Properties of the solar wind electrons between 1.1 and 3.3 AU from Ulysses thermal noise measurements
- Observatoire de Paris, Departement de Recherche Spatiale, Meudon (France)
Using the distribution function f(v) of the solar wind electrons made of two Maxwellians: a core (density n{sub c}, temperature T{sub c}) and a halo (density n{sub h}, temperature T{sub h}), we determine the quasi-thermal noise (QTN) induced by the ambient electrons on the long wire dipole antenna connected to the radio receiver on the Ulysses Unified Radio and Plasma Wave (URAP) Experiment. The QTN spectroscopy yields the total electron density n{sub e}, the core temperature T{sub c}, and the core and halo kinetic pressures n{sub c}T{sub c} and n{sub h}T{sub h}. We present the results of n{sub e} and T{sub c} measured between 1.1 and 3.3 AU in the ecliptic plane, from November 1990 to June 1991. We investigate the variation of T{sub c} with the heliocentric distance. We also study this radial gradient as a function of three classes of n{sub e} normalized to 1 AU: Low, intermediate and high densities. The T{sub c} gradient is found to increase with increasing plasma density.
- OSTI ID:
- 21163487
- Journal Information:
- AIP Conference Proceedings, Vol. 382, Issue 1; Conference: 8. international solar wind conference: Solar wind eight, Dana Point, CA (United States), 25-30 Jun 1995; Other Information: DOI: 10.1063/1.51485; (c) 1996 American Institute of Physics; Country of input: International Atomic Energy Agency (IAEA); ISSN 0094-243X
- Country of Publication:
- United States
- Language:
- English
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