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Chemical Evolution of Turbulent Multiphase Molecular Clouds
Valeska Valdivia, Patrick Hennebelle, Benjamin Godard +3
Molecular clouds are essentially made up of atomic and molecular hydrogen, which in spite of being the simplest molecule in the ISM plays a key role in the chemical evolution of mo…
Stellar mass spectrum within massive collapsing clumps II. Thermodynamics and tidal forces of the first Larson core
Yueh-Ning Lee, Patrick Hennebelle
We investigate the dependence of the peak of the IMF on the physics of the so-called first Larson core, which corresponds to the point where the dust becomes opaque to its own radi…
Stellar mass spectrum within massive collapsing clumps I. Influence of the initial conditions
Yueh-Ning Lee, Patrick Hennebelle
We conduct numerical experiments in which we systematically vary the initial density over four orders of magnitude and the turbulent velocity over a factor ten. In a companion pape…
The FRIGG project: From intermediate galactic scales to self-gravitating cores
Patrick Hennebelle
Abridged. Understanding the detailed structure of the interstellar gas is essential for our knowledge of the star formation process. The small-scale structure of the interstellar m…
Analytical core mass function (CMF) from filaments: Under which circumstances can filament fragmentation reproduce the CMF?
Yueh-Ning Lee, Patrick Hennebelle, Gilles Chabrier
Observations suggest that star formation in filamentary molecular clouds occurs in a two-step process, with the formation of filaments preceding that of prestellar cores and stars.…
The Formation of Massive Molecular Filaments and Massive Stars Triggered by a MHD Shock Wave
Tsuyoshi Inoue, Patrick Hennebelle, Yasuo Fukui +3
Recent observations suggest that intensive molecular cloud collision can trigger massive star/cluster formation. The most important physical process caused by the collision is a sh…