Stokes diagnostics of simulated solar magneto-convection
Version 2 2024-06-05, 01:40Version 2 2024-06-05, 01:40
Version 1 2018-11-02, 15:27Version 1 2018-11-02, 15:27
journal contribution
posted on 2024-06-05, 01:40 authored by Sergiy ShelyagSergiy Shelyag, M Schüssler, SK Solanki, A VöglerWe present results of synthetic spectro-polarimetric diagnostics of radiative MHD simulations of solar surface convection with magnetic fields. Stokes profiles of Zeeman-sensitive lines of neutral iron in the visible and infrared spectral ranges emerging from the simulated atmosphere have been calculated in order to study their relation to the relevant physical quantities and compare with observational results. We have analyzed the dependence of the Stokes-I line strength and width as well as of the Stokes-V signal and asymmetries on the magnetic field strength. Furthermore, we have evaluated the correspondence between the actual velocities in the simulation with values determined from the Stokes-I (Doppler shift of the centre of gravity) and Stokes-V profiles (zero-crossing shift). We confirm that the line weakening in strong magnetic fields results from a higher temperature (at equal optical depth) in the magnetic flux concentrations. We also confirm that considerable Stokes-V asymmetries originate in the peripheral parts of strong magnetic flux concentrations, where the line of sight cuts through the magnetopause of the expanding flux concentration into the surrounding convective donwflow. © ESO 2007.
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Journal
Astronomy and AstrophysicsVolume
469Pagination
731-747Location
London, Eng.Publisher DOI
Open access
- Yes
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0004-6361eISSN
1432-0746Publication classification
CN.1 Other journal articleIssue
2Publisher
EDP SciencesUsage metrics
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