Emerging dimmings of active regions observed by SDO

TL;DR

This study statistically analyzes emerging dimmings in active regions observed by SDO, revealing their timing, shape, duration, and magnetic flux changes, and linking them to magnetic reconnection processes.

Contribution

It provides the first comprehensive statistical characterization of emerging dimmings, including their types, timing, and magnetic flux evolution, based on SDO observations.

Findings

Emerging dimmings occur several hours after active region emergence.

Two types of EDs: fan-shaped and halo-shaped.

EDs are associated with magnetic flux reconfiguration and reconnection.

Abstract

With the observations from the Atmospheric Imaging Assembly and the Helioseismic and Magnetic Imager aboard the \emph{Solar Dynamics Observatory}, we statistically investigate the emerging dimmings (EDs) of 24 isolated active regions (IARs) from June 2010 to May 2011. All the IARs present EDs in lower temperature lines (e.g., 171 {\AA}) at their early emerging stages, meanwhile in higher temperature lines (e.g., 211 {\AA}), the ED regions brighten continuously. There are two type of EDs: fan-shaped and halo-shaped. There are 19 fan-shaped EDs and 5 halo-shaped ones. The EDs appear several to more than ten hours delay to the first emergence of the IARs. The shortest delay is 3.6 hr and the longest 19.0 hr. The EDs last from 3.3 hr to 14.2 hr, with a mean duration of 8.3 hr. Before the appearance of the EDs, the emergence rate of the magnetic flux of the IARs is from 1.2 $\times$ 10$^{19}$ Mx hr$^{-1}$ to 1.4 $\times$ 10$^{20}$ Mx hr$^{-1}$. The larger the emergence rate is, the shorter the delay time is. While the dimmings appear, the magnetic flux of the IARs ranges from 8.8 $\times$ 10$^{19}$ Mx to 1.3 $\times$ 10$^{21}$ Mx. These observations imply that the reconfiguration of the coronal magnetic fields due to reconnection between the newly-emerging flux and the surrounding existing fields results in a new thermal distribution which leads to a dimming for the cooler channel (171 {\AA}) and brightnening in the warmer channels.