The Quasi-stationary Structure of Radiating Shock Waves II. The Two-temperature Fluid
| dc.creator | Sincell, M W | |
| dc.creator | Gehmeyr, M | |
| dc.creator | Mihalas, D | |
| dc.date | 1997-10-09 | |
| dc.date.accessioned | 2026-07-07T02:24:29Z | |
| dc.date.available | 2026-07-07T02:24:29Z | |
| dc.description | We solve the equations of radiation hydrodynamics in the two-temperature fluid approximation on an adaptive grid. The temperature structure depends upon the electron-ion energy exchange length, $l_{ei}$, and the electron conduction length, $l_{ec}$. Three types of radiating shock structure are observed: subcritical, where preheating of the unshocked gas is negligible; electron supercritical, where radiation preheating raises the temperature of the unshocked electron fluid to be equal to the final electron temperature; supercritical, where preheating and electron-ion energy exchange raise the preshock $T_{e,i}$ to their final post shock values. No supercritical shock develops when $l_{ei}$ is larger than the photospheric depth of the shocked gas because a negligible amount of the ion energy is transferred to the electrons and the shock is weakly radiating. Electron conduction smooths the $T_e$ profile on a length scale $l_{ec}$, reducing the radiation flux. | |
| dc.identifier | https://arxiv.org/abs/astro-ph/9710095 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/9710095 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/11628 | |
| dc.subject | Astrophysics | |
| dc.title | The Quasi-stationary Structure of Radiating Shock Waves II. The Two-temperature Fluid | |
| dc.type | text |