Volume 509, January 2010
|Number of page(s)||9|
|Published online||21 January 2010|
Magnetic field intensification: comparison of 3D MHD simulations with Hinode/SP results
Max-Planck-Institut für Sonnensystemforschung,
Max-Planck-Straße 2, 37191 Katlenburg-Lindau,
Germany e-mail: email@example.com
2 Astronomical Observatory, Volgina 7, 11160 Belgrade 74, Serbia
3 School of Space Research, Kyung Hee University, Yongin, Gyeonggi, 446-701, Korea
Accepted: 9 October 2009
Context. Recent spectro-polarimetric observations have provided detailed measurements of magnetic field, velocity and intensity during events of magnetic field intensification in the solar photosphere.
Aims. By comparing with synthetic observations derived from MHD simulations, we investigate the physical processes underlying the observations, as well as verify the simulations and the interpretation of the observations.
Methods. We consider the temporal evolution of the relevant physical quantities for three cases of magnetic field intensification in a numerical simulation. In order to compare with observations, we calculate Stokes profiles and take into account the spectral and spatial resolution of the spectropolarimeter (SP) on board Hinode. We determine the evolution of the intensity, magnetic flux density and zero-crossing velocity derived from the synthetic Stokes parameters, using the same methods as applied to the Hinode/SP observations to derive magnetic field and velocity information from the spectro-polarimetric data.
Results. The three events considered show a similar evolution: advection of magnetic flux to a granular vertex, development of a strong downflow, evacuation of the magnetic feature, increase of the field strength and the appearance of the bright point. The magnetic features formed have diameters of 0.1-0.2´´. The downflow velocities reach maximum values of 5-10 km s-1 at τ = 1. In the largest feature, the downflow reaches supersonic speed in the lower photosphere. In the same case, a supersonic upflow develops approximately 200 s after the formation of the flux concentration. We find that synthetic and real observations are qualitatively consistent and, for one of the cases considered, also agree very well quantitatively. The effect of finite resolution (spatial smearing) is most pronounced in the case of small features, for which the synthetic Hinode/SP observations miss the bright point formation and also the high-velocity downflows during the formation of the smaller magnetic features.
Conclusions. The observed events are consistent with the process of field intensification by flux advection, radiative cooling, and evacuation by strong downflow found in MHD simulations. The quantitative agreement of synthetic and real observations indicates the validity of both the simulations and the interpretations of the spectro-polarimetric observations.
Key words: Sun: photosphere / Sun: granulation / magnetic fields
© ESO, 2010
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