number of configurations obtained by varying the relevant parameters of the diffusion model. A very good agreement with B/C data arises for a number of configurations, all of which are compatible with sub-Fe/Fe data. Different source spectra $Q(E)$ and diffusion coefficients $K(E)$ have been tried, but for both parameters only one form gives a good fit. Another important result is that models without convection or without reacceleration are excluded. We find that the various parameters, i.e. the diffusion coefficient normalisation $K_0$ and spectral index $delta$, the halo thickness $L$, the Alfvén velocity $V_a$, and the convection velocity $V_c$ are strongly correlated. We obtain limits on the spectral index $delta$ of thediffusion coefficient, and in particular we exclude a Kolmogorov spectrum ($delta = 1/3$). | | Source: | arXiv, astro-ph/0101231 | | Services: | Forum | Review | PDF | Favorites | |
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