Saved in:
| Main Authors: | , , , |
|---|---|
| Format: | Preprint |
| Published: |
2025
|
| Subjects: | |
| Online Access: | https://arxiv.org/abs/2503.07218 |
| Tags: |
Add Tag
No Tags, Be the first to tag this record!
|
| _version_ | 1866912303389081600 |
|---|---|
| author | López-Coto, Rubén Green, David Méndez-Gallego, Javier Wilhelmi, Emma de Oña |
| author_facet | López-Coto, Rubén Green, David Méndez-Gallego, Javier Wilhelmi, Emma de Oña |
| contents | Context: Several new phenomena have been surrounding the area of study of the repeating thermonuclear explosions called novae. For example, recurrent novae have been proven to be efficient cosmic ray hadronic accelerators thanks to the recent observations of RS Ophiuchi by different gamma-ray instruments. Novae have also demonstrated to have the ability to carve large cavities into the Interstellar Medium with parallelisms with the remnants of supernovae. We aim at calculating what is the effect of novae in their surrounding media and to which distances these effects dominate over the average quantities that are measured in the ISM. We calculate the filling factor of novae and their contribution to cosmic ray fluxes using cosmic ray propagation codes. To limit what is the atomic density of the Interstellar Medium (ISM) surrounding the region around RS Oph, we use Fermi-LAT observations of the region. The filling factor of novae in the Galaxy is not significant under all assumptions done in the paper. They do not dominate over the local cosmic ray fluxes, even at the lowest energies, for distances larger than a few parsec. The particle density of the ISM surrounding them is, however, very much modified, lowering it more than one order of magnitude with respect to galactic averages, confirming estimates done using other observatories. As a conclusion, even though at global galactic distances, novae do not seem to be dominating cosmic ray transport, they have the power to modify the conditions of their surrounding ISM over parsec distances. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2503_07218 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | Cosmic Ray bubbles from nova super remnants and their contribution to local cosmic ray spectra López-Coto, Rubén Green, David Méndez-Gallego, Javier Wilhelmi, Emma de Oña High Energy Astrophysical Phenomena Context: Several new phenomena have been surrounding the area of study of the repeating thermonuclear explosions called novae. For example, recurrent novae have been proven to be efficient cosmic ray hadronic accelerators thanks to the recent observations of RS Ophiuchi by different gamma-ray instruments. Novae have also demonstrated to have the ability to carve large cavities into the Interstellar Medium with parallelisms with the remnants of supernovae. We aim at calculating what is the effect of novae in their surrounding media and to which distances these effects dominate over the average quantities that are measured in the ISM. We calculate the filling factor of novae and their contribution to cosmic ray fluxes using cosmic ray propagation codes. To limit what is the atomic density of the Interstellar Medium (ISM) surrounding the region around RS Oph, we use Fermi-LAT observations of the region. The filling factor of novae in the Galaxy is not significant under all assumptions done in the paper. They do not dominate over the local cosmic ray fluxes, even at the lowest energies, for distances larger than a few parsec. The particle density of the ISM surrounding them is, however, very much modified, lowering it more than one order of magnitude with respect to galactic averages, confirming estimates done using other observatories. As a conclusion, even though at global galactic distances, novae do not seem to be dominating cosmic ray transport, they have the power to modify the conditions of their surrounding ISM over parsec distances. |
| title | Cosmic Ray bubbles from nova super remnants and their contribution to local cosmic ray spectra |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2503.07218 |