| Full text | |
| Author(s): |
Lazarian, A.
;
Kowal, G.
;
Gouveia dal Pino, B.
;
Pogorelov, NV
;
Font, JA
;
Audit, E
;
Zank, GP
Total Authors: 7
|
| Document type: | Journal article |
| Source: | STARS WITH THE B[E] PHENOMENON, PROCEEDINGS; v. 459, p. 3-pg., 2011-01-01. |
| Abstract | |
Astrophysical reconnection takes place in a turbulent medium. The turbulence in most cases is pre-existing, not caused by the reconnection itself. The model of magnetic reconnection in Lazarian & Vishniac (1999) predicts that in the presence of turbulence the reconnection becomes fast, i.e. it is independent of resistivity, but dependent on the level of turbulence. Magnetic reconnection injects energy into plasmas through a turbulent outflow from the reconnection region and this outflow can enhance the level of turbulence creating bursts of reconnection. Magnetic reconnection in the presence of turbulence can accelerate energetic particles through the first order Fermi mechanism, as was predicted in Gouveia dal Pino & Lazarian (2005). We discuss new numerical results on particle acceleration in turbulent reconnection and compare the acceleration arising from turbulent reconnection to the acceleration of energetic particles in turbulent medium. (AU) | |
| FAPESP's process: | 06/50654-3 - Investigation of high energy and plasma astrophysics phenomena: theory, observation, and numerical simulations |
| Grantee: | Elisabete Maria de Gouveia Dal Pino |
| Support Opportunities: | Research Projects - Thematic Grants |
| FAPESP's process: | 09/50053-8 - Magnetic reconnection and particle acceleration in astrophysical sources and diffuse media |
| Grantee: | Grzegorz Kowal |
| Support Opportunities: | Scholarships in Brazil - Post-Doctoral |