Diagnostics of the Heating Processes in Solar Flares Using Chromospheric Spectral Lines
| dc.creator | Cheng, J. X. | |
| dc.creator | Ding, M. D. | |
| dc.creator | Li, J. P. | |
| dc.date | 2006-09-25 | |
| dc.date.accessioned | 2026-07-07T10:40:15Z | |
| dc.date.available | 2026-07-07T10:40:15Z | |
| dc.description | We have calculated the H$α$ and Ca {\sc ii} 8542 Å line profiles based on four different atmospheric models, including the effects of nonthermal electron beams with various energy fluxes. These two lines have different responses to thermal and nonthermal effects, and can be used to diagnose the thermal and nonthermal heating processes. We apply our method to an X-class flare that occurred on 2001 October 19. We are able to identify quantitatively the heating effects during the flare eruption. We find that the nonthermal effects at the outer edge of the flare ribbon are more notable than that at the inner edge, while the temperature at the inner edge seems higher. On the other hand, the results show that nonthermal effects increase rapidly in the rise phase and decrease quickly in the decay phase, but the atmospheric temperature can still keep relatively high for some time after getting to its maximum. For the two kernels that we analyze, the maximum energy fluxes of the electron beams are $\sim$ 10$^{10}$ and 10$^{11}$ ergs cm$^{-2}$ s$^{-1}$, respectively. However, the atmospheric temperatures are not so high, i.e., lower than or slightly higher than that of the weak flare model F1 at the two kernels. We discuss the implications of the results for two-ribbon flare models. | |
| dc.description | 6 pages, 9 figures, accepted for publication in ApJ | |
| dc.identifier | https://arxiv.org/abs/astro-ph/0609674 | |
| dc.identifier | http://arxiv.org/abs/astro-ph/0609674 | |
| dc.identifier | Astrophys.J.653:733-738,2006 | |
| dc.identifier | doi:10.1086/508855 | |
| dc.identifier.uri | http://salesiana.dossiersoluciones.com/handle/123456789/181283 | |
| dc.subject | Astrophysics | |
| dc.title | Diagnostics of the Heating Processes in Solar Flares Using Chromospheric Spectral Lines | |
| dc.type | text |