Emerging Flux Simulations and Proto-Active Regions

TL;DR

This paper presents simulations of magnetic flux emergence from deep within the Sun, demonstrating the formation of pores and spots, and analyzing their magnetic properties and observational signatures.

Contribution

It introduces a simulation approach for magnetic flux emergence that produces realistic pore and spot structures with detailed magnetic field analysis.

Findings

Magnetic flux emerges first as a mixed polarity pattern.

Strong vertical fields form persistent spots, weak fields dissipate.

Simulated Stokes profiles match observational effects.

Abstract

The emergence of minimally structured (uniform and horizontal) magnetic field from a depth of 20 Mm has been simulated. The field emerges first in a mixed polarity pepper and salt pattern, but then collects into separate, unipolar concentrations and produces pores. The field strength was then artificially increased to produce spot-like structures. The field strength at continuum optical depth unity peaks at 1 kG, with a maximum of 4 kG. Where the vertical field is strong, the spots persist (at present an hour of solar time has been simulated). Where the field is weak, the spot gets filled in and disappears. Stokes profiles have been calculated and processed with the Hinode annular mtf, the slit diffraction and frequency smoothing. These data are available at steinr.pa.msu.edu/~bob/stokes.