Comparison of transient horizontal magnetic fields in a plage region and in the quiet Sun

TL;DR

This study compares transient horizontal magnetic fields in plage and quiet Sun regions, revealing similar occurrence rates and field strength distributions, suggesting a local dynamo process generates these fields across the Sun.

Contribution

It provides the first detailed comparison of THMF properties in plage and quiet Sun, highlighting the role of local dynamo processes and large-scale magnetic influence.

Findings

Occurrence rates of THMFs are similar in plage and quiet Sun.

Vertical magnetic flux is significantly larger in plage regions.

Higher LP THMFs in plage show preferred orientation aligned with large-scale fields.

Abstract

Properties of transient horizontal magnetic fields (THMFs) in both plage and quiet Sun regions are obtained and compared. Spectro-polarimetric observations with the Solar Optical Telescope (SOT) on the Hinode satellite were carried out with a cadence of about 30 seconds for both plage and quiet regions located near disk center. We select THMFs that have net linear polarization (LP) higher than 0.22%, and an area larger than or equal to 3 pixels, and compare their occurrence rates and distribution of magnetic field azimuth. We obtain probability density functions (PDFs) of magnetic field strength and inclination for both regions.The occurrence rate in the plage region is the same as for the quiet Sun. The vertical magnetic flux in the plage region is ~8 times larger than in the quiet Sun. There is essentially no preferred orientation for the THMFs in either region. However, THMFs in the plage region with higher LP have a preferred direction consistent with that of the plage-region's large-scale vertical field pattern. PDFs show that there is no difference in the distribution of field strength of horizontal fields between the quiet Sun and the plage regions when we avoid the persistent large vertical flux concentrations for the plage region. The similarity of the PDFs and of the occurrence rates in plage and quiet regions suggests that a local dynamo process due to the granular motion may generate THMFs all over the sun. The preferred orientation for higher LP in the plage indicates that the THMFs are somewhat influenced by the larger-scale magnetic field pattern of the plage.