Hostname: page-component-cd9895bd7-dzt6s Total loading time: 0 Render date: 2024-12-25T17:22:06.427Z Has data issue: false hasContentIssue false
  • English
  • Français

Investigations of solar plasma in the interior and corona from Solar Dynamics Observatory

Published online by Cambridge University Press:  08 June 2011

A. G. Kosovichev
A. G. Kosovichev*
Affiliation:
W. W. Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, [email protected]
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.

The Sun is a plasma laboratory for astrophysics, which allows us to investigate many important phenomena in turbulent magnetized plasma in detail. Solar Dynamics Observatory (SDO) launched in February 2010 provides unique information about plasma processes from the interior to the corona. The primary processes of magnetic field generation and formation of magnetic structures are hidden beneath the visible surface. Helioseismic diagnostics, based on observations and analysis of solar oscillations and waves, give insights into the physical processes in the solar interior and mechanisms of solar magnetic activity. In addition, simultaneous high-resolution multi-wavelength observations of the solar corona provide opportunity to investigate in unprecedented detail the coronal dynamics and links to the interior processes. These capabilities are illustrated by initial results on the large-scale dynamics of the Sun, the subsurface structure and dynamics of a sunspot and observations of a X-class solar flare.

Keywords

PlasmasSun: helioseismologymagnetic fieldssunspotsphotosphereflares
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S274: Advances in Plasma Astrophysics , September 2010 , pp. 287 - 290
Copyright
Copyright © International Astronomical Union 2011

References

Golub, L. 2006, Sp. Sci. Rev., 124, 23CrossRefGoogle Scholar
Kitiashvili, I. N., Kosovichev, A. G., Wray, A. A., & Mansour, N. N. 2010, ApJ, 719, 307.CrossRefGoogle Scholar
Kosovichev, A. G. & HMI Science Team 2007, Astron. Nach., 328, 339CrossRefGoogle Scholar
Kosovichev, A. G. 2011, arXiv:1102.3954Google Scholar
Schou, J., et al. . 2010, Sol. Phys, in press.Google Scholar
Woods, T. N., et al. . 2010, Sol. Phys, in pressGoogle Scholar
Zhao, J., Kosovichev, A. G., & Sekii, T. 2010, ApJ, 708, 304CrossRefGoogle Scholar
Zhao, J., et al. . 2011, Sol, Phys., submitted.Google Scholar