Solar Interior and Helioseismology

Physics

Scientific paper

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Scientific paper

The Sun vibrates in many different modes of acoustic oscillations excited by convection. These modes are sensitive to the internal properties of the Sun and thus inferences can be drawn about the interior from surface observations of wave motions. Helioseismology is a powerful tool to test and refine the physics of stellar interiors, but also to search for clues regarding the origin and variability of the Sun's magnetic field, possibly the most important unsolved problem in solar physics. A selected overview of recent results in helioseismology will be presented. Particular emphasis will be placed on how to observe and model the effect of magnetic structures, and active regions in particular, on wave propagation. According to theory, the correlations in the seismic wave field contain all the information needed to estimate the Green's function between two spatial locations. This will be demonstrated using MDI/SOHO observations as well as numerical simulations of small-amplitude MHD waves. A general discussion of the helioseismological inverse problem will follow.
This presentation would not be complete without mentioning the Helioseismic and Magnetic Imager (HMI), an experiment to be launched at the beginning of 2009 onboard the Solar Dynamics Observatory (SDO). HMI/SDO will continuously provide full-disk Doppler images at high spatial resolution, and will lead to important advances in local helioseismology. While SDO is a significant technological step beyond SOHO, the solar scientific community is to be inundated with a flood of large-volume data. The establishment of the DLR German Data Center for SDO will provide an advanced data management system to effectively deliver rapid and simple access to users and developers in Germany and, hopefully, throughout Europe.

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