# Spatial Distributions of Sunspot Oscillation Modes at Different Temperatures

## TL;DR

This study investigates how sunspot oscillation modes at different temperatures distribute spatially across solar atmospheric layers, revealing temperature-dependent patterns and suppression effects in high-temperature regions.

## Contribution

It provides detailed observations of sunspot oscillation spatial distributions across multiple atmospheric layers, highlighting temperature-dependent changes and the suppression of five-minute oscillations at higher temperatures.

## Key findings

- Five-minute oscillation powers form expanding circle shapes with increasing temperature.
- High-temperature regions suppress five-minute oscillations, leading to disordered power distributions.
- Three-minute oscillations are concentrated within the umbra and at coronal loop footpoints.

## Abstract

Three- and five-minute oscillations of sunspots have different spatial distributions in the solar atmospheric layers. The spatial distributions are crucial to reveal the physical origin of sunspot oscillations and to investigate their propagation. In this study, six sunspots observed by Solar Dynamics Observatory/Atmospheric Imaging Assembly were used to obtain the spatial distributions of three- and five-minute oscillations. The fast Fourier transform method is applied to represent the power spectra of oscillation modes. We find that, from the temperature minimum to the lower corona, the powers of the five-minute oscillation exhibit a circle-shape distribution around its umbra, and the shapes gradually expand with temperature increase. However, the circle-shape is disappeared and the powers of the oscillations appear to be very disordered in the higher corona. This indicates that the five-minute oscillation can be suppressed in the high-temperature region. For the three-minute oscillations, from the temperature minimum to the high corona, their powers mostly distribute within an umbra, and part of them locate at the coronal fan loop structures. Moreover, those relative higher powers are mostly concentrated in the position of coronal loop footpoints.