| Affiliation: | 1.Astronomical Institute,Czech Academy of Sciences,Ond?ejov,Czech Republic;2.CNRS, PSL, LESIA,Observatoire de Paris,Meudon,France;3.DAMTP,University of Cambridge,Cambridge,UK;4.College of Science,George Mason University,Fairfax,USA;5.NASA Goddard Space Flight Center,Greenbelt,USA;6.Northumbria University,Newcastle Upon Tyne,UK;7.STFC Rutherford Appleton Laboratory,Chilton, Didcot,UK;8.Space Research Centre (CBK PAN),Warsaw,Poland;9.Space Sciences Laboratory,University of California,Berkeley,USA;10.Leibniz-Institut für Astrophysik,Potsdam,Germany;11.Imperial College London,London,UK;12.University of Applied Sciences and Arts Northwestern Switzerland,Windisch,Switzerland;13.ESAC,European Space Agency,Madrid,Spain;14.Institute of Experimental Physics,SAS,Ko?ice,Slovak Republic |
| Abstract: | We review the presence and signatures of the non-equilibrium processes, both non-Maxwellian distributions and non-equilibrium ionization, in the solar transition region, corona, solar wind, and flares. Basic properties of the non-Maxwellian distributions are described together with their influence on the heat flux as well as on the rates of individual collisional processes and the resulting optically thin synthetic spectra. Constraints on the presence of high-energy electrons from observations are reviewed, including positive detection of non-Maxwellian distributions in the solar corona, transition region, flares, and wind. Occurrence of non-equilibrium ionization is reviewed as well, especially in connection to hydrodynamic and generalized collisional-radiative modeling. Predicted spectroscopic signatures of non-equilibrium ionization depending on the assumed plasma conditions are summarized. Finally, we discuss the future remote-sensing instrumentation that can be used for the detection of these non-equilibrium phenomena in various spectral ranges. |
