# Talk:Stellar convection simulations

### To the editors

A very impressive entry on convection, covering a lot of ground. It does, however, need a few changes, as detailed below, and carried out in the edited version of the entry.

I would also like to apologize to the editors, as well as the authors, for tardiness of my contribution. I hope it will, in the end, benefit all parties involved.

   Best wishes,

       Regner Trampedach


### To the authors

I have changed the order and heading of some sections, please make sure these changes make sense and that the new sections have the necessary introductions.

A number of remaining issues (in chronological order):

"Going beyond MLT:...":

• Explain why (if) we need to go to resolutions that encompass Re=10^{12}.
• Define RGB and AGB stars.

"Surface Convection":

• I think it would be a good idea to show some observations of Solar granulation, here. I would like to suggest pictures from the Solar Swedish Telescope (SST), which can be found at: [1]

There are several astonishing ones!

"Convection and Rotation":

• Fig. 2: At what depth does Fig. 2 show the radial velocity?

"Differential Convection and Rotation in the Sun":

• Explain Reynolds stresses,
• ...and how they can affect large scale flows.
• Explain what is meant by "...thermal wind balance..."
• Define references BT02, MBT06.

"Convective Dynamos"

• Should this section be split up into further sub-sections?
• Better wording of the explanation of how convection "...can convert toroidal flux to poloidal flux through the fragmentation and dispersal of photospheric active regions." I don't quite see what the fragmentation and dispersal has to do with the flux conversion.
• Explain what effect HD and MHD instabilities might have on the evolution of the Solar radiative interior.
• This sentence is not clear to me: "The large-scale magnetic torques are found to be 2 orders of magnitude smaller, confirming the small dynamical role played by the mean fields in global MHD simulations without a tachocline of shear and a self-established 11-yr cycle." - and do the MHD simulations have the 11 yr cycle or not?

"Conclusions":

• I find that the conclusions don't quite agree with the text.
• Maybe a conclusion isn't really needed in this forum.
• Maybe "Recommended reading" (monographs) and "External links" would be more useful for a user of scholarpedia - I stole the idea from a quick glance at other entries in scholarpedia.

And thanks for contributing to this excellent resource for the greater community.

    Best wishes,

       Regner Trampedach