Computer Science – Sound
Scientific paper
Dec 2002
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufmsh21c..06k&link_type=abstract
American Geophysical Union, Fall Meeting 2002, abstract #SH21C-06
Computer Science
Sound
7522 Helioseismology, 7529 Photosphere, 7536 Solar Activity Cycle (2162), 7544 Stellar Interiors And Dynamo Theory, 7594 Instruments And Techniques
Scientific paper
Helioseismic and Magnetic Imager on board SDO will significantly expand the possibilities for imaging plasma flows and structures in the solar interior. It will provide for the first time high-resolution data for continuous monitoring of emerging flux and developing active regions in the upper convection zone. It will also allow us to look for localized structures and flows in the tachocline region and deeper interior, and also investigate the near-polar regions. The expected results may give important clues of how the solar dynamo works and active regions develop. HMI will observe the entire spectrum of the solar acoustic and surface gravity waves, and provide the most comprehensive data for global and local helioseismology. The high-frequency part of the oscillation spectrum will be used for studying seismic properties of the solar atmosphere in the quiet Sun and active regions. The method of acoustic tomography or time-distance helioseismology is one of the primary tools of the HMI investigation. It is based on measurements and inversions of travel-time delays of solar waves, caused by plasma flows and variations of temperature and magnetic field. The data analysis requires deep understanding of the physics of wave propagation in the Sun and substantial computer resources. One of the important goals is to provide the flow and sound-speed maps of the upper convection zone in near-real time for space weather applications. We present the current status of the field, and discuss plans and challenges for the HMI data analyses and interpretation.
Birch Aaron C.
Duvall Thomas L.
Gizon Laurent
Kosovichev Aleksandr G.
Sekii Takashi
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