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Large-Scale Alfvenic Impulses on the Sun: How They Are Generated and What We Learn From ThemNASA GSFC The Sun's atmosphere hosts a wide variety of magnetosonic disturbances. These wave modes are detected, almost exclusively, by examining images of the Sun's magnetic atmosphere and looking for propagating distortions. Although none of the Sun's plasma parameters are measured directly, we derive a great deal of information from these observations. In fact, by modeling these propagating disturbances, we may be able to derive the most accurate estimates plasma parameters. From observations absorption, refraction, reflection, and coupling of numerous wave modes, we advance our knowledge of the Sun's magnetic field, temperature, density, and current. The Sun's continuous oscillation, coronal mass ejections, flares, and other dynamic phenomena can produce wave disturbances which are observable from near-Earth space. Several of these disturbances have been traced from the inner corona out into the heliosphere. From the generation of these disturbances, we are able to learn about the phenomena which create them as well as the media through which they re-propagating. The presentation will include a discussion of the generation of Alfvenic disturbances on the Sun, ways we observe these disturbances, and how recent advances in modeling and analysis have brought us closer to determining solar in situ parameters.
Document ID
20040182417
Acquisition Source
Goddard Space Flight Center
Document Type
Conference Paper
Authors
Thompson, Barbara
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Date Acquired
August 22, 2013
Publication Date
January 1, 2004
Subject Category
Solar Physics
Meeting Information
Meeting: Alfven Conference
Location: Steamboat Springs, CO
Country: United States
Start Date: August 22, 2004
End Date: August 28, 2004
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.

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