Multi-Scale Variability of Coronal Loops Set by Thermal Non-Equilibrium and Instability as a Probe for Coronal Heating

  title={Multi-Scale Variability of Coronal Loops Set by Thermal Non-Equilibrium and Instability as a Probe for Coronal Heating},
  author={Patrick Antolin and Clara Froment},
  booktitle={Frontiers in Astronomy and Space Sciences},
Solar coronal loops are the building blocks of the solar corona. These dynamic structures are shaped by the magnetic field that expands into the solar atmosphere. They can be observed in X-ray and extreme ultraviolet (EUV), revealing the high plasma temperature of the corona. However, the dissipation of magnetic energy to heat the plasma to millions of degrees and, more generally, the mechanisms setting the mass and energy circulation in the solar atmosphere are still a matter of debate… 
Prevalence of Thermal Nonequilibrium over an Active Region
Recent observations have shown that besides the characteristic multimillion degree component, the corona also contains a large amount of cool material called coronal rain, whose clumps are 10–100


Thermal instability and non-equilibrium in solar coronal loops: from coronal rain to long-period intensity pulsations
  • P. Antolin
  • Physics
    Plasma Physics and Controlled Fusion
  • 2019
The complex interaction of the magnetic field with matter is the key to some of the most puzzling observed phenomena at multiple scales across the Universe, from tokamak plasma confinement
Dynamics of solar coronal loops
Observations in X-ray and EUV of the solar corona reveal the existence of very complex and dynamic structures made of plasma magnetically confined in loops. These structures can be studied by means
Multi-scale observations of thermal non-equilibrium cycles in coronal loops
Context. Thermal non-equilibrium (TNE) is a phenomenon that can occur in solar coronal loops when the heating is quasi-constant and highly-stratified. Under such heating conditions, coronal loops
Constant cross section of loops in the solar corona
Context. The corona of the Sun is dominated by emission from loop-like structures. When observed in X-ray or extreme ultraviolet emission, these million K hot coronal loops show a more or less
Quasi-constant heating at the footpoints of loops leads to evaporation and condensation cycles of the plasma: thermal non-equilibrium (TNE). This phenomenon is believed to play a role in the
Coronal Heating by MHD Waves
The heating of the solar chromosphere and corona to the observed high temperatures, imply the presence of ongoing heating that balances the strong radiative and thermal conduction losses expected in
Seismological constraints on the solar coronal heating function
Aims. The hot solar corona exists because of the balance between radiative and conductive cooling and some counteracting heating mechanism that remains one of the major puzzles in solar physics.
The location and frequency of events that heat the million-degree corona are still a matter of debate. One potential heating scenario is that the energy release is effectively steady and highly
Magnetohydrodynamic Spectroscopy of a Non-adiabatic Solar Atmosphere
The quantification of all possible waves and instabilities in a given system is of paramount importance, and knowledge of the full magnetohydrodynamic (MHD) spectrum allows one to predict the
A Fast and Accurate Method to Capture the Solar Corona/Transition Region Enthalpy Exchange
The brightness of the emission from coronal loops in the solar atmosphere is strongly dependent on the temperature and density of the confined plasma. After a release of energy, these loops undergo a