Helioseismology is probing the interior structure and dynamics of the sun with ever-increasing precision, providing a well-calibrated laboratory in which physical processes can be studied under conditions that are unattainable on Earth. Nearly 10 million resonant modes of oscillation are observable in the solar atmosphere, and their frequencies need to be known with great accuracy in order to gauge the sun's interior. The advent of nearly continuous imaged observations from the complementary ground-based Global Oscillation Network Group (GONG) observatories and the space-based Solar and Heliospheric Observatory instruments augurs a new era of discovery. The flow of early results from GONG resolves some issues and raises a number of theoretical questions whose answers are required for understanding how a seemingly ordinary star actually operates.
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Dispersion relations, rays and ray splitting in magnetohelioseismology.
Philos Trans A Math Phys Eng Sci
February 2006
Centre for Stellar and Planetary Astrophysics, School of Mathematical Sciences, Monash University, Clayton, Victoria 3800, Australia.
Local helioseismology seeks to probe the near surface regions of the Sun, and in particular of active regions. These are distinguished by their strong magnetic fields, yet current local techniques do not take proper account of this. Here, we first derive appropriate gravito-magneto-acoustic dispersion relations, and then use these to examine how acoustic rays entering regions of strong field split into fast and slow components, and the subsequent fates of each.
View Article and Find Full Text PDFPerspectives in Helioseismology.
Science
May 1996
D. O. Gough is with the Institute of Astronomy, University of Cambridge, Cambridge, CB3 OHA UK. J. W. Leibacher is with the National Solar Observatory, Tucson, AZ, USA. P. H. Scherrer is with the Department of Physics, Stanford University, Stanford, CA, USA. J. Toomre is with JILA, University of Colorado, Boulder, CO, USA.
Helioseismology is probing the interior structure and dynamics of the sun with ever-increasing precision, providing a well-calibrated laboratory in which physical processes can be studied under conditions that are unattainable on Earth. Nearly 10 million resonant modes of oscillation are observable in the solar atmosphere, and their frequencies need to be known with great accuracy in order to gauge the sun's interior. The advent of nearly continuous imaged observations from the complementary ground-based Global Oscillation Network Group (GONG) observatories and the space-based Solar and Heliospheric Observatory instruments augurs a new era of discovery.
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