Magnetohydrostatic Sunspot Models from Deep Subphotospheric to Chromospheric Layers

Bibcode
2008ApJ...689.1379K
DOI
10.1086/592681
Khomenko, E.; Collados, M.
Bibliographical reference

The Astrophysical Journal, Volume 689, Issue 2, pp. 1379-1387.

Advertised on:
12
2008
Journal
The Astrophysical Journal
Number of authors
2
IAC number of authors
2
Citations
37
Refereed citations
33
Description
In order to understand the influence of magnetic fields on the propagation properties of waves, as derived from different local helioseismology techniques, forward modeling of waves is required. Such calculations need a model in magnetohydrostatic equilibrium as an initial atmosphere through which to propagate oscillations. We provide a method to construct such a model in equilibrium for a wide range of parameters, for use in simulations of artificial helioseismologic data. The method combines the advantages of self-similar solutions and current-distributed models. A set of models is developed by numerical integration of magnetohydrostatic equations from the subphotospheric to chromospheric layers.
Related projects
Project Image
Solar and Stellar Magnetism

Magnetic fields are at the base of star formation and stellar structure and evolution. When stars are born, magnetic fields brake the rotation during the collapse of the mollecular cloud. In the end of the life of a star, magnetic fields can play a key role in the form of the strong winds that lead to the last stages of stellar evolution. During

Tobías
Felipe García
In progress
Type
Refereed
Magnetic fields
Sunspots
Solar Physics (FS)

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