Electron temperatures within magnetic clouds between 2 and 4 AU: Voyager 2 observations

Details Electron temperatures within magnetic clouds between 2 and 4 AU: Voyager 2 observations Electron temperatures within magnetic clouds between 2 and 4 AU: Voyager 2 observations

Aug 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998jgr...10317447s&link_type=abstract

Journal of Geophysical Research, Volume 103, Issue A8, p. 17447-17454

Physics

9

Interplanetary Physics: Ejecta, Driver Gases, And Magnetic Clouds

Scientific paper

We have performed an analysis of Voyager 2 plasma electron observations within magnetic clouds between 2 and 4 AU identified by Burlaga and Behannon [1982]. The analysis has been confined to three of the magnetic clouds identified by Burlaga and Behannon that had high-quality data. The general properties of the plasma electrons within a magnetic cloud are that (1) the moment electron temperature anticorrelates with the electron density within the cloud, (2) the ratio Te/Tp tends to be >1, and (3) on average, Te/Tp~7.0. All three results are consistent with previous electron observations within magnetic clouds. Detailed analyses of the core and halo populations within the magnetic clouds show no evidence of either an anticorrelation between the core temperature TC and the electron density Ne or an anticorrelation between the halo temperature TH and the electron density. Within the magnetic clouds the halo component can contribute more than 50% of the electron pressure. The anticorrelation of Te relative to Ne can be traced to the density of the halo component relative to the density of the core component. The core electrons dominate the electron density. When the density goes up, the halo electrons contribute less to the electron pressure, so we get a lower Te. When the electron density goes down, the halo electrons contribute more to the electron pressure, and Te goes up. We find a relation between the electron pressure and density of the form Pe=αNeγ with γ~0.5.

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