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 …

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This work presents revised detailed reaction mechanism for small hydrocarbons combustion
with possibly full implementation of available kinetic data related to the prompt NO route via …

Context. Numerical simulations of stellar convection and photospheres have been
developed to the point where detailed shapes of observed spectral lines can be explained …

High-resolution images of the solar surface show a granulation pattern of hot rising and
cooler downward-sinking material–the top of the deep-reaching solar convection zone …

Heating the outer layers of the magnetically quiet solar atmosphere to more than one million
kelvin and accelerating the solar wind requires an energy flux of approximately 100 to 300 …

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 …

As the interface between the Sun's photosphere and corona, the chromosphere and
transition region play a key role in the formation and acceleration of the solar wind …

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 …

Magnetic waves are a relevant component in the dynamics of the solar atmosphere. Their
significance has increased because of their potential as a remote diagnostic tool and their …