Observations and simulations of the Na I D1 line profiles in an M-class solar flare

Abstract

We study the temporal evolution of the Na I D1 line profiles in the M3.9 flare SOL2014-06-11T21:03 UT, using high spectral resolution observations obtained with the IBIS instrument on the Dunn Solar Telescope combined with radiative hydrodynamic simulations. Our results show a significant increase in line core and wing intensities during the flare. The analysis of the line profiles from the flare ribbons reveal that the Na I D1 line has a central reversal with excess emission in the blue wing (blue asymmetry). We combine RADYN and RH simulations to synthesise Na I D1 line profiles of the flaring atmosphere and find good agreement with the observations. Heating with a beam of electrons modifies the radiation field in the flaring atmosphere and excites electrons from the ground state $3s{}^2\mathrm{S}$ to the first excited state $3p{}^2\mathrm{P}$, which in turn modifies relative population of the two states. The change in temperature and the population density of the energy states make the sodium line profile revert from absorption into emission. Analysis of the simulated spectra also reveals that the Na I D1 flare profile asymmetries are produced by the velocity gradients generated %and opacity effects in the lower solar atmosphere.

7 pages, 8 figures, accepted in ApJ

References in corpus (4)

• The solar chromosphere at high resolution with IBIS. I. New insights from the Ca II 854.2 nm line
• Fine structure of flare ribbons and evolution of electric currents
• Diagnostics of the Heating Processes in Solar Flares Using Chromospheric Spectral Lines
• The Influence of Solar Flares on the Lower Solar Atmosphere: Evidence from the Na D Absorption Line Measured by GOLF/SOHO

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