HR: 1330h
AN: SP13A-01    [Abstracts]
TI: Five-Minute Power Maps From GONG and MDI.
AU: * Howe, R
EM: rhowe@noao.edu
AF: National Solar Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719 United States
AU: Komm, R W
EM: komm@noao.edu
AF: National Solar Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719 United States
AU: Hill, F
EM: hill@noao.edu
AF: National Solar Observatory, 950 N. Cherry Avenue, Tucson, AZ 85719 United States
AU: Haber, D A
EM: dhaber@solarz.colorado.edu
AF: JILA and Department of Atmospheric and Planetary Sciences, University of Colorado, Boulder, CO 80309 United States
AU: Hindman, B W
EM: hindman@solarz.colorado.edu
AF: JILA and Department of Atmospheric and Planetary Sciences, University of Colorado, Boulder, CO 80309 United States
AB: The presence of magnetic active regions on the solar surface is well known to influence the detected power of the oscillation signal. We consider maps of the five-minute power in the velocity signal from Global Oscillations Network Group (GONG) observations covering much of the disk over multiple Carrington Rotations, and compare these in detail with magnetic and continuum intensity images, with estimates of the velocity power from ring diagram helioseismic analysis, and also with a small sample of contemporaneous MDI (Michelson Doppler Imager) data. The comparison of power maps with magnetograms is carried out at a pixel-by-pixel level, for averages over patches of 16× 16 degrees in heliographic latitude and longitude, and at some intermediate scales. This research was supported by the National Science Foundation and NASA.
DE: 7500 SOLAR PHYSICS, ASTROPHYSICS, AND ASTRONOMY
DE: 7522 Helioseismology
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly