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Observational Study of Large Amplitude Longitudinal Oscillations in a Solar Filament

Published online by Cambridge University Press:  06 January 2014

Kalman Knizhnik ,
Manuel Luna ,
Karin Muglach ,
Holly Gilbert ,
Therese Kucera  and
Judith Karpen
Kalman Knizhnik
Affiliation:
Department of Physics and Astronomy The Johns Hopkins University, Baltimore, MD 21218 email: kalman.knizhnik@nasa.gov NASA/GSFC, Greenbelt, MD 20771, USA
Manuel Luna
Affiliation:
Instituto de Astrofísica de Canarias, E-38200 La Laguna, Tenerife, Spain
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
Judith Karpen
Affiliation:
NASA/GSFC, Greenbelt, MD 20771, USA
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Abstract

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On 20 August 2010 an energetic disturbance triggered damped large-amplitude longitudinal (LAL) oscillations in almost an entire filament. In the present work we analyze this periodic motion in the filament to characterize the damping and restoring mechanism of the oscillation. Our method involves placing slits along the axis of the filament at different angles with respect to the spine of the filament, finding the angle at which the oscillation is clearest, and fitting the resulting oscillation pattern to decaying sinusoidal and Bessel functions. These functions represent the equations of motion of a pendulum damped by mass accretion. With this method we determine the period and the decaying time of the oscillation. Our preliminary results support the theory presented by Luna and Karpen (2012) that the restoring force of LAL oscillations is solar gravity in the tubes where the threads oscillate, and the damping mechanism is the ongoing accumulation of mass onto the oscillating threads. Following an earlier paper, we have determined the magnitude and radius of curvature of the dipped magnetic flux tubes hosting a thread along the filament, as well as the mass accretion rate of the filament threads, via the fitted parameters.

Keywords

solar prominencesoscillationsmagnetic structures
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. 428 - 429
Copyright
Copyright © International Astronomical Union 2013 

References

Karpen, J. T., Antiochos, S. K., & Klimchuk, J. A. 2006, ApJ, 637, 531Google Scholar
Luna, M., Karpen, J. T., & Devore, C. R. 2012a, ApJ, 746, 30CrossRefGoogle Scholar
Luna, M. & Karpen, J. 2012, ApJ, 750, L1CrossRefGoogle Scholar
Luna, M., Knizhnik, K., Muglach, K., Gilbert, H, Kucera, T., & Karpen, J., this volume, 2014Google Scholar
Luna, M., Knizhnik, K., Muglach, K., Gilbert, H, Kucera, T., & Karpen, J., ApJ 2013 in prep.Google Scholar
Mackay, D., Karpen, J., Ballester, J., Schmieder, B., & Aulanier, G. 2010, Sp. Sci. Rev., 151, 333CrossRefGoogle Scholar
Tandberg-Hanssen, E. and Anzer, U. 1970, Solar Physics 15, 158TCrossRefGoogle Scholar