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B. Pichardo, E. Vazquez-Semadeni (Instituto de Astronomia, UNAM), J. Ballesteros-Paredes (Instituto de Astronomia, UNAM, and Harvard-Smithsonian CFA), A. Gazol, T. Passot (Observatory of Nice)
We present three-dimensional numerical simulations of turbulence in two different regimes: a) Full models of the ISM including the magnetic field, parameterized cooling and diffuse and stellar heating, self-gravity and rotation. b) Barotropic flows (P \propto \rho\gamma), with \gamma smaller, equal and larger than 1. We compare the physical-space density distribution with its representation in position-position-velocity space, noting that the two may give very different views, the latter introducing features of the velocity structure into that of the density. We compare the morphologies of both regimes with that of spectral map observational data. Finally, we present preliminary results of a Principal Component Analysis (PCA) of the numerical data.
The author(s) of this abstract have provided an email address for comments about the abstract: barbara@astroscu.unam.mx