18 citations · 63 across the 10 of their papers we have counts for
11 papers
1.5D investigation of the Hanle effect in the Ca I 4227 line using partial frequency redistribution. Comparison of synthetic Stokes profiles in Bifrost and MURaM-ChE rMHD models
Devang Agnihotri, L. S. Anusha, D. Przybylski +2
Modeling scattering polarization in the Ca I 4227 Å line is important for diagnosing chromospheric magnetic fields. We investigate the relative influence of formation heights and m…
A single frequency approach to nonequilibrium modeling of the chromosphere
W. Ruan, D. Przybylski, R. Cameron +1
The solar chromosphere is a region where radiation plays a critical role in energy transfer and interacts strongly with the plasma. In this layer, strong spectral lines, such as th…
Ca ii 854.2 nm in an enhanced network region simulated with MURaM-ChE
P. A. Ondratschek, D. Przybylski, H. N. Smitha +2
The Ca ii 854.2 nm line is widely used to study the chromosphere of the Sun. In the quiet Sun, the spatially averaged line profile shows a red asymmetry and a redshift of the line…
Stellar-wind Fueled Accretion onto Sagittarius A* in the Presence of a Nuclear Star Cluster
Edward Skrabacz, Lena Murchikova, Sean M. Ressler +2
The Milky Way's Galactic Center hosts the black hole Sagittarius A* (Sgr A*), which provides us with a close-up view into supermassive black hole accretion and feedback. Recent wor…
Formation of chromospheric Fe I lines in the near ultraviolet in 1D atmospheres
E. Harnes, H. N. Smitha, A. Korpi-Lagg +2
In the near ultraviolet (NUV) part of the solar spectrum, there are several Fe I lines with very broad profiles, typical of chromospheric lines. These lines are largely unexplored…
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…
Three-dimensional non-LTE radiative transfer effects in Fe I lines IV. Line formation at high spatial resolution
R. Holzreuter, H. N. Smitha, S. K. Solanki
In the first three papers of this series, we investigated the formation of photospheric neutral iron lines in different atmospheres ranging from idealised flux tube models to compl…
A magnetic avalanche as the central engine powering a solar flare
L. P. Chitta, D. I. Pontin, E. R. Priest +17
Solar flares are the most powerful, magnetically driven, explosions in the heliosphere. The nature of magnetic energy release in the solar corona that heats the plasma and accelera…
Coronal hole picoflare jets are progenitors of both fast and Alfvénic slow solar wind
L. P. Chitta, Z. Huang, R. D'Amicis +19
Solar wind, classified by its bulk speed and the Alfvénic nature of its fluctuations, generates the heliosphere. The elusive physical processes responsible for the generation of th…
Mg ii h&k spectra of an enhanced network region simulated with the MURaM-ChE code. Results using 1.5D synthesis
P. Ondratschek, D. Przybylski, H. N. Smitha +3
The Mg ii h&k lines are key diagnostics of the solar chromosphere. They are sensitive to the temperature, density, and non-thermal velocities in the chromosphere. The average Mg ii…
Non-thermal broadening of coronal lines in a 3D MHD loop model
C. A. Breu, H. Peter, S. K. Solanki +2
Observed spectral profiles of emission lines from the corona are found to have widths exceeding the thermal line width. To investigate the physical mechanism, we run a 3D MHD model…