Detailed analysis of dynamic evolution of three Active Regions before flare and CME occurrence at the photospheric level

TL;DR

This study analyzes the evolution of magnetic parameters in three active regions before solar flares and CMEs, revealing a shared U-shaped pattern that could improve eruption forecasting.

Contribution

It identifies a common U-shaped pattern in magnetic parameters prior to eruptions, linking shearing motion to solar flare and CME initiation, enhancing predictive capabilities.

Findings

Shared U-shaped pattern in magnetic parameters before eruptions

Shearing motion may be a key driver for solar eruptions

Decreasing-approaching pattern in shearing helicity as a precursor

Abstract

We present a combined analysis of the applications of the weighted horizontal magnetic gradient (denoted as WG_M in Korsos et al., ApJ, 802, L21, 2015) method and the magnetic helicity tool (Berger & Field, JFM, 147, 133, 1984) employed for three active regions (ARs), namely NOAA AR11261, AR11283 and AR11429. All three active regions produced series flares and CMEs. We followed the evolution of the components of the WG_M and the magnetic helicity before the flare and CME occurrences. We found an unique and mutually shared behavior, called the U-shaped pattern, of the weighted distance component of WG_M and of the shearing component of the helicity flux before the flare and CME eruptions. This common pattern is associated with the decreasing-receding phase yet reported only known to be a necessary feature prior to solar flare eruption(s), but found now at the same time in the evolution of the shearing helicity parameter. This result leads to the conclusion that (i) the shearing motion of photospheric magnetic field may be a key driver for the solar eruption in addition to the flux emerging process, and that (ii) the found decreasing-approaching pattern in the evolution of shearing helicity may be another precursor indicator for improving the forecasting of solar eruptions.