Evolution of an afterglow with a hard electron spectrum
| dc.creator | Bhattacharya, D | |
| dc.creator | Resmi, L | |
| dc.date | 2003-01-19 | |
| dc.date.accessioned | 2026-07-07T02:07:16Z | |
| dc.date.available | 2026-07-07T02:07:16Z | |
| dc.description | Diffusive shock acceleration theory suggests that the ``universal'' energy spectrum of electrons with a power-law index p approximately equal to 2.3, commonly used to model GRB afterglows, cannot extend below an electron lorentz factor gamma_e equal to the bulk lorentz factor of the blast wave multiplied by the ratio of proton and electron masses. We suggest that the electron energy distribution has a slope p < 2 below this limit, down to an appropriate gamma_m. A two-slope spectrum such as this provides a good model for the afterglow of GRB010222. | |
| dc.description | 4 pages, 2 figures, contribution to Rome 2002 GRB Workshop | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0301379 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0301379 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/5639 | |
| dc.subject | Astrophysics | |
| dc.title | Evolution of an afterglow with a hard electron spectrum | |
| dc.type | text |