HR: 0800h
AN: SH21A-0289    [Abstracts]
TI: Alfven Waves in the Solar Corona
AU: * Tomczyk, S
EM: tomczyk@ucar.edu
AF: HAO/NCAR, 1850 Table Mesa Dr., Boulder, CO 80305, United States
AU: McIntosh, S W
EM: mcintosh@boulder.swri.edu
AF: HAO/NCAR, 1850 Table Mesa Dr., Boulder, CO 80305, United States
AU: McIntosh, S W
EM: mcintosh@boulder.swri.edu
AF: Southwest Research Institute, 1050 Walnut St., Boulder, CO 80302, United States
AU: Keil, S L
EM: skeil@nso.edu
AF: National Solar Observatory, 1 Loop Drive, Sunspot, NM 88349, United States
AU: Judge, P G
EM: judge@ucar.edu
AF: HAO/NCAR, 1850 Table Mesa Dr., Boulder, CO 80305, United States
AU: Schad, T
EM: schad@noao.edu
AF: University of Notre Dame, 225 Nieuwland Science Hall, Notre Dame, IN 46556, United States
AU: Seeley, D H
EM: dseeley@framingham.k12.ma.us
AF: Framingham High School, 115 A Street, Framingham, MA 01701, United States
AU: Edmondson, J
EM: jkedmond@gmail.com
AF: University of Michigan, 2455 Hayward Street, Ann Arbor, MI 48109, United States
AB: We present observations of the coronal intensity, line-of-sight velocity, and linear polarization obtained in the FeXIII 1074.7 nm coronal emission line with the Coronal Multi-channel Polarimeter (CoMP) instrument. Analysis of these observations reveal ubiquitous upward propagating waves with phase speeds of 1-4 Mm/s and trajectories consistent with the direction of the magnetic field inferred from the linear polarization measurements. We can definitively identify these as Alfvén waves. An estimate of the energy carried by the waves that we spatially resolve indicates that they are unable to heat the solar corona, however, unresolved waves may carry sufficient energy.
DE: 7509 Corona
DE: 7594 Instruments and techniques
DE: 7836 MHD waves and instabilities (2149, 2752, 6050)
SC: SPA-Solar and Heliospheric Physics [SH]
MN: 2007 Fall Meeting