High-speed translunar magnetotail plasma flows

Simple item page
dc.contributor.advisorFreeman, John W.en_US
dc.creatorShull, Peter Ottoen_US
dc.date.accessioned2018-12-18T21:14:59Zen_US
dc.date.available2018-12-18T21:14:59Zen_US
dc.date.issued1979en_US
dc.description.abstractUnusual, high-speed flows of plasma away from the Sun in the translunar magnetotail are discovered to occur persistently. Faster, cooler, and less dense than the plasma flows customarily encountered in the translunar magnetotail, these flows suggest that small-scale magnetic merging occurs regularly in the plasma sheet. Particle and field data from eight and one-half magnetotail crossings are studied, making this the most extensive survey to date. Those crossings are chosen for which there are magnetometer data from Explorer 35 and particle data from the Rice Suprathermal Ion Detector Experiment (SIDE) set up on the Moon by the crew of Apollo 14. This SIDE, like its twins from Apollos 12 and 15, measures plasma energy distributions in the energy/charge range between 1 and 35 eV/q. Computer reduction of these SIDE data yields plasma bulk speeds, temperatures, and densities. With the assumption that the plasma is entirely hydrogen, it is found that the plasma flows are characterized by bulk velocity u = 25 to 7 km/s, ion temperature kT = 5 to 1 eV, and ion density n = .1 to .1 cm. Most of these flows ("bubble" flows) occur within one or two hours of changes in tail magnetic field strength and direction, changes suggesting the passage of the Moon near a magnetic bubble. Two or three flows ("lobe" flows) are associated exclusively with >= 1/y magnetic fields parallel or anti-parallel to the Earth-Sun axis. Neither type of flow is directly related to solar or geomagnetic activity. The transfer of magnetic field energy to mantle plasma in the cislunar magnetotail may cause the bubble flows. Appearances of doubly peaked plasma energy distributions are briefly discussed. The origin of the lobe flows is uncertain. If the field lines associated with them map into a magnetic bubble, the flows are probably bubble flows observed farther than usual from their places of origin. If the field lines map into the polar regions of Earth, then the lobe flows may be ions such as H+, He+, He++, and + escaping from the polar ionospheres.en_US
dc.format.digitalOriginreformatted digitalen_US
dc.format.extent61 ppen_US
dc.identifier.callnoTHESIS SP. SCI. 1979 SHULLen_US
dc.identifier.citationShull, Peter Otto. "High-speed translunar magnetotail plasma flows." (1979) Master’s Thesis, Rice University. <a href="https://hdl.handle.net/1911/103886">https://hdl.handle.net/1911/103886</a>.en_US
dc.identifier.digitalRICE1512en_US
dc.identifier.urihttps://hdl.handle.net/1911/103886en_US
dc.language.isoengen_US
dc.rightsCopyright is held by the author, unless otherwise indicated. Permission to reuse, publish, or reproduce the work beyond the bounds of fair use or other exemptions to copyright law must be obtained from the copyright holder.en_US
dc.titleHigh-speed translunar magnetotail plasma flowsen_US
dc.typeThesisen_US
dc.type.materialTexten_US
thesis.degree.departmentSpace Scienceen_US
thesis.degree.disciplineNatural Sciencesen_US
thesis.degree.grantorRice Universityen_US
thesis.degree.levelMastersen_US
thesis.degree.nameMaster of Scienceen_US
Files
Original bundle
Now showing 1 - 1 of 1
Thumbnail Image
Name:
RICE1512.pdf
Size:
2.08 MB
Format:
Adobe Portable Document Format
Download
Collections
Rice University Theses and Dissertations