Waves and oscillations have been observed in the Sun's atmosphere for over half a century.
While such phenomena have readily been observed across the entire electromagnetic …

The application of machine learning in solar physics has the potential to greatly enhance our
understanding of the complex processes that take place in the atmosphere of the Sun. By …

We present a series of models for the plasma properties along open magnetic flux tubes
rooted in solar coronal holes, streamers, and active regions. These models represent the …

We have simulated the generation of Ca II H 2V bright grains by acoustic shocks. We employ
a one-dimensional, non-LTE radiation-hydrodynamic code, with six-level model atoms for …

We present a unified computational framework that can be used to describe impulsive flares
on the Sun and on dMe stars. The models assume that the flare impulsive phase is caused …

ABSTRACT A multilevel accelerated lambda iteration (MALI) method for radiative transfer
calculations with partial frequency redistribution (PRD) is presented. The method, which is …

We present the results of optically thick non-LTE radiative transfer calculations of lines and
continua of H, C I-IV, and O I-VI and other elements using a new one-dimensional, time …

Enhanced chromospheric emission which corresponds to an outwardly increasing
semiempirical temperature structure can be produced by wave motion without any increase …

An overview is given of the observational and the theoretical methods used to investigate
solar magnetic fields. It includes an introduction to the Stokes parameters, their radiative …

The chromosphere is a thin layer of the solar atmosphere that bridges the relatively cool
photosphere and the intensely heated transition region and corona. Compressible and …