Hostname: page-component-586b7cd67f-2brh9 Total loading time: 0 Render date: 2024-11-22T23:04:34.748Z Has data issue: false hasContentIssue false
  • English
  • Français

Sunquakes and starquakes

Published online by Cambridge University Press:  18 February 2014

Alexander G. Kosovichev
Alexander G. Kosovichev*
Affiliation:
Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA email: [email protected] Big Bear Solar Observatory, Big Bear City, CA 92314, USA Crimean Astrophysical Observatory, Nauchny, Crimea 98409, Ukraine
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.

In addition to well-known mechanisms of excitation of solar and stellar oscillations by turbulent convection and instabilities, the oscillations can be excited by an impulsive localized force caused by the energy release in solar and stellar flares. Such oscillations have been observed on the Sun (‘sunquakes’), and created a lot of interesting discussions about physical mechanisms of the impulsive excitation and their relationship to the flare physics. The observation and theory have shown that most of a sunquake's energy is released in high-degree, high-frequency p modes. In addition, there have been reports on helioseismic observations of low-degree modes excited by strong solar flares. Much more powerful flares observed on other stars can cause ‘starquakes’ of substantially higher amplitude. Observations of such oscillations can provide new asteroseismic information and also constraints on mechanisms of stellar flares. I discuss the basic properties of sunquakes, and initial attempts to detect flare-excited oscillations in Kepler short-cadence data.

Keywords

Sun: flaresoscillationsstars: flaresoscillations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S301: Precision Asteroseismology , August 2013 , pp. 349 - 352
Copyright
Copyright © International Astronomical Union 2014 

References

Balona, L. A. 2012, MNRAS, 423, 3420Google Scholar
Bryson, S., Kosovichev, A., & Levy, D. 2005, Physica D Nonlinear Phenomena, 201, 1Google Scholar
Chaplin, W. J., Basu, S., Huber, D., et al. 2014, ApJS, 210, 1Google Scholar
Contadakis, M. E. 2012, in: Papadakis, I. & Anastasiadis, A. (eds.), 10th Hellenic Astronomical Conference, p. 27Google Scholar
Contadakis, M. E., Avgoloupis, S. J., & Seiradakis, J. H. 2012, AN, 333, 583Google Scholar
Jakimiec, J. & Tomczak, M. 2012, Solar Phys., 278, 393CrossRefGoogle Scholar
Karoff, C. & Kjeldsen, H. 2008, ApJ, 678, L73Google Scholar
Koljonen, K. I. I., Hannikainen, D. C., & McCollough, M. L. 2011, MNRAS, 416, L84CrossRefGoogle Scholar
Kosovichev, A. G. 2006, Solar Phys., 238, 1CrossRefGoogle Scholar
Kosovichev, A. G. 2009, AIP-CS, 1170, 547Google Scholar
Maehara, H., Shibayama, T., Notsu, S., et al. 2012, Nature, 485, 478Google Scholar
Qian, S.-B., Zhang, J., Zhu, L.-Y., et al. 2012, MNRAS, 423, 3646Google Scholar
Walkowicz, L. M., Basri, G., Batalha, N., et al. 2011, AJ, 141, 50Google Scholar