This thesis examines the two state structure of the solar wind and its influence upon proton temperatures. To examine this question, data from the Helios spacecraft are examined. The results from the data are interpreted in light of several theoretical models of the solar wind. In particular, it is found that the interplanetary heating of the protons observed by Helios is consistent with models that rely on extended deposition of energy and momentum in the form of Alfvenic waves.
Analysis shows that between 4-10% of the time the data are consistent with two fluid models which do not include extended deposition of energy and momentum. For the rest of the data, the magnetic fluctuations are analyzed and it is found that there is dissipation of wave energy. Calculations show that the heating required by the protons can be accounted for by the apparent dissipation of Alfvenic wave energy. The relationships of temperature to velocity, to number density, and to momentum flux are also examined and are found to be consistent with a bifurcation of the solar wind based upon Alfven waves. A qualitative scenario for the generation of the two state solar wind wherein all the energy for the solar wind comes from convection in the sun is discussed.
| Identifer | oai:union.ndltd.org:RICE/oai:scholarship.rice.edu:1911/16030 |
| Date | January 1985 |
| Creators | LOPEZ, RAMON E. |
| Source Sets | Rice University |
| Language | English |
| Detected Language | English |
| Type | Thesis, Text |
| Format | application/pdf |
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