TY  - JOUR
A1  - Kostogryz, Nadiia M.
A1  - Kupka, Friedrich
A1  - Piskunov, Nikolai
A1  - Fabbian, Damian
A1  - Krüger, Daniel
A1  - Gizon, Laurent
T1  - Accurate Short-Characteristics Radiative Transfer in A Numerical Tool for Astrophysical Research (ANTARES)
JF  - Solar Physics
KW  - Astrophysics
Y1  - 
ER  - 
TY  - JOUR
A1  - Shan, Yutong
A1  - Reiners, Ansgar
A1  - Fabbian, Damian
A1  - Marfil, Emilio
A1  - Montes, David
A1  - Tabernero, Hugo M.
A1  - Ribas, Ignasi
A1  - Caballero, Jose A.
A1  - Quirrenbach, Andreas
A1  - Amado, Pedro J.
A1  - Aceituno, Jesus
A1  - Bejar, Victor J. S.
A1  - Cortes-Contreras, Miriam
A1  - Dreizler, Stefan
A1  - Hatzes, Artie P.
A1  - Henning, Thomas
A1  - Jeffers, Sandra V.
A1  - Kaminski, Adrian
A1  - Kurster, Martin
A1  - Lafarga, Marina
A1  - Morales, Juan Carlos
A1  - Nagel, Evangelos
A1  - Palle, Enric
A1  - Passegger, Vera M.
A1  - Lopez, Cristina Rodriguez
A1  - Schweitzer, Andreas
A1  - Zechmeister, Mathias
T1  - The CARMENES search for exoplanets around M dwarfs Not-so-fine hyperfine-split vanadium lines in cool star spectra
JF  - Astronomy & Astrophysics
KW  - Atomic data
KW  - Low-mass stars
Y1  - 
VL  - 654
ER  - 
TY  - JOUR
A1  - Cubas Armas, Melania
A1  - Fabbian, Damian
T1  - Do MURaM and STAGGER Simulations of Solar Faculae Match Observational Signatures from Magnetic Structures?
JF  - The Astrophysical Journal
N2  - We compare results of simulations of solar facular-like conditions performed using the numerical codes MURaM and STAGGER. Both simulation sets have a similar setup, including the initial condition of ≈200 G vertical magnetic flux. After interpolating the output physical quantities to constant optical depth, we compare them and test them against inversion results from solar observations. From the snapshots, we compute the monochromatic continuum in the visible and infrared, and the full Stokes vector of the Fe i spectral line pair around 6301–6302 Å. We compare the predicted spectral lines (at the simulation resolution and after smearing to the HINODE SP/SOT resolution) in terms of their main parameters for the Stokes I line profiles, and of their area and amplitude asymmetry for the Stokes V profiles. The codes produce magnetoconvection with similar appearance and distribution in temperature and velocity. The results also closely match the values from recent relevant solar observations. Although the overall distribution of the magnetic field is similar in both radiation-magnetohydrodynamic (RMHD) simulation sets, a detailed analysis reveals substantial disagreement in the field orientation, which we attribute to the differing boundary conditions. The resulting differences in the synthetic spectra disappear after spatial smearing to the resolution of the observations. We conclude that the two sets of simulations provide robust models of solar faculae. Nevertheless, we also find differences that call for caution when using results from RMHD simulations to interpret solar observational data.
KW  - Magnetohydrodynamics
KW  - Magnetohydrodynamical simulations
KW  - Radiative transfer
KW  - Active sun
KW  - Solar magnetic fields
Y1  - 
VL  - 923
IS  - 2
ER  -