Rosseland Center for Solar Physics
Natural Sciences (Astrophysics and Astrononmy)
The chromosphere is the interface between the photosphere and the
corona. In the chromosphere the dynamics change from gas-pressure driving
to magnetic-force driving, radiation transport changes from optically thick to
optically thin, the gas state changes from neutral to ionized, and from local
thermodynamic equilibrium to non-equilibrium conditions. The magnetic
field is the key quantity in the physics of the chromosphere. Understanding
its physics thus requires determination of the magnetic field at all locations
of the chromosphere.
The chromosphere is relatively dificult to study compared to the photosphere:
evolution timescales are shorter, chromospheric lines are broad
and deep, and thus have a relatively small photon flux, magnetic
flux densities and polarization signals are weaker and fundamental spatial scales are
expected to be very small.
In this talk I will introduce the science that SG3 has planned for EST,
some selected examples of observing plans and the requirements that we
think EST should deliver in order to be able to carry out the mentioned
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