Low Energy Cosmic Ray Interactions in Astrophysics
| dc.creator | Ramaty, Reuven | |
| dc.date | 1996-01-10 | |
| dc.date.accessioned | 2026-07-07T06:31:59Z | |
| dc.date.available | 2026-07-07T06:31:59Z | |
| dc.description | Solar flare observations are used to demonstrate the new technique of abundance determination based on gamma ray line emission produced by accelerated particle bombardment. Some of the implications of similar gamma ray line emission observed from Orion, including the production of light elements by low energy cosmic rays, are reviewed. For such an origin for the light elements, limitations on the total available energy in low energy cosmic rays imply that the production takes place at relatively high particle energies, around 30 MeV/nucl. Such low energy cosmic rays can reproduce the meteoritic B isotopic ratio of 4, but they require an accelerated C/O on the order of the observed solar system ratio ($\sim$0.5). If in the early Galaxy C/O in the ejecta of Type II supernovae from massive star progenitors (which are thought to be the sources of the postulated cosmic rays) is much lower, then the B isotopic ratio in low metallicity stars should be significantly lower than the measured meteoritic value. | |
| dc.description | 10 pages with 5 figures, uuencoded, compressed, tared to appear in the Proceedings of the Vietnam Conference, "The Sun and Beyond", 1966 | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9601049 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9601049 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/98774 | |
| dc.subject | Astrophysics | |
| dc.title | Low Energy Cosmic Ray Interactions in Astrophysics | |
| dc.type | text |