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Cassini Observations of Saturn's Dawn-Magnetotail Region: Preliminary ResultsUsing Cassini thermal plasma, hot plasma and magnetic field observations for several intervals between the dawn meridian of Saturn's outer magnetosphere and Saturn's magnetotail region, we investigate the structure of the magnetotail, plasma and magnetic field properties within tail-like current sheet regions and ion flows within the dawn to magnetotail regions. We use Cassini Plasma Spectrometer (CAPS) Ion Mass Spectrometer (IMS) and Electron Plasma Spectrometer (ELS) observations and MIMI LEMMS ion and electron observations to characterize the plasma environment. LMS observations are used to measure plasma flow velocities from which one can infer rotation versus convective flows. IMS composition measurements are used to trace the, source of plasma from the inner magnetosphere (protons, H(2+) and water group ions) versus an external solar wind source (protons and He++ ions). A critical parameter for both models is the strength of the convection electric field with respect to the rotational electric field for the large scale magnetosphere. For example, are there significant return flows (i.e., negative radial velocities, V(sub R) < 0) and/or plasmoids (V(sub R) > 0) within the magnetotail region?
Document ID
20080039262
Acquisition Source
Goddard Space Flight Center
Document Type
Conference Paper
Authors
Sittler, Edward C.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Date Acquired
August 24, 2013
Publication Date
January 1, 2007
Publication Information
Publication: EPSC Abstracts
Volume: 2
Subject Category
Astronomy
Report/Patent Number
EPSC2007-A-00428
Meeting Information
Meeting: European Planetary (Europlanet) Science Congress 2007
Location: Potsdam
Country: Germany
Start Date: August 20, 2007
End Date: August 24, 2007
Distribution Limits
Public
Copyright
Other

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