On the (in)stability of sunspots

TL;DR

This study investigates the stability mechanisms of sunspots using 3D MURaM simulations, revealing how buoyancy, fluting instability, and magnetic tension influence sunspot stability and decay at various depths.

Contribution

It provides a detailed analysis of the depth-dependent stability factors affecting sunspots, highlighting the role of fluting instability and buoyancy forces in their evolution.

Findings

Sunspots are stabilized by buoyancy forces above 2 Mm depth.

Fluting instability peaks at about 3 Mm depth, destabilizing the flux tube.

Deeper layers show slower corrugation due to magnetic tension and field orientation.

Abstract

The stability of sunspots is one of the long-standing unsolved puzzles in the field of solar magnetism. We study the effects that destabilise and stabilise the flux tube of a simulated sunspot in the upper convection zone. The depth-varying effects of fluting instability, buoyancy forces, and timescales on the flux tube are analysed. The simulation was calculated with the MURaM code. The domain has a lateral extension of 98 Mm x 98 Mm and extends almost 18 Mm below the solar surface. The analysed data set of 30 hours shows a stable sunspot at the solar surface. We studied the evolution of the flux tube at horizontal layers by means of the relative change in perimeter and area with a linear stability analysis. We find a corrugation along the perimeter of the flux tube that proceeds fastest at a depth of about 8 Mm below the surface. Towards the surface and towards deeper layers, the decrease in compactness is damped. From the stability analysis, we find that above a depth of 2 Mm, the sunspot is stabilised by buoyancy forces. The spot is least stable at a depth of about 3 Mm because of fluting instability. The stability of the sunspot at the surface affects the behaviour of the field lines in deeper layers by magnetic tension. Therefore the fluting instability is damped at depths of about 3 Mm, and the decrease in compactness is strongest at a depth of about 8 Mm. The more vertical orientation of the magnetic field and the longer convective timescale slow down the corrugation process in layers deeper than 10 Mm. The formation of large intrusions of field-free plasma below the surface destabilises the sunspot, and eventually lead to the disruption and decay of the sunspot. This process is not visible at the surface, where the sunspot is stabilised by buoyancy forces. The onset of sunspot decay occurs in deeper layers, while the sunspot still appears stable in the photosphere.