Magnetic properties of the umbral boundary during sunspot decay. Comparative study of multiple datasets

TL;DR

This study compares magnetic and intensity properties at sunspot boundaries during decay using Hinode and SDO datasets, revealing how these properties evolve and differ across datasets and decay stages.

Contribution

It provides a detailed comparative analysis of magnetic and intensity boundary properties during sunspot decay using multiple datasets, highlighting dataset discrepancies and decay processes.

Findings

Good correspondence between Hinode and HMI_dcon magnetic maps.

Continuum intensity differences due to scattered light effects.

Slow boundary evolution during decay with abrupt changes in naked-spot stage.

Abstract

The magnetic properties of the umbra-penumbra (UP) boundary of sunspots and the boundary of pores at various evolutionary stages have been characterised using datasets from different instruments. We aim to study the differences between the intensity and vector magnetic field properties derived from Hinode/SP and SDO/HMI observations of a decaying sunspot. We analysed the sunspot embedded in AR 12797 during six days in 30 SP/Hinode scans and 704 HMI/SDO for both regular maps and HMI_dcon. We studied the correlation of the magnetic properties and continuum intensity in the datasets within the spot, and at the UP boundary. We examined the decaying process using the full temporal resolution of the HMI_dcon maps. We find a good correspondence between the magnetic properties in the SP and HMI_dcon maps, but the continuum intensity of the spots in the SP maps is 0.04I_qs brighter than in the HMI_dcon maps. The influence of scattered light in the HMI maps makes it the least ideal dataset for studying the boundary of spots without a penumbra. The properties at the UP boundary evolve slowly during the sunspot decay stage, while the penumbra still provides some stability. In contrast, they respond more abruptly to areal changes in the naked-spot stage. During the sunspot decay, we find linear decay in the area and in the magnetic flux. Moreover, the umbra shows two characteristic decaying processes: a slow decay during the first three days, and a sudden fast decay during the final dissipation of the penumbra. We find indications of a 3.5h lag between the dissipation of the vertical fields in the umbral region and the photometric decay of the umbral area. The differences found in the continuum intensity and in the vertical component of the magnetic field, Bver, between the analysed datasets explain the discrepancies among the Bver values found at the boundaries of umbrae in previous studies.