Oscillatory Power Distribution in Full-disk Magnetograms

This work utilizes data obtained by the Global Oscillation Network Group (GONG) program, managed by the National Solar Observatory, which is operated by AURA, Inc. under a cooperative agreement with the National Science Foundation. The data were acquired by instruments operated by the Big Bear Solar Observatory, High Altitude Observatory, Learmonth Solar Observatory, Udaipur Solar Observatory, Instituto de Astrofisica de Canarias, and Cerro Tololo Interamerican Observatory. This work was supported by NASA grant NNG 08E154I. Motivation: The interaction of acoustic waves with magnetic plasma modifies the observed amplitude of the propagating waves. Observations suggest that the amplitude of p modes in the 3-mHz band is suppressed in regions of strong magnetic field while it is enhanced at frequencies above 5 mHz. These results provide information about the nature of the propagation of waves in the solar atmosphere and the conditions in the thermal cavity where the modes are trapped.