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The Jovian Magnetosheath: Factors In...

Joy, Steven Peter.

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The Jovian Magnetosheath: Factors Influencing the Size, Shape, and Mirror Mode Content and Distribution.

紀錄類型:	書目-語言資料,印刷品 : Monograph/item
正題名/作者:	The Jovian Magnetosheath: Factors Influencing the Size, Shape, and Mirror Mode Content and Distribution./
作者:	Joy, Steven Peter.
面頁冊數:	251 p.
附註:	Source: Dissertation Abstracts International, Volume: 71-12, Section: B, page: .
Contained By:	Dissertation Abstracts International71-12B.
標題:	Geophysics. -
電子資源:	http://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=3431900
ISBN:	9781124328157

The Jovian Magnetosheath: Factors Influencing the Size, Shape, and Mirror Mode Content and Distribution.
Joy, Steven Peter.

The Jovian Magnetosheath: Factors Influencing the Size, Shape, and Mirror Mode Content and Distribution. - 251 p.

Source: Dissertation Abstracts International, Volume: 71-12, Section: B, page: .

Thesis (Ph.D.)--University of California, Los Angeles, 2010.

Planetary magnetosheaths, regions of deflected, heated, and decelerated solar wind, are bounded by a bow shock and a magnetopause. We studied how solar wind dynamic pressure and interplanetary magnetic field (IMF) influence the size and shape of the Jovian magnetosheath boundaries. At low pressure, the magnetopause is asymmetric about the planet-sun line, flattened in the poleward direction and bulging out at dusk. As pressure increases, the system boundaries become more symmetric about the planet-sun line.

ISBN: 9781124328157Subjects--Topical Terms:

535228
Geophysics.

The Jovian Magnetosheath: Factors Influencing the Size, Shape, and Mirror Mode Content and Distribution.
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245 1 4 $a The Jovian Magnetosheath: Factors Influencing the Size, Shape, and Mirror Mode Content and Distribution.
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500 $a Source: Dissertation Abstracts International, Volume: 71-12, Section: B, page: .
500 $a Adviser: Margaret G. Kivelson.
502 $a Thesis (Ph.D.)--University of California, Los Angeles, 2010.
520 $a Planetary magnetosheaths, regions of deflected, heated, and decelerated solar wind, are bounded by a bow shock and a magnetopause. We studied how solar wind dynamic pressure and interplanetary magnetic field (IMF) influence the size and shape of the Jovian magnetosheath boundaries. At low pressure, the magnetopause is asymmetric about the planet-sun line, flattened in the poleward direction and bulging out at dusk. As pressure increases, the system boundaries become more symmetric about the planet-sun line.
520 $a Using spacecraft data and boundary shapes extracted from a magnetohydrodynamic simulation, we found a statistically significant bimodal distribution of stand-off distances of the Jovian magnetopause for all solar cycle phases but a statistically significant bimodal distribution of the bow shock stand-off distance was found only near solar minimum. The mean stand-off distances for the magnetopause are 63+/-4 Jupiter radii (RJ) and 92+/-6 RJ; the upper and lower quartile locations of the bow shock standoff distances are 102 RJ and 71 RJ. The statistical characteristics of solar wind pressure and IMF strength near 5 AU were found not to be large enough to account for the magnetopause observations and could be fit to bimodal distributions only at solar minimum. We conclude that internal magnetospheric pressure changes must contribute to the observed bimodal distribution of the stand-off distance.
520 $a Large fluctuations of the magnetic field magnitude are almost always present in magnetosheaths. For Jupiter, criteria were developed for identifying magnetic field perturbations as minor mode structures (MMS) and classifying them by their magnetic signatures into depressions (dips), enhancements (peaks) and "other" (QP, quasi-periodic). We found that "other" MMS were present throughout the magnetosheath and were the only form consistently observed near the bow shock. Peaks were present in the middle magnetosheath at high plasma beta and dips were observed near the magnetopause and in comparatively low beta plasma. We propose that MMS form as QP, evolve into peaks through non-linear saturation of their growth, and form dips as they decay. THEMIS particle distribution functions, used to test the model in the terrestrial magnetosheath, were consistent for QP and peak MMS, but the evidence for dip formation was inconclusive.
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791 $a Ph.D.
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