Bibcode
Cheung, M. C. M.; Schüssler, M.; Moreno-Insertis, F.
Referencia bibliográfica
14th Cambridge Workshop on Cool Stars, Stellar Systems, and the Sun ASP Conference Series, Vol. 384, proceedings of the conference held 5-10 November, 2006, at the Spitzer Science Center and Michelson Science Center, Pasadena, California, USA. Edited by Gerard van Belle., p.181
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4
2008
Número de citas
0
Número de citas referidas
0
Descripción
The most prominent magnetic structures on the surface of the Sun are
bipolar active regions. These magnetic complexes are comprised of a
hierarchy of magnetic structures of different sizes, the largest of
which are sunspots. Observations indicate that the appearance of active
regions on the solar surface result from the emergence of bundles of
magnetic flux from the underlying convection zone. We study the
emergence process by means of 3D radiation MHD simulations. In the
simulations, an initially buoyant magnetic flux tube is introduced into
the near-surface layers of the convection zone. Subject to the buoyancy
force, the flux tube rises towards the photosphere. Our simulations
highlight the importance of magneto-convection on the evolution of the
magnetic flux tube. The external convective flow field has an important
influence on the emergence morphology of the emerging magnetic field.
Depending on the initial properties of the magnetic flux tube (e.g.
field strength, twist, entropy etc.), flux emergence may lead to a
disturbance of the local granulation pattern. The observational
signatures associated with emerging magnetic flux in our simulations are
in qualitative and quantitative agreement with observational studies of
emerging flux regions on the Sun.