125 citations · 497 across the 20 of their papers we have counts for
20 papers
Modeling Solar Atmosphere Dynamics with MAGEC
Anamaría Navarro, E. Khomenko, N. Vitas +1
Modeling the solar atmosphere is challenging due to its layered structure and multi-scale dynamics. We aim to validate the new radiative MHD code MAGEC, which combines the MANCHA a…
The effect of local magnetic fields in quiet regions of stellar atmospheres simulated with MANCHA
Andrea Perdomo García, Nikola Vitas, Elena Khomenko +1
Our aim is to characterize the effects of the local magnetic fields in quiet regions of stellar atmospheres. We compute magneto-hydrodynamic and purely hydrodynamic simulations of…
Convergence study of ambipolar diffusion in realistic simulations of magneto-convection
E. Khomenko, N. Vitas, M. Collados +1
The aim of this paper is to improve our understanding of the heating mechanisms of the solar chromosphere via realistic three-dimensional (3D) modeling of solar magneto-convection,…
Hydrodynamic simulations of cool stellar atmospheres with \texttt{MANCHA}
Andrea Perdomo García, Nikola Vitas, Elena Khomenko +1
Aims. Our aim is to test how different binning strategies previously studied in one-dimensional models perform in three-dimensional radiative hydrodynamic simulations of stellar at…
The influence of thermal pressure gradients and ionization (im)balance on the ambipolar diffusion and charge-neutral drifts
M. M. Gómez-Míguez, D. Martínez-Gómez, E. Khomenko +1
Solar partially ionized plasma is frequently modeled using single-fluid (1F) or two-fluid (2F) approaches. In the 1F case, charge-neutral interactions are often described through a…
Mancha3D code: Multi-purpose Advanced Non-ideal MHD Code for High resolution simulations in Astrophysics
M. Modestov, E. Khomenko, N. Vitas +14
The Mancha3D code is a versatile tool for numerical simulations of magnetohydrodynamic processes in solar/stellar atmospheres. The code includes non-ideal physics derived from plas…
Opacity for realistic 3D MHD simulations of cool stellar atmospheres
A. Perdomo García, N. Vitas, E. Khomenko +4
Context. Realistic 3D time-dependent simulations of stellar near-surface convection employ the opacity binning method for efficient and accurate computation of the radiative energy…
A study of the capabilities for inferring atmospheric information from high-spatial-resolution simulations
C. Quintero Noda, E. Khomenko, M. Collados +8
In this work, we study the accuracy that can be achieved when inferring the atmospheric information from realistic numerical magneto-hydrodynamic simulations that reproduce the spa…
Modeling the thermal conduction in the solar atmosphere with the code MANCHA3D
Anamaría Navarro, E. Khomenko, M. Modestov +1
Thermal conductivity is one of the important mechanisms of heat transfer in the solar corona. In the limit of strongly magnetized plasma, it is typically modeled by Spitzer's expre…
Newly formed downflow lanes in exploding granules in the solar photosphere
M. Ellwarth, C. E. Fischer, N. Vitas +2
Exploding granules have drawn renewed interest because of their interaction with the magnetic field. Especially the newly forming downflow lanes developing in their centre seem to…
Joint action of Hall and ambipolar effects in 3D magneto-convection simulations of the quiet Sun. I. Dissipation and generation of waves
P. A. Gonzalez-Morales, E. Khomenko, N. Vitas +1
The partial ionization of the solar plasma causes several nonideal effects such as the ambipolar diffusion, the Hall effect, and the Biermann battery effect. Here we report on the…
Three-dimensional simulations of solar magneto-convection including effects of partial ionization
E. Khomenko, N. Vitas, M. Collados +1
Over the last decades, realistic 3D radiative-MHD simulations have become the dominant theoretical tool for understanding the complex interactions between the plasma and the magnet…
Numerical simulations of quiet Sun magnetic fields seeded by Biermann battery
E. Khomenko, N. Vitas, M. Collados +1
The magnetic fields of the quiet Sun cover at any time more than 90\% of its surface and their magnetic energy budget is crucial to explain the thermal structure of the solar atmos…
First detection of sign-reversed linear polarization from the forbidden [O I] 630.03 nm line
A. G. de Wijn, H. Socas-Navarro, N. Vitas
We report on the detection of linear polarization of the forbidden [O i] 630.03 nm spectral line. The observations were carried out in the broader context of the determination of t…
How different are the Liège and Hamburg atlases of the solar spectrum?
H. -P. Doerr, N. Vitas, D. Fabbian
Context: The high-fidelity solar spectral atlas prepared by Delbouille and co-workers (Liège atlas), and the one by Neckel and co-workers (Hamburg atlas), are widely recognised as…
Fluid description of multi-component solar partially ionized plasma
Elena Khomenko, Manuel Collados, Antonio Diaz +1
We derive self-consistent formalism for the description of multi-component partially ionized solar plasma, by means of the coupled equations for the charged and neutral components…
Ellerman bombs: fallacies, fads, usage
Robert J. Rutten, Gregal J. M. Vissers, Luc H. M. Rouppe van der Voort +2
Ellerman bombs are short-lived brightenings of the outer wings of Halpha that occur in active regions with much flux emergence. We point out fads and fallacies in the extensive Ell…
Line shape effects on intensity measurements of solar features: Brightness correction to SoHO MDI continuum images
S. Criscuoli, I. Ermolli, D. Del Moro +4
Continuum intensity observations obtained with the Michelson Doppler Imager (MDI) on-board the SoHO mission provide long time series of filtergrams that are ideal for studying the…
Explanation of the activity sensitivity of Mn I 5394.7 Å
N. Vitas, B. Viticchiè, R. J. Rutten +1
There is a long-standing controversy concerning the reason why the Mn I 5394.7 A line in the solar irradiance spectrum brightens more at larger activity than most other photospheri…
On the solar abundance of indium
N. Vitas, I. Vince, M. Lugaro +3
The generally adopted value for the solar abundance of indium is over six times higher than the meteoritic value. We address this discrepancy through numerical synthesis of the 451…