1. Allow gravity to form ìmolecular cloudsî (watch out for turbulence, clouds might take a while to formÖor use pressure-cooker to speed up the process)
2. Allow turbulent cascade to form in molecular cloud (be careful with the B-field)
3. Let magnetic turbulence & support decay enough for ìdense coresî to form in molecular clouds (be careful to watch for core-core interactions & outflows)
4. Watch dense cores slowly collapse, until one (or several?) Kelvin-Helmholtz-radiating protostar(s) form(s) near the center
Steps:
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