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Prominence Structure and DynamicsNonerupting prominences are not dull, static objects. Rather, they are composed of fine-scale blobs and threads that are highly dynamic, often appearing to travel in opposite directions on adjacent tracks (denoted counterstreaming). Because the plasma is largely constrained to travel along the magnetic field, these cool, dense features can serve as tracers of the prominence magnetic structure, a valuable resource in view of the long-standing difficulty of observing the coronal field. Conversely, greater understanding of the fundamental magnetic geometry of filament channels can provide important constraints on the physical processes governing the accumulation, support, motion, and eruption of the cool plasma. Despite over a century of detailed observations, large gaps remain in our knowledge of filament channel/plasma formation and evolution. Resolving these issues will shed light on the physics of coronal heating, helicity transport throughout the solar cycle, and the origins of eruptive activity on the Sun. I will discuss the leading models for the magnetic and plasma structure, and outline how new observations and theory /modeling could solve long-standing uncertainties regarding this majestic solar phenomenon.
Document ID
20110008720
Acquisition Source
Goddard Space Flight Center
Document Type
Abstract
Authors
Karpen, Judy T.
(NASA Goddard Space Flight Center Greenbelt, MD, United States)
Date Acquired
August 25, 2013
Publication Date
September 1, 2009
Subject Category
Solar Physics
Meeting Information
Meeting: NSO Workshop 25: Chromospheric Structure and Dynamics
Location: Sunspot, NM
Country: United States
Start Date: September 1, 2009
End Date: September 5, 2009
Sponsors: National Solar Observatory
Distribution Limits
Public
Copyright
Work of the US Gov. Public Use Permitted.
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