Julien Devriendt: Publications

Modelling the Galaxy Bimodality: Shutdown Above a Critical Halo Mass

(2006)

Authors:

A Cattaneo, A Dekel, J Devriendt, B Guiderdoni, J Blaizot

UV-optical colours as probes of early-type galaxy evolution

(2006)

Authors:

S Kaviraj, K Schawinski, JEG Devriendt, I Ferreras, S Khochfar, S-J Yoon, SK Yi, J-M Deharveng, A Boselli, T Barlow, T Conrow, K Forster, P Friedman, DC Martin, P Morrissey, S Neff, D Schiminovich, M Seibert, T Small, T Wyder, L Bianchi, J Donas, T Heckman, Y-W Lee, B Madore, B Milliard, RM Rich, A Szalay

Formation of structure in molecular clouds: A case study

Astrophysical Journal 633:2 II (2005)

Authors:

F Heitsch, A Burkert, LW Hartmann, AD Slyz, JEG Devriendt

Abstract:

Molecular clouds (MCs) are highly structured and turbulent. Colliding gas streams of atomic hydrogen have been suggested as a possible source of MCs, imprinting the filamentary structure as a consequence of dynamical and thermal instabilities. We present a two-dimensional numerical analysis of MC formation via converging H I flows. Even with modest flow speeds and completely uniform inflows, nonlinear density perturbations arise as possible precursors of MCs. Thus, we suggest that MCs are inevitably formed with substantial structure, e.g., strong density and velocity fluctuations, which provide the initial conditions for subsequent gravitational collapse and star formation in a variety of Galactic and extragalactic environments. © 2005. The American Astronomical Society. All rights reserved.

Formation of structure in molecular clouds: A case study

ASTROPHYSICAL JOURNAL 633:2 (2005) L113-L116

Authors:

F Heitsch, A Burkert, LW Hartmann, AD Slyz, JEG Devriendt

Formation of Structure in Molecular Clouds: A Case 51��

Astrophys.J. 633 (2005) L113-L116

Authors:

F Heitsch, A Burkert, L Hartmann, AD Slyz, JEG Devriendt

Abstract:

Molecular clouds (MCs) are highly structured and ``turbulent''. Colliding gas streams of atomic hydrogen have been suggested as a possible source of MCs, imprinting the filamentary structure as a consequence of dynamical and thermal instabilities. We present a 2D numerical analysis of MC formation via converging HI flows. Even with modest flow speeds and completely uniform inflows, non-linear density perturbations as possible precursors of MCs arise. Thus, we suggest that MCs are inevitably formed with substantial structure, e.g., strong density and velocity fluctuations, which provide the initial conditions for subsequent gravitational collapse and star formation in a variety of galactic and extragalactic environments.

51��