K. Galsgaard, M. S. Madjarska, K. Vanninathan, Z. Huang and M. Presmann

Active region upflows. II. Data driven magnetohydrodynamic

Figure 10. The magnetic field line structure is shown in the same way as in Fig. 5. Additionally, the red/purple blobs represent the vertical down/up flow velocities indicating the compression/decompression patterns of the propagating waves.

Abstract

Context. Observations of many active regions show a slow systematic outflow/upflow from their edges lasting from hours to days. At present no physical explanation has been proven, while several suggestions have been put forward.

Aims. This paper investigates one possible method for maintaining these upflows assuming that convective motions drive the magnetic field to initiate them through magnetic reconnection.

Methods. We use Helioseismic and Magnetic Imager (HMI) data to provide an initial potential three dimensional magnetic field of the active region NOAA 11123 on 2010 November 13 where the characteristic upflow velocities are observed. A simple one-dimensional hydrostatic atmospheric model covering the region from the photosphere to the corona is derived. Local Correlation Tracking of the magnetic features in the HMI data is used to derive a proxy for the time dependent velocity field. The time dependent evolution of the system is solved using a resistive three-dimensional MagnetoHydro-Dynamic code.

Results. The magnetic field contains several null points located well above the photosphere, with their fan planes dividing the mag- netic field into independent open and closed flux domains. The stressing of the interfaces between the different flux domains is expected to provide locations where magnetic reconnection can take place and drive systematic flows. In this case, the region between the closed and open flux is identified as the region where observations find the systematic upflows.

Conclusions. In the present experiment, the driving only initiates magneto-acoustic waves, without driving any systematic upflows at any of the flux interfaces.

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Last Revised: 2015 October 14th