Abstract:
We analyze data from the Helioseismic Magnetic Imager (HMI) and the Atmospheric Imaging Assembly (AIA) instruments on board
the Solar Dynamics Observatory (SDO) to characterize the spatio-temporal acoustic power distribution in active regions as a function of
the height in the solar atmosphere. For this, we use Doppler velocity and continuum intensity observed using the magnetically sensitive
line at 6173 A as well as intensity at 1600 A and 1700 A. We focus on the power enhancements seen around AR 11330 as a function of
wave frequency, magnetic field strength, field inclination and observation height. We find that acoustic halos occur above the acoustic
cutoff frequency and extends up to 10 mHz in HMI Doppler and AIA 1700 A observations. Halos are also found to be strong functions
of magnetic field and their inclination angle. We further calculate and examine the spatially averaged relative phases and cross-coherence
spectra and find different wave characteristics at different heights.
