The radiation belts of jupiter

Degioanni, Joseph J.C.

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https://hdl.handle.net/2142/79028 Copy

Description

Title

The radiation belts of jupiter

Author(s)

Degioanni, Joseph J.C.

Issue Date

1973-06

Director of Research (if dissertation) or Advisor (if thesis)

Dickel, John R.

Department of Study

Astronomy

Discipline

Astronomy

Degree Granting Institution

University of Illinois at Urbana-Champaign

Degree Name

Ph.D. (doctoral)

Degree Level

Dissertation

Keyword(s)

• Jovian magnetosphere
• Jupiter
• Radiation belts
• Decimetric continuum
• Thermal emission

Language

en

Abstract

A simplified model of the Jovian magnetosphere consists of a thermal plasma with superimposed radiation belts. Recently Melrose (1966) and Ioannidis and Brice (1971) have described the possible sources and distribution of the thermal plasma trapped in the magnetosphere of Jupiter. The model to be described here deals exclusively with the cloud of relativistic electrons which forms the radiation belts at a distance of a few Jovian radii from the planet and is responsible for the intense continuum of decimetric emission. The purpose of this model is to describe the structure of the radiation belts on the basis of the observations of their continuum emission at decimetric wavelengths. Most of this data was obtained in the past decade and consists of the following: (i) observations of the integrated flux in the decimetric continuum (See Figure 16a); (ii) observations of the degree of polarization of the radiation (See=·Figures 17 and 18); (iii) observations of the dependence on the rotation of Jupiter (or dependence on the System III longitude) of the integrated flux, degree of polarization, and orientation of the plane of polarization (See Figure 33a); (iv) high-resolution interferometric studies of the radiation belts (Berge, 1966; Branson, 1968); (v) lunar occultation studies of the radiation belts (Gulkis, 1970). In addition, the non-thermal emission is separated from the thermal emission of the planetary disk with the aid of the observations by Berge (1966) and Branson (1968) and models of Jupiter's atmosphere by Goodman (1969).

Type of Resource

text

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http://hdl.handle.net/2142/79028

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