pdf 3.6 MB

More documents

Recommendations

Info

Wednesday, September 5, 12 At 5123 100 and the usual set 100 up: As before mass of planetesimals 0 depends on 0 the available mass. 500 400 300 200 100 500 400 300 200 100 0 100 200 300 400 500 t=36.1 0 0 100 200 300 400 500 t=36.3 0 0 100 200 300 400 500 0 100 200 300 400 500 t=36.2 0 0 100 200 300 400 500 new: Intermediate Formation of Binaries; Johansen, Klahr & Henning (2011) 500 400 300 200 100 500 400 300 200 100 t=36.5 0 0 100 200 300 400 500 Fig. 6. The particle column density as a function of time after self-gravity is turned on after t = 35.0Torb. Theinsertshowsanenlargementofthe region around the point of highest column density.
Not the process but numerical resolution limit the smallest possible planetesimals. Johansen, Klahr & Henning 2011 To predict an initial mass distribution of Planetesimals one needs A: the proper size distribution of precursors and B: the likely hood 12/13/2009 for concentrations Hubert as Klahr a - Planet function Formation - MPIA of particle size. 10 Heidelberg Wednesday, September 5, 12
Page 1 and 2: The Role of Turbulence in Planetesi
Page 3 and 4: Turbulence in a non rotating frame:
Page 5 and 6: V e r t i c a l From dust/gas eq. 1
Page 7 and 8: Disk: 12/13/2009 Hubert Klahr - Pla
Page 9: Formation Of Planetesimals From pre
Page 13 and 14: Natalia Dziurkevich (in prep.) see
Page 15 and 16: 12/13/2009 Hubert Klahr - Planet Fo
Page 17 and 18: Ri 0.001 0.000 �0.001 �0.002
Page 19 and 20: 12/13/2009 Hubert Klahr - Planet Fo
Page 21 and 22: 2D axissymetric Pluto Simulation: T
Page 23 and 24: 2D axissymetric Pluto Simulation: R
Page 25 and 26: Interface MRI - Dead Zone linear ax
Page 27 and 28: Small particles in pressure maxima
Page 29 and 30: St = 0.05 particles (few millimeter
Page 31: Conclusions: Johansen and Klahr: Hi

pdf 3.6 MB

You also want an ePaper? Increase the reach of your titles

Delete template?

Save as template?