Changes between Version 5 and Version 6 of u/JCMar2212


Ignore:
Timestamp:
03/22/12 15:40:01 (13 years ago)
Author:
Jonathan
Comment:

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  • u/JCMar2212

    v5 v6  
    318318== Questions ==
    319319 * Does driving turbulence before turning on gravity, give turbulence a head start in dominating structures on all scales? 
    320  * Does their choice of periodic boundaries prevent gravity's strongest mode
    321  * Is it fair to assume that every cell that is denser then the critical density is surrounded by enough mass to collapse?
    322  * What is their IMF or CMF?
     320 * Does their choice of periodic boundaries prevent gravity's strongest mode?  The box is 5-10 Jeans lengths so it should globally collapse in 1 free fall time.  Periodic boundaries == Fictitious dark energy...
     321
     322[[Image(blog:johannjc11102011:UniformCollapse.jpg, width=800)]]
     323  By .4 t_ff, the radius is at .9 and the density should have increased by 30%...
     324
     325
     326
     327 * Is it fair to assume that every cell that is denser then [[latex($8000 \rho_0$)]] will collapse?  Or that every cell denser than [[latex($\rho_{cr}$)]] is surrounded by enough mass to collapse?  [[latex($\rho_{cr}/\rho_0= .547 \alpha_{vir} \mathcal{M}^2$)]] so [[latex($8000 \rho_0 > \rho_{cr}$)]] for all the choices of [[latex($\mathcal{M}$)]] and [[latex($\alpha_{vir}$)]].  But numerous instabilities can destabilize the shocks before they have built up a thick layer of material...  Especially the NTSI (Blondin & Marks 1996).  It would have been instructive to have seen an IMF
     328
     329
     330
     331
     332 = Colliding Supersonic Flows =
     333
     334
    323335
    324336 = [http://arxiv.org/pdf/1107.3616v1.pdf Clustered Star Formation in Magnetic Clouds: Properties of Dense Cores Formed in Outflow-Driven Turbulence] (Nakamura & Li) =
     
    333345  * [[latex($\beta = 2$)]] (W)
    334346  * [[latex($\beta = .2$)]] (S) (initial virial equilibrium with turbulence)
     347