On May 29, 2013, at 3:17 PM, Comer Duncan wrote: > Hi Eric, > > Thanks for your reply. > > I found a reference to an old paper by Vulcanov in which he mentions a thorn > he calls Cosmo which is purported to begin to include cosmological > backgrounds and expanding outer bc. However, I can not seem to find such > nowadays in ET. Do you remember it? If so, is it now defunct and/or > inadequate? > > Treating the expanding background as an asymptotic bc with a gauge choice is > something I thought about. I was just thinking of running some problems > using McLachlan with say FRW outer bc and was wondering whether McLachlan has > been used by anyone in this context? I have not seen such.
Hi Comer, if the work from Vulcanov is the one I'm thinking of (http://arxiv.org/abs/gr-qc/0210006), then that involved ODEs (assuming that all the 3+1 quantities were spatial constants), so no boundary conditions were required. You can find an example of a full 3D evolution of a cosmological model with the ET in the ET paper (http://arxiv.org/abs/1111.3344), and the corresponding parameter file under the par/arXiv:1111.3344/cosmology/ directory in your ET tree. Using FLRW only as a boundary condition is a completely different story, which entails, among other things, figuring out whether that specification is compatible with the evolution equations. Which sort of spacetime do you have in mind? I suggest straightening out the formulation of the problem before turning to the technical question of how to implement this in Cactus. Best, Eloisa _______________________________________________ Users mailing list Users@einsteintoolkit.org http://lists.einsteintoolkit.org/mailman/listinfo/users
