Modelling Star Formation with AMR* Simulations
Modelling Star Formation with AMR* Simulations
Modelling Star Formation with AMR* Simulations
Create successful ePaper yourself
Turn your PDF publications into a flip-book with our unique Google optimized e-Paper software.
<strong>Star</strong> <strong>Formation</strong> <strong>with</strong> AMR <strong>Simulations</strong><br />
Collapse of Hydrostatic Cores<br />
Slowly rotating Bonnor-<br />
Ebert-Spheres<br />
Low Mass M ~ 2.1M sol<br />
High Mass ~ 170 M sol<br />
Cooling due to molecular<br />
excitations, gas-dust<br />
interaction, H 2<br />
dissociation<br />
AMR ⇒ resolves Jeans<br />
length <strong>with</strong> more than 8<br />
grid points during collapse<br />
(Truelove et al. 1997)<br />
Up to 27 refinement levels<br />
(dynamical range ~ 10 7 )<br />
Initial conditions:<br />
cool molecular cloud (T =<br />
16 K)<br />
hot ambient, low density,<br />
medium (pressure match at<br />
the sphere boundary)<br />
Ωt ff<br />
= 0.1 - 0.4<br />
BE-density profile<br />
ITA Colloquium, Nov. 6, 2006
Change language