Numerical simulation of the three-dimensional structure and dynamics of the non-magnetic solar chromosphere

By S. Wedemeyer, Bernd Freytag, M. Steffen, H. Ludwig, H. Holweger. 2003

227 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/b8325777ff74b376d919246aca277153cc5a4a24

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In Astronomy and Astrophysics

Citations in the corpus

First stars XII. Abundances in extremely metal-poor turnoff stars,and comparison with the giants (2009, methodology): “To accomplish this, we used the two CO5BOLD (Freytag et al. 2002; Wedemeyer et al. 2004) 3D models described in Paper XI (Teff/log g/[Fe/H]: 6550/4.”
On the Generation, Propagation, and Reflection of Alfvén Waves from the Solar Photosphere to the Distant Heliosphere (2004, background): “Compressible MHD waves and shocks must also be considered alongside the incompressible waves modeled in this paper (for recent work, see Rosenthal et al. 2002; Bogdan et al. 2002, 2003; Hasan et al. 2003; Hasan & Ulmschneider 2004; Wedemeyer et al. 2004; Bloomfield et al. 2004; Suzuki 2004).”
The metal–poor end of the Spite plateau: gravity sensitivity of the Hα wings fitting. (2009, unknown): “…Ali & Griem (1966) self-broadening theories (BA and ALI scales); H α ﬁtting against a 3D-hydrodynamical grid based on CO 5 BOLD models (Freytag et al. 2002; Wedemeyer et al. 2004) with Barklem et al. (2000) self-broadening (3D scale); InfraRed Flux method (IRFM, Gonz´alez Hern´andez & Bonifacio…”
SOLAR MODELS WITH ACCRETION. I. APPLICATION TO THE SOLAR ABUNDANCE PROBLEM (2011, background): “…last decade, the advent of 3D hydrodynamic models of near-surface solar convection (Stein & Nordlund 1998; Asplund et al. 2000; Freytag et al. 2002; Wedemeyer et al. 2004), a more careful selection of spectral lines (e.g. Allende Prieto et al. 2001) and, in some cases, relaxation of the assumption…”
Sub-surface convection zones in hot massive stars and their observable consequences (2009, methodology): “In order to verify such a picture, multi-dimensional calculations of the FeCZ and the radiative layers above, including the stellar atmosphere, are required – similar to the recent generation of atmosphere models for cool stars (e.g., Asplund et al. 1999; Wedemeyer et al. 2004).”
THE FORMATION OF THE Hα LINE IN THE SOLAR CHROMOSPHERE (2012, result): “Still, if we assume it is valid and apply it, our observations yield internetwork temperatures compatible with radiation-MHD simulations of the internetwork chromosphere (Carlsson & Stein 1995; Skartlien 2000; Wedemeyer et al. 2004; Leenaarts et al. 2007).”
Helioseismology and Solar Abundances (2007, methodology): “They used 3D models computed with CO5BOLD code (Freytag et al. 2002; Wedemeyer et al. 2004).”
Emergence of magnetic flux from the convection zone into the corona (2004, unknown): “…simultaneously present, the latter being created by the dissipation of vertically running waves generated mainly through the ongoing convection in the (sub)photospheric levels and steepening to yield shocks (Ayres 1981; Asensio Ramos et al. 2003; Carlsson & Stein 2002; Wedemeyer et al. 2004).”