Simulations of magneto-convection in the solar photosphere Equations, methods, and results of the MURaM code

By A. Vögler, S. Shelyag, M. Schüssler, F. Cattaneo, Thierry Emonet, T. Linde. 2005

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Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/867110054f53700b7764e5d93ec0d348f43bae51

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Citations in the corpus

SIMULATION OF THE FORMATION OF A SOLAR ACTIVE REGION (2010, methodology): “The radiative MHD simulation was carried out with the MURaM code (Vögler et al. 2005; Rempel et al. 2009b), which takes into account radiative energy transport in the energy equation (assuming local thermodynamic equilibrium) and a realistic equation of state.”
Magnetoconvection in a Sunspot Umbra (2006, methodology): “…of field-free plasma from the underlying convection 2Since our numerical scheme includes a spatio-temporarily varying thermal ‘hyperdiffusivity’ (Vögler et al. 2005), the value of ζ is not readily determined in the lower part of the computational box, where κ is no longer dominated by the…”
State of the Field: Extreme Precision Radial Velocities (2016, methodology): “Magneto-convection simulations were then used to simulate the temperature and velocity structure with one degree spatial resolution using the MURaM code (Vögler et al. 2005) and a radiative transfer code was used to produce composite spectra for 156 absorption lines at each of 40 rotation phases.”
Solar Surface Emerging Flux Regions: A Comparative Study of Radiative MHD Modeling and Hinode SOT Observations (2008, methodology): “In Cheung et al. (2007a), we presented a study of magnetic flux emergence in granular convection by means of numerical radiative MHD simulations with the MURaM code (Vögler et al. 2005).”
EXTENSION OF THE MURAM RADIATIVE MHD CODE FOR CORONAL SIMULATIONS (2016, methodology): “The radiative transfer module, originally developed by Vögler et al. (2005) was modified to dynamically switch off once the transition region is reached.”
Magnetic flux emergence in granular convection: radiative MHD simulations and observational signatures (2007, methodology): “The appearance of stronger magnetic fields several granulation timescales after the initial emergence of flux suggests that convective intensification operates (e.g., Nordlund & Stein, 1990; Grossmann-Doerth et al., 1998; Vögler et al., 2005; Stein & Nordlund, 2006).”
The Stagger-grid: A grid of 3D stellar atmosphere models - I. Methods and general properties (2013, methodology): “Beeck et al. (2012) compared solar models from three of the above 3D stellar 1 http://www.astro.ku.dk/~kg/Papers/MHD_code.ps.gz atmosphere codes (Stagger, CO5BOLD and MURaM), and showed that the models are overall very similar, despite the distinct numerical approaches.”
RADIATIVE MAGNETOHYDRODYNAMIC SIMULATION OF SUNSPOT STRUCTURE (2008, methodology): “At the bottom, the boundary is open for the flow and the magnetic field kept vertical (for details, see Vögler et al. 2005).”
HEATING OF THE SOLAR CHROMOSPHERE AND CORONA BY ALFVÉN WAVE TURBULENCE (2011, background): “This is plausible because the flux tubes are sur- rounded by convective downflows that are highly turbulent (Cattaneo et al. 2003; Vögler et al. 2005; Stein & Nordlund 2006; Bushby et al. 2008).”
The Magnetic Connection between the Convection Zone and Corona in the Quiet Sun (2007, background): “…the spectrum are more realistic threedimensionalMHDmodels of active region flux emergence through the turbulent surface layers (Cheung et al. 2007a) and of solar surface magnetoconvection (Bercik 2002; Stein & Nordlund 2002, 2006; Stein et al. 2003; Vögler et al. 2005; Schaffenberger et al. 2006).”
NUMERICAL SIMULATIONS OF QUIET SUN MAGNETISM: ON THE CONTRIBUTION FROM A SMALL-SCALE DYNAMO (2014, methodology): “Numerical scheme We use for our simulations the MURaM radiative MHD code (Vögler et al. 2005; Rempel et al. 2009).”
Solar Surface Magnetism and Irradiance on Time Scales from Days to the 11-Year Cycle (2009, methodology): “The MURaM code (Vögler 2003; Vögler et al. 2005) has been used for these simulations.”
A solar surface dynamo (2007, methodology): “Further details of the boundary conditions are described in Vögler et al. (2005).”
Numerical Modeling of Magnetohydrodynamic Wave Propagation and Refraction in Sunspots (2006, methodology): “To stabilize the code and reduce highfrequency variations on scales unresolved by the numerical scheme, we included artificial diffusion terms in equations (1)–(4) following the strategy described in Vögler et al. (2005).”