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Solar carbon abundance from 3D non-LTE modelling of the diagnostic lines of the CH molecule
Richard Hoppe, Maria Bergemann, Philipp Eitner +5
The spectral lines of the CH molecule are a key carbon (C) abundance diagnostic in FGKM-type stars. These lines are detectable in metal-rich and, in contrast to atomic C lines, als…
Structure and dynamics of the internetwork solar chromosphere: results of a small-scale dynamo simulation
D. Przybylski, R. Cameron, S. K. Solanki +3
The heating and structure of the solar chromosphere depends on the underlying magnetic field, among other parameters. The lowest magnetic flux of the solar atmosphere is found in t…
High flow speeds and transition-region like temperatures in the solar chromosphere during flux emergence
J. Leenaarts, M. van Noort, J. de la Cruz Rodríguez +7
Context: Flux emergence in the solar atmosphere is a complex process that causes a release of magnetic energy as heat and acceleration of solar plasma at a variety of spatial scale…