Talk:Stellar convection simulations

From Scholarpedia

This page is not peer reviewed.
[edit]

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
[edit]

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
Retrieved from "http://www.scholarpedia.org/article/Talk:Stellar_convection_simulations"
For authors