• CO5BOLD non-magnetic solar comparison model: Emergent continuum intensity (Salhab, Steiner, Steffen 2017)
  d3gt57g44rsn01_400x400x188_int01B3_R_070-080.mpg

• CO5BOLD non-magnetic solar comparison model: Line wing intensity showing reversed granulation (Salhab, Steiner, Steffen 2017)
  d3gt57g44rsn01_400x400x188_int03B3_R_070-080.mpg

• CO5BOLD solar magneto-convection with <Bz>=50 G : Emergent continuum intensity (see Salhab et al. 2018, A&A 614, A78)
  d3gt57g44v50rsn01_400x400x188_int01B3_R_070-081.mpg

• CO5BOLD solar magneto-convection with <Bz>=50 G: Line wing intensity showing reversed granulation (see Salhab et al. 2018, A&A 614, A78)
  d3gt57g44v50rsn01_400x400x188_int03B3_R_070-081.mpg

• CO5BOLD solar magneto-convection with <Bz>=50 G: Magnetic f field strength |B| in vertical slice (see Salhab et al. 2018, A&A 614, A78)
  d3gt57g44v50rsn01_400x400x188_bfield_070-081_yellow.mpg

• CO5BOLD solar magneto-convection with <Bz>=100 G: Emergent continuum intensity (Salhab, Steiner, Steffen 2017)
  d3gt57g44v100rsn01_400x400x188_int01B3_R_070-080.mpg

• CO5BOLD solar magneto-convection with <Bz>=100 G: Line wing intensity showing reversed granulation (Salhab, Steiner, Steffen 2017)
  d3gt57g44v100rsn01_400x400x188_int03B3_R_070-080.mpg

• CO5BOLD solar magneto-convection with <Bz>=100 G: Magnetic f field strength |B| in vertical slice (Salhab, Steiner, Steffen 2017)
  d3gt57g44v100rsn01_400x400x188_bfield_070-080_yellow.mpg

• CO5BOLD low-resolution solar MHD with <Bz>=200 G (magnetic field) [Steffen 2019]
  d3gt57g44b200n59b_bfield_150-200.mpg

• CO5BOLD low-resolution solar MHD with <Bz>=200 G (emergent intensity) [Steffen 2019]
  d3gt57g44b200n59b_intensity_150-200.mpg