HR: 1330h
AN: SH13C-11    [Abstracts]
TI: Acoustic Mapping of the Magnetic Canopy in the Solar Chromosphere
AU: * Jefferies, S M
EM: stuartj@msrc.unm.edu
AF: Maui Scientific Research Center, University of New Mexico, 590 Lipoa Parkway, Ste 262, Kihei, HI 96753 United States
AU: Armstrong, J D
EM: jd@msrc.unm.edu
AF: Maui Scientific Research Center, University of New Mexico, 590 Lipoa Parkway, Ste 262, Kihei, HI 96753 United States
AU: Cacciani, A
EM: alessandro@nso.edu
AF: Dipartimento di Fisica, Universita degli Studi di Roma "La Sapienza", Piazzale Aldo Moro 2, Roma, I-00185 Italy
AU: Finsterle, W
EM: wolfgang@pmodwrc.ch
AF: Department Radiometry, World Radiation Center, Dorfstrasse 33, Davos, CH-7260 Switzerland
AU: McIntosh, S W
EM: mcintosh@boulder.swrc.edu
AF: South West Research Institute, 1050 Wlanut Street, Suite 400, Boulder, CO 80302 United States
AB: We show that high-frequency acoustic waves can be used to map the location where the gas and magnetic pressures of the plasma in the solar chromosphere are comparable. This transition region, which can be considered as a "magnetic canopy" where MHD waves can transform from one type into another, is believe to play a key role in the flow of mass and energy through the chromosphere. Results will be presented from the analysis of 18 (uninterrupted) hours of simultaneous, full-disk, velocity observations using the Ni (676 nm), K (770 nm) and Na (589 nm) Fraunhofer lines (with the SOHO/MDI and MOTH/South Pole instruments), and 106 (uninterrupted) hours of K and Na data (from the MOTH/South Pole instrument). The MOTH data were acquired every 10 seconds and the MDI data every 60 seconds. This work was funded by awards OPP-0087541 and OPP-0338251 from the National Science Foundation.
DE: 7500 SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY
DE: 7507 Chromosphere
DE: 7522 Helioseismology
DE: 7524 Magnetic fields
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2005 Joint Assembly