Simulated Magnetic Flows in the Solar Photosphere

TL;DR

This study uses realistic MHD simulations to investigate the origin of supersonic magnetic flows observed in the solar photosphere, comparing synthetic signals with actual observations to understand their formation mechanisms.

Contribution

The paper introduces detailed MHD simulations of magnetic flux emergence and cancellation, linking these processes to observed supersonic flows in the solar photosphere.

Findings

Simulated events are smaller and mostly associated with downflows compared to observations.

Strong line-of-sight velocities with magnetic fields produce significant Stokes V signals.

Emergence of magnetic flux increases the occurrence of high-speed magnetized flows.

Abstract

Recent Sunrise/IMaX observations have revealed the existence of supersonic magnetic flows. Our aim is to determine the origin of such flows by using realistic MHD simulations. We simulate cancellation and emergence of magnetic flux through the solar photosphere. Our first numerical experiment starts with magnetic field of both polarities. To simulate emergence into a region with pre-existing field, we introduce a large-scale horizontally uniform sheet of horizontal field. We follow the subsequent evolution, creating synthetic polarimetric observations, including known instrumental effects of the Sunrise/IMaX and Hinode/SP instruments. We compare the simulated and observed spectropolarimetric signals. Strongly blue- and redshifted Stokes V signals are produced in locations where strong line-of-sight velocities coincide with the strong line-of-sight component of magnetic field. The size and strength of simulated events is smaller than observed and they are mostly associated with downflows, contrary to observations. In a few cases where they appear above a granule, single blue lobed Stokes V are produced due to strong gradients in magnetic field and velocity. No change of magnetic field sign is detected along the line of sight in these instances. More high-speed magnetized flows occur in the case where emergence is simulated than in the case where no horizontal field was added. The simulations indicate that the observed events result from magnetic flux emergence, where reconnection may take place but does not seem to be necessary.