High-resolution coverage of the Sun both from space and ground-based telescopes is leading to a plethora of observations of small-scale dynamic structures observed from the chromosphere to the transition region and corona. Nowadays, there is a general consensus that the key to understanding how the solar plasma is accelerated and heated may well be found in the studies of these fine structures. Among them spicules seem to be the most prominent ones characterizing the chromospheric network. While these chromosperic structures are observed and studied for several decades in the visible, near UV and recently also in EUV emission lines and continua, there are still many questions to be answered. The dynamics of spicules and other fine structures may well have broad implications for the mass and energy balance of the outer atmosphere of the Sun and the solar wind.
In this work we will perform:
a) the study of short term dynamics of spicules,
b) the determination of their physical parameters (morphology, temperat ure density, velocity etc) and their temporal evolution,
c) the contribution of fine structures to the mass and energy budget of the solar chromosphere and corona.
The work will be based on:
a) the data analysis of existing observations, as well as new coordinated multi-wavelength observations of spicules and other small-scale structures and their longitudinal photospheric magnetic field with SOHO, TRACE and ground-based telescopes (THEMIS and DOT),
b) interpretation of the results and
c) theoretical work to describe the physical processes in a rather quantitative manner.
This theoretical work will include non-LTE radiative transfer calculations of the Halpha line profile and evaluation of the proposed heating mechanisms.
Call for proposal
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