A Study of the relation between intensity oscillations and magnetic field parameters in a Sunspot: Hinode Observations

TL;DR

This study investigates how intensity oscillations in a sunspot relate to magnetic field parameters in the photosphere and chromosphere using Hinode observations, revealing frequency-dependent power variations and correlations with magnetic components.

Contribution

It provides new insights into the relationship between intensity oscillations and magnetic field components across different layers of a sunspot, using simultaneous imaging and spectropolarimetric data.

Findings

Gband power decreases with increasing magnetic field strength.

CaIIH shows more high-frequency power in stronger fields.

Sunspot umbral power is anti-correlated with magnetic strength, except at low frequencies.

Abstract

We present properties of intensity oscillations of a sunspot in the photosphere and chromosphere using G~band and CaIIH filtergrams from Hinode. Intensity power maps as function of magnetic field strength and frequency reveal reduction of power in Gband with increase in photospheric magnetic field strength at all frequencies. In CaIIH, however, stronger fields exhibit more power at high frequencies particularly in the 4.5 mHz-8.0 mHz band. Power distribution in different locations of the active region show that the oscillations in CaIIH exhibit more power in comparison to that of Gband. We also relate the power in intensity oscillations with different components of the photospheric vector magnetic field using near simultaneous spectro-polarimetric observations of the sunspot from the Hinode spectropolarimeter. The photospheric umbral power is strongly anti-correlated with the magnetic field strength and its the line-of-sight component while there is a good correlation with the transverse component. A reversal of this trend is observed in the chromosphere with the exception at low frequencies ($\nu\le$ 1.5 mHz). The power in sunspot penumbrae is anti-correlated with the magnetic field parameters at all frequencies (1.0 $\le\nu\le$ 8.0 mHz) in both the photosphere and chromosphere, except that the chromospheric power shows a strong correlation in the frequency range 3-3.5 mHz.