Added Banerjee & Pudritz to my library.

Banerjee and Pudritz employed an EOS that was density and time dependent. They also incorporated radiative cooling into their model and studied both the isothermal and non-isothermal phases of the collapse of rotating BE spheres. As this is already much more complicated than our current rotating BE clumps, not sure how much of an overlap in results we can expect. Furthermore, they report seeing no fragmentation or 'non-central' collapse in the isothermal phase.. :/. (Currently the setup is only isothermal).

​https://clover.pas.rochester.edu/trac/astrobear/wiki/u/EricasLibrary

So I hope this isn't too silly, but, on an aside, if one does not initialize differential rotation, can the simulation relax to such a state on its own? Is this possible without the equation for such rotation explicitly written into astrobear? Or, do all numerical models operate on "if this condition, use this equation, for this q variable"? ..

Comments

1. Adam Frank -- 13 years ago

Not a silly question and I think depending on the initial conditions in the flow the answer must be yes. Conservation of angular momentum together with dissipation will change each particles Omega as it falls and depending on where it ends up you will not have solid body rotation at the end.