Understanding the solar chromosphere through 3D MHD modeling and 3D non-LTE radiative transfer
by
Jorrit Leenaarts(Stockholm University)
→
Europe/Stockholm
FA31
FA31
Description
The solar chromosphere is the interface between the convective interior of
the Sun and the magnetic corona. The chromosphere guides and regulates the
mass, energy and magnetic flux flow to the corona and is the source of the
bulk of the UV radiation impinging on Earth. It also serves as a close-up
example of stellar chromospheres.
I will discuss 3D time-dependent MHD models of the solar chromosphere
performed with the Bifrost stellar atmosphere code developed at the
University of Oslo. In addition I will discuss recent progress in
understanding the formation of spectral lines in the chromosphere. In
particular I will show how 3D radiation effects cause the appearance of the
chromosphere as seen in the H-alpha line. If time permits I'll discuss
early results from the IRIS satellite, a NASA SMEX observatory that was
launched on June 27, 2013.