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.
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Notes
The power-law index \(\gamma_{\mathrm{thin}}\) of a thin-target photon spectrum is related to the power-law index \(\delta\) of electron flux distribution and the power-law index \(\delta'\) of electron density distribution by \(\gamma_{\mathrm{thin}} = \delta+1\) and \(\gamma_{\mathrm{thin}} = \delta' + 0.5\), respectively (e.g., Brown, 1971; Tandberg-Hanssen and Emslie, 1988).
Here, the power-law index \(\gamma_{\mathrm{thick}}\) of a uniform thick-target photon spectrum is related to the power-law index \(\delta\) of the electron flux distribution and the power-law index \(\delta'\) of electron density distribution by \(\gamma_{\mathrm{thick}} = \delta- 1\) and \(\gamma_{\mathrm{thick}} = \delta' - 1.5\), respectively (e.g., Holman et al., 2011).
Because the phase space density of the \(\kappa\)-distribution has the form \(f(v)\propto v^{-2(\kappa+1)}\), the corresponding power indices of the electron flux distributions are \(\delta\) \({\sim}\,4\) and \({\sim}\,14\) (or \({\sim}\,4.5\) and \({\sim}\,14.5\) for the density distribution).
Reduced level-2 spectra containing absolute fluxes for 101 flares and active region plasma is accessible at www.cbk.pan.wroc.pl/experiments/resik/RESIK_Level2/index.html .
References
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Acknowledgements
The authors thank the anonymous referee for numerous improvements to the manuscript. The authors also acknowledge useful discussions with M. Battaglia, P. Heinzel and A. Zemanová. J.D. and E.Dz. authors acknowledge support by Grant Agency of the Czech Republic, Grant No. 17-16447S, and institutional support RVO:67985815 from the Czech Academy of Sciences. G.D.Z. and H.E.M. acknowledge funding from STFC. J.D., G.D.Z., and H.E.M. acknowledge funding from Royal Society via the Newton Alumni programme. P.R.Y. acknowledges support from NASA grant NNX15AF25G. A.G. acknowledges the in-house research support provided by the STFC. B.S. and J.S. acknowledge support from the Polish National Science Centre grant 2013/11/B/ST9/00234. M.O. was supported by NASA grant NNX08AO83G at UC Berkeley. L.M. was supported by the UK Science and Technology Facilities Council grant ST/K001051/1. The authors benefited greatly from participation in the International Team 276 funded by the International Space Science Institute (ISSI) in Bern, Switzerland. CHIANTI is a collaborative project involving the University of Cambridge (UK), the George Mason University (USA), and the University of Michigan (USA). ADAS is a project managed at the University of Strathclyde (UK) and funded through memberships universities and astrophysics and fusion laboratories in Europe and worldwide.
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Dudík, J., Dzifčáková, E., Meyer-Vernet, N. et al. Nonequilibrium Processes in the Solar Corona, Transition Region, Flares, and Solar Wind (Invited Review) . Sol Phys 292, 100 (2017). https://doi.org/10.1007/s11207-017-1125-0
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DOI: https://doi.org/10.1007/s11207-017-1125-0