Atmospheric oscillatory behaviour of magnetic helicity flux in eruptive and non-eruptive Active Regions
Abstract
The magnetic helicity slowly and continuously accumulates in response to plasma flows tangential to the photosphere and magnetic flux emergence normal to it, it into the solar atmosphere. Analysing the evolution of magnetic helicity flux at different atmospheric heights is key for identifying its role in the dynamics of active regions (ARs). The three-dimensional magnetic field is studied of eruptive and non-eruptive ARs. The magnetic field is constructed using field extrapolations. For each studied flaring and non-flaring ARs, the emergence, shearing, and total magnetic helicity components are derived at different atmospheric heights. Oscillatory behaviour is searched for in these obtained magnetic helicity components. In the eruptive ARs, we found that the largest period of the three helicity fluxes are common from the photosphere up to at least 1Mm above the photosphere. The non-eruptive ARs do not show this kind of coupled oscillatory behaviour as the eruptive ARs. Therefore, we suggest that when the vertical and horizontal helicity flux components became a coupled oscillatory system from the photosphere up to the chromosphere then this particular oscillatory feature of the AR could produce large energetic solar eruptions.
- Publication:
-
44th COSPAR Scientific Assembly. Held 16-24 July
- Pub Date:
- July 2022
- Bibcode:
- 2022cosp...44.2426K