Data-driven model of the solar corona above an active region. (arXiv:1903.00455v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Warnecke_J/0/1/0/all/0/1">Jörn Warnecke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peter_H/0/1/0/all/0/1">Hardi Peter</a> (Max-Planck-Institut für Sonnensystemforschung)
In this study we aim to reproduce the structure of the corona above a solar
active region as seen in the extreme ultraviolet (EUV) using a
three-dimensional magnetohydrodynamic (3D MHD) model. The 3D MHD data-driven
model solves the induction equation and the mass, momentum and energy balance.
To drive the system, we feed the observed evolution of the magnetic field in
the photosphere of the active region AR 12139 into the bottom boundary. This
creates a hot corona above the cool photosphere in a self-consistent way. We
synthesize the coronal EUV emission from the densities and temperatures in the
model and compare this to the actual coronal observations. We are able to
reproduce the overall appearance and key features of the corona in this active
region. The model shows long loops, fan loops, compact loops and diffuse
emission forming at the same locations at similar times as in the observation.
Furthermore, the low intensity contrast of the model loops in EUV matches the
observations. In our model the energy input into the corona is similar as in
the scenarios of fieldline-braiding or fluxtube tectonics, i.e. through the
driving of the vertical magnetic field by horizontal photospheric motions. The
success of our model shows the central role this process plays for the
structure, dynamics and heating of the corona.
In this study we aim to reproduce the structure of the corona above a solar
active region as seen in the extreme ultraviolet (EUV) using a
three-dimensional magnetohydrodynamic (3D MHD) model. The 3D MHD data-driven
model solves the induction equation and the mass, momentum and energy balance.
To drive the system, we feed the observed evolution of the magnetic field in
the photosphere of the active region AR 12139 into the bottom boundary. This
creates a hot corona above the cool photosphere in a self-consistent way. We
synthesize the coronal EUV emission from the densities and temperatures in the
model and compare this to the actual coronal observations. We are able to
reproduce the overall appearance and key features of the corona in this active
region. The model shows long loops, fan loops, compact loops and diffuse
emission forming at the same locations at similar times as in the observation.
Furthermore, the low intensity contrast of the model loops in EUV matches the
observations. In our model the energy input into the corona is similar as in
the scenarios of fieldline-braiding or fluxtube tectonics, i.e. through the
driving of the vertical magnetic field by horizontal photospheric motions. The
success of our model shows the central role this process plays for the
structure, dynamics and heating of the corona.
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