Properties of shock waves in the quiet-Sun chromosphere

Abstract

Context. Short-lived (100 s or less), sub-arcsec to a couple of arcsec sized features of enhanced brightenings in the narrowband images at the H2V and K2V positions of the Ca II H&K lines in the quiet Sun are known as bright grains. These bright grains are interpreted as manifestations of acoustic shock waves in the chromosphere. Aims. We aim to study time-varying stratified atmospheric properties, such as the temperature, line-of-sight (LOS) velocity, and microturbulence inferred from observations of the bright grains during such acoustic shock events. Methods. With simultaneous observations of a quiet-Sun internetwork region in the Fe I 6173 Å, Ca II 8542 Å, and Ca II K lines acquired by the CRisp Imaging Spectro-Polarimeter and the CHROMospheric Imaging Spectrometer instruments on the Swedish 1-m Solar Telescope, we performed multi-line non-local thermodynamic equilibrium inversions using the STockholm inversion Code to infer the time-varying stratified atmosphere’s physical properties. Results. The Ca II K profiles of bright grains show enhancement in the K2V peak intensities with the absence of the K2R features. At the time of maximum enhancement in the K2V peak intensities, we found average enhancements in temperature at lower chromospheric layers (at log τ500 ≃ −4.2) of about 1.1 kK, with a maximum enhancement of ∼4.5 kK. These temperature enhancements are co-located with upflows, as strong as −6 km s−1, in the direction of the LOS. The LOS velocities at upper chromospheric layers at log τ500 < −4.2 show consistent downflows greater than +8 km s−1. The retrieved value of microturbulence in the atmosphere of bright grains is negligible at chromospheric layers. Conclusions. This study provides observational evidence to support the interpretation that the bright grains observed in narrowband images at the H2V and K2V positions of the Ca II H&K lines are manifestations of upward propagating acoustic shocks against a background of downflowing atmospheres.

On the Magnetic Nature of Quiet-Sun Chromospheric Grains

“…They are now known as Ca II K grains and are associated with sudden narrowband emission features at the blue side of the line core. Similar features are found in the Ca II IR lines, in phase with those of the Ca II K line (Cram et al 1977;Martínez-Sykora et al 2015;Mathur et al 2022).…”

Decay of a photospheric transient filament at the boundary of a pore and the chromospheric response

“…We note that the enhancement and the following depression in the temperature stratification of Pixel P1 (see Fig. 8) could, in principle, also be caused by an acoustic shock similar to the model introduced by Carlsson & Stein (1997) and recently observed by Mathur et al (2022). However, we limit the discussion to magnetic reconnection as the driver of the observed temperature and velocity signals because these two observed signatures occur co-spatial and co-temporal to the decay of the magnetic transient filament; also we do not identify a mechanism related to the shock front that would also explain the observed flow field.…”

Decay of a photospheric transient filament at the boundary of a pore and the chromospheric response

“…We note that the enhancement and the following depression in the temperature stratification of Pixel P1 (see Fig. 8) could, in principle, also be caused by an acoustic shock similar to the model introduced by Carlsson & Stein (1997) and recently observed by Mathur et al (2022). However, we limit the discussion to magnetic reconnection as the driver of the observed temperature and velocity signals because these two observed signatures occur co-spatial and co-temporal to the decay of the magnetic transient filament and we also do not identify a mechanism how the shock front would also explain the observed flow field.…”