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Response of the solar five-minute oscillations to a major flare

Published online by Cambridge University Press:  03 August 2017

Deborah A. Haber ,
Juri Toomre  and
Frank Hill
Deborah A. Haber
Affiliation:
Joint Institute for Laboratory Astrophysics, and Department of Astrophysical, Planetary and Atmospheric Sciences, University of Colorado, Boulder, CO 80309-0440, USA
Juri Toomre
Affiliation:
Joint Institute for Laboratory Astrophysics, and Department of Astrophysical, Planetary and Atmospheric Sciences, University of Colorado, Boulder, CO 80309-0440, USA
Frank Hill
Affiliation:
National Solar Observatory, National Optical Astronomy Observatories, Tucson, AZ 85726-6732, USA

Abstract

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Solar five-minute oscillations of intermediate-degree ℓ were observed both before and after a very strong white-light flare. Intensity images of the full Sun taken on two sides of the Fe I λ 5576 spectral line were recorded on film, digitized with 8″ spatial resolution, and then converted into Doppler velocities. The data were projected onto both equatorial and polar sectoral modes and Fourier transformed in time. Comparing the resulting power spectra, we find a substantial increase in power in the p5 ridge of the equatorial modes on the day after the flare; such an increase may be a consequence of the solar flare. When data from all the ridges are considered, there is an average increase in power of only a few percent the day after the flare. This overall increase is probably not significant due to uncertainties from effects of the beating of unresolved modes.

Type
Chapter 1: Observations of Solar Oscillations
Information
Symposium - International Astronomical Union , Volume 123: Advances In Hello- and Asteroseismology , 1988 , pp. 59 - 62
Copyright
Copyright © Reidel 1988 

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