| Full text | |
| Author(s): |
Echer, E.
Total Authors: 1
|
| Document type: | Journal article |
| Source: | Geophysical Research Letters; v. 46, n. 11, p. 5681-5688, JUN 16 2019. |
| Web of Science Citations: | 0 |
| Abstract | |
Fast interplanetary shocks occurrence, their parameters, and drivers near Jupiter's orbit are determined in this paper. It was found that 70% of the fast shocks are forward (FS) and 30% are reverse (RS). Interplanetary coronal mass ejection-driven FS occur more frequently in all solar cycle phases except in the declining phase, when corotating interaction region-driven shocks predominate. Most of the shocks were quasi-perpendicularly (65 degrees to 70 degrees) propagating relative to the ambient interplanetary magnetic field. The average shock magnetosonic Mach number is slightly higher for FS (2.6) than for RS (2.4), which in turn are stronger than shocks near 1 and 10 AU reported in previous works. This occurs because of the full development of corotating interaction region shocks and higher occurrence of strong interplanetary coronal mass ejections near 5 AU and that the magnetosonic speed at 5 AU has only 60% of its value at 1 AU. (AU) | |
| FAPESP's process: | 18/21657-1 - Study of Jupiter magnetospheric auroral radio activity variability |
| Grantee: | Ezequiel Echer |
| Support Opportunities: | Regular Research Grants |