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The Mass Spectra of Cores in Turbulent Molecular Clouds and Implications for the Initial Mass Function

  • Authors: Javier Ballesteros-Paredes, Adriana Gazol, Jongsoo Kim, Ralf S. Klessen, Anne-Katharina Jappsen, and Epimenio Tejero

Ballesteros‐Paredes et al. 2006 The Astrophysical Journal 637 384.

  • Provider: AAS Journals

Caption: Fig. 1.

Temporal evolution of the Mach number (top); and the number of cores found in the SPH models (middle) and in the TVD models (bottom). Solid lines denote SPH runs, and dotted lines denote TVD runs. Quoted numbers in the top panel give the mean Mach number, averaged over the frames whose times are larger than one turbulent crossing time (see Table 1). Note that after 1 turbulent crossing time, the fluid has reached equilibrium, since (1) the Mach number becomes nearly constant, with fluctuations not larger than 6.5% (top), and (2) the number of cores has reached its typical value. Note that fluctuations up to 20% in the number of cores can still be found, showing the importance of averaging over several time steps when calculating CMDs.

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