Context. A significant part of the penumbral magnetic field returns below the surface in the very deep photosphere. For lines in the visible, a large portion of this return field can only be detected indirectly by studying its imprints on strongly asymmetric and three-lobed Stokes V profiles. Infrared lines probe a narrow layer in the very deep
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Magnetic fields of opposite polarity in sunspot penumbraeFranz, M. et al.112016
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Magnetic Flux Emergence and its Interaction with AN Existing Coronal Field
Not Available
Galsgaard, K. et al.Advertised on:
112005 -
Magnetic Flux Emergence and its Interaction with AN Existing Coronal Field
Not Available
Galsgaard, K. et al.Advertised on:
112005 -
Magnetic flux emergence into the solar photosphere and chromosphere
Aims: We model the emergence of magnetized plasma across granular convection cells and the low atmosphere, including layers up to the mid-chromosphere. Methods: Three-dimensional numerical experiments are carried out in which the equations of MHD and radiative transfer are solved self-consistently. We use the MURaM code, which assumes local
Tortosa-Andreu, A. et al.Advertised on:
112009 -
Magnetic Loops in the Quiet Sun
We investigate the fine structure of magnetic fields in the atmosphere of the quiet Sun. We use photospheric magnetic field measurements from SUNRISE/IMaX with unprecedented spatial resolution to extrapolate the photospheric magnetic field into higher layers of the solar atmosphere with the help of potential and force-free extrapolation techniques
Wiegelmann, T. et al.Advertised on:
112010 -
Magneto-acoustic wave energy in sunspots: observations and numerical simulations
We have reproduced some sunspot wave signatures obtained from spectropolarimetric observations through 3D MHD numericalsimulations. The results of the simulations arecompared with the oscillations observed simultaneously at different heights from the SiI lambda10827Å line, HeI lambda10830Å line, the CaII H core and the FeI blends at the wings of
Felipe, T. et al.Advertised on:
112011