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Large-amplitude longitudinal oscillations in solar prominences

Published online by Cambridge University Press:  06 January 2014

Manuel Luna ,
Judith Karpen ,
Antonio Díaz ,
Kalman Knizhnik ,
Karin Muglach ,
Holly Gilbert  and
Therese Kucera
Manuel Luna
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain Universidad de La Laguna, Dept. Astrofísica, E-38206 La Laguna, Tenerife, Spain email: [email protected]
Judith Karpen
Affiliation:
NASA/GSFC, Greenbelt, MD 20771, USA
Antonio Díaz
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain Universidad de La Laguna, Dept. Astrofísica, E-38206 La Laguna, Tenerife, Spain email: [email protected]
Kalman Knizhnik
Affiliation:
NASA/GSFC, Greenbelt, MD 20771, USA Johns Hopkins University, Baltimore, MDUSA
Karin Muglach
Affiliation:
NASA/GSFC, Greenbelt, MD 20771, USA ARTEP, Inc., Maryland, USA
Holly Gilbert
Affiliation:
NASA/GSFC, Greenbelt, MD 20771, USA
Therese Kucera
Affiliation:
NASA/GSFC, Greenbelt, MD 20771, USA
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Abstract

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Large-amplitude longitudinal (LAL) prominence oscillations consist of periodic mass motions along a filament axis. The oscillations appear to be triggered by an energetic event, such as a microflare, subflare, or small C-class flare, close to one end of the filament. Observations reveal speeds of several tens to 100 km/s, periods of order 1 hr, damping times of a few periods, and displacements equal to a significant fraction of the prominence length. We have developed a theoretical model to explain the restoring force and the damping mechanism. Our model demonstrates that the main restoring force is the projected gravity in the flux tube dips where the threads oscillate. Although the period is independent of the tube length and the constantly growing mass, the motions are strongly damped by the steady accretion of mass onto the threads. We conclude that the LAL movements represent a collective oscillation of a large number of cool, dense threads moving along dipped flux tubes, triggered by a nearby energetic event. Our model yields a powerful seismological method for constraining the coronal magnetic field strength and radius of curvature at the thread locations.

Keywords

Solar prominenceOscillationsMagnetic structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S300: Nature of Prominences and their role in Space Weather , June 2013 , pp. 155 - 158
Copyright
Copyright © International Astronomical Union 2013 

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