A Study of Acoustic Halos in Active Region NOAA 11330 using Multi-Height SDO Observations

TL;DR

This study investigates the spatial and temporal distribution of acoustic power in solar active regions using multi-height observations from SDO, revealing how acoustic halos depend on magnetic field properties and observation height.

Contribution

It provides a detailed analysis of acoustic halos across different heights and magnetic conditions, offering new insights into wave behavior in solar active regions.

Findings

Acoustic halos occur above the acoustic cutoff frequency up to 10 mHz.

Halos are strongly influenced by magnetic field strength and inclination.

Wave characteristics vary with observation height, as shown by phase and coherence spectra.

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 \AA\ as well as intensity at 1600 \AA\ and 1700 \AA. 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 \AA\ 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.