Hostname: page-component-848d4c4894-m9kch Total loading time: 0 Render date: 2024-05-04T06:29:28.803Z Has data issue: false hasContentIssue false
  • English
  • Français

What can He II 304 Å tell us about transient seismic emission from solar flares?

Published online by Cambridge University Press:  12 September 2017

C. Lindsey  and
A. C. Donea
C. Lindsey
Affiliation:
NorthWest Research Associates, Colorado Division, 3380 Mitchell Lane, Boulder, Colorado, USA email: clindsey@nwra.com
A. C. Donea
Affiliation:
Center for Astrophysics, School of Mathematical Science Monash University, Victoria 3800, Australia
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

After neary 20 years since their discovery by Kosovichev and Zharkova, the mechanics of the release of seismic transients into the solar interior from some flares remain a mystery. Seismically emissive flares invariably show the signatures of intense chromosphere heating consistent with pressure variations sufficient to drive seismic transients commensurate with helioseismic observations—under certain conditions. Magnetic observations show the signatures of apparent magnetic changes, suggesting Lorentz-force transients that could likewise drive seismic transients—similarly subject to certain conditions. But, the diagnostic signatures of both of these prospective drivers are apparent over vast regions from which no significant seismic emission emanates. What distinguishes the source regions of transient seismic emission from the much vaster regions that show the signatures of both transient heating and magnetic variations but are acoustically unproductive? Observations of acoustically active flares in He II 304 Å by the Atomospheric Imaging Assembly (AIA) aboard the Solar Dynamics Observatory (SDO) offer a promising new resource with which to address this question.

Keywords

Sun: flaresmagnetic fieldsUV radiationhelioseismologychromosphere
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S327: Fine Structure and Dynamics of the Solar Atmosphere , October 2016 , pp. 113 - 116
Copyright
Copyright © International Astronomical Union 2017 

References

Alvarado Gómez, J. D., Buitrago Casas, J. C., Martínez Oliveros, J. C., Lindsey, C., & Hudson, H. S. 2013, Solar Phys. 280, 335 Google Scholar
Donea, A.-C. & Lindsey, C. 2005, Ap. J. 630, 1168 Google Scholar
Kosovichev, A. G. & Zharkova, V. V. 1998, Nature 393, 317 Google Scholar
Hudson, H. S., Fisher, G. W., & Welsch, B. J. 2008, ASPC 383 Howe, R. & Komm, R. (eds.) 383, p. 221 Google Scholar
Fisher, G. W., Bercik, D. J., Welsch, B. J., & Hudson, H. S. 2012, Solar Phys. 277, p. 59 Google Scholar
Lindsey, C. & Donea, A.-C. 2008, Solar Phys. 251, 627 Google Scholar
Zharkov, S., Green, L. M., Matthews, S. A., & Zharkova, V. V. 2011, Ap. J. 741, 35 Google Scholar
Zharkov, S., Green, L. M., Matthews, S. A., & Zharkova, V. V. 2013, Solar Phys. 284, 315 Google Scholar