Speaker
Nikola Vitas
(Instituto de Astrofísica de Canarias)
Description
The three-dimensional simulation of magnetoconvection in a
sunspot umbra by V\"ogler and Sch\"ussler (2006) was an
important step towards more realistic sunspot and
active-region simulations. In spite of the idealized
boundary conditions in this simulation (it describes a
periodic umbra-like atmosphere isolated from the surrounding
quiet sun) it predicted the typical coffee-bean shape of
umbral-dots that was later on confirmed by high-resolution
observations. Here we use snapshots from a similar
simulation run to synthetize the monochromatic continuum
intensity (0.4 to 1.6 \mu m) and the Fe I 6302 \AA lines.
The continuum and its center-to-limb variation are compared
to observations available in the literature. The Fe lines
are spatially and spectrally degraded to replicate realistic
observations with Hinode SP/SOT. Several inversion
techniques are applied to this quasi-Hinode data to retrieve
magnetic field, temperature and velocity as if it were a
real observation. These results are then compared to the
original values in the snapshot and the sensitivity of
different methods is estimated.
