Structure of the Venus tail.
Abstract
The steady-state tail of Venus at relatively close distances to the planet consists of two magnetic field lobes separated by a current sheet. It is believed to be formed by the mass loading of passing solar wind magnetic flux tubes by planetary ions. Within the Venusian tail at close and intermediate downstream distances (from 0.5v to ≡5 Rv) Venera 9 and 10 measured relatively low-energy ion fluxes that appear to be nearly permanent. At least two plasma populations were identified: one within the tail lobes, and another more energetic one at the current layer. Pioneer Venus data also indicated the presence of two ion populations in the tail at ≡10 - 12 Rv, with the higher energy population being interpreted as accelerated planetary oxygen ions. In this report the authors analyze different plasma regimes in the context of the observed magnetic field configurations in the tail.
- Publication:
-
Geophysical Monograph Series
- Pub Date:
- 1994
- DOI:
- 10.1029/GM084p0207
- Bibcode:
- 1994GMS....84..207V
- Keywords:
-
- Venus: Tails;
- Venus: Solar Wind;
- Venus: Plasma