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| Main Authors: | , |
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| Format: | Preprint |
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2023
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| Online Access: | https://arxiv.org/abs/2309.08823 |
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| _version_ | 1866916287930695680 |
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| author | Cowsik, Ramanath Huth, Dawson |
| author_facet | Cowsik, Ramanath Huth, Dawson |
| contents | The recent measurements of the spectral intensities of cosmic-ray nuclei have suggested that the ratio of Boron to Carbon nuclei, $R(E)$, comprises two components, $R_1(E)$ which carries all of the energy dependence and the other $R_A$, a constant independent of energy per nucleon. This finding supports the earlier theoretical expectations and results of gamma-ray astronomy that one of these components is attributable to spallation in a cocoon like region surrounding the sources and the other in the general interstellar medium before cosmic rays leak away from the Galaxy. A new model-independent way of analyzing cosmic-ray spectra is presented here to shed light on the recent findings: Imposing the single constraint that the source function of B nuclei is minimal we use a cascade of rate equations to map point-by-point the observed cosmic ray spectra of p, B, C, O and Fe on to their source spectra and the two life-times of cosmic rays $τ_G$ in the Galaxy and $τ_S$ in the cocoons surrounding the sources. The model independent results show that the appropriate choice is $τ_S(E)$ is responsible for $R_1(E)$ and the source spectra are power laws with indices of $\sim-2.7$. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2309_08823 |
| institution | arXiv |
| publishDate | 2023 |
| record_format | arxiv |
| spellingShingle | Mapping the AMS-02 and CALET Data onto the Source Spectra and Residence Times of Galactic Cosmic Rays Cowsik, Ramanath Huth, Dawson High Energy Astrophysical Phenomena The recent measurements of the spectral intensities of cosmic-ray nuclei have suggested that the ratio of Boron to Carbon nuclei, $R(E)$, comprises two components, $R_1(E)$ which carries all of the energy dependence and the other $R_A$, a constant independent of energy per nucleon. This finding supports the earlier theoretical expectations and results of gamma-ray astronomy that one of these components is attributable to spallation in a cocoon like region surrounding the sources and the other in the general interstellar medium before cosmic rays leak away from the Galaxy. A new model-independent way of analyzing cosmic-ray spectra is presented here to shed light on the recent findings: Imposing the single constraint that the source function of B nuclei is minimal we use a cascade of rate equations to map point-by-point the observed cosmic ray spectra of p, B, C, O and Fe on to their source spectra and the two life-times of cosmic rays $τ_G$ in the Galaxy and $τ_S$ in the cocoons surrounding the sources. The model independent results show that the appropriate choice is $τ_S(E)$ is responsible for $R_1(E)$ and the source spectra are power laws with indices of $\sim-2.7$. |
| title | Mapping the AMS-02 and CALET Data onto the Source Spectra and Residence Times of Galactic Cosmic Rays |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2309.08823 |