Radiation from Relativistic Strongly Magnetized Outflows
| dc.creator | Usov, Vladimir V. | |
| dc.date | 1999-09-26 | |
| dc.date.accessioned | 2026-07-07T02:33:28Z | |
| dc.date.available | 2026-07-07T02:33:28Z | |
| dc.description | Relativistic strongly magnetized winds outflowing from fast-rotating compact objects like millisecond pulsars with surface magnetic fields of $\sim 10^{15}-10^{16}$ G are plausible sources of cosmological $γ$-ray bursts. In such winds, there are at least three regions where extremely powerful X-ray and $γ$-ray emission may be generated. The first radiating region is the wind photosphere that is at a distance of $\sim 10^9$ cm from the compact object. The second radiating region is at a distance of $\sim 10^{13}-10^{14}$ cm. In this region, the striped component of the wind field is transformed into large-amplitude electromagnetic waves. The third radiating region is at a distance of $\sim 10^{16}-10^{17}$ cm, where deceleration of the wind due to its interaction with an ambient medium becomes important. Radiation from all these regions is considered. | |
| dc.description | 20 pages, 6 eps figures. To appear in the Proceedings of "Gamma-Ray Bursts: The First Three Minutes", eds. J. Poutanen and R. Svensson | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9909435 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9909435 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/14858 | |
| dc.subject | Astrophysics | |
| dc.title | Radiation from Relativistic Strongly Magnetized Outflows | |
| dc.type | text |