"Oh No" schreef in bericht
...

In this case you are wrong. The math has been done, in the form of
simulations on supercomputers.

That is correct. However all of this is very complicated
and very difficult to evaluate if it is done correctly.

To get an idea about the software being used read this:
http://www.mpa-garching.mpg.de/galfo...get2-paper.pdf
"The cosmological simulation code GADGET-2" by Volker Springel
The above software also takes supernovae into account.
The details are at page 1109.
SPH = Smoothed Particle Hydrodynamics

For a general document about SPH simulations read this:
http://arxiv.org/PS_cache/arxiv/pdf/...001.3115v1.pdf
"Gas cooling in semi-analytic models and SPH simulations: are
results consistent?"
Specific read the introduction.
Here we read:
"In fact, lacking a 'complete theory' of star formation (as well
as of almost all the physical processes at play), we are currently not
in the position to model galaxy formation from first principles"

For a detailed document using Gadget 2 read this:
http://arxiv.org/PS_cache/arxiv/pdf/...909.0664v1.pdf
"Simulating the effect of AGN feedback on the metal enrichment of
galaxy clusters"

IMO there are two types of simulations:
1. N body simulations. A typical application is the merger of two galaxies.
2. Physical simulations. A typical application is one supernova.
Of course you can combine those two.
The problem is they are extremely complex.
For example: to study metal enrichment in a galaxy.
The easy part is that you can test your simulation because this simulation
belongs to the visible realm.
What IMO is also important that this is some sort of mixing process
i.e. the leftovers from the supernova are the building blocks
for the next generation of "heavier" stars.

In the simulation under discussion:
"Bulgeless dwarf galaxies and dark matter cores from
supernova-driven outflows" the physics involved is totally different:
the underlying concept is gas removal.
The question now becomes:
How does CDM responds to a supernova ?
Will it stay within or will it be removed from ?
IMO the simplest is a mixing process.
A removal process which results in a halo (NFW profile)
is much more complex.
See also:
http://en.wikipedia.org/wiki/Navarro...3White_profile
The extra complication is that this whole process which
involves dark matter is invisible.

For more comments see:
http://users.telenet.be/nicvroom/nat...Jan%202010.htm

Regards

--
Charles Francis

http://www.rqgravity.net

Nicolaas Vroom