Two Models of Magnetic Support for Photoevaporated Molecular Clouds

Details Two Models of Magnetic Support for Photoevaporated Molecular Clouds Two Models of Magnetic Support for Photoevaporated Molecular Clouds

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005ap%26ss.298..183r&link_type=abstract

Astrophysics and Space Science, Volume 298, Issue 1-2, pp. 183-190

Astronomy and Astrophysics

Astrophysics

7

Molecular Clouds, Photoevaporation, Mhd Turbulence, Reconnection

Scientific paper

The thermal pressure inside molecular clouds is insufficient for maintaining the pressure balance at an ablation front at the cloud surface illuminated by nearby UV stars. Most probably, the required stiffness is provided by the magnetic pressure. After surveying existing models of this type, we concentrate on two of them: the model of a quasi-homogeneous magnetic field and the recently proposed model of a “magnetostatic turbulence”. We discuss observational consequences of the two models, in particular, the structure and the strength of the magnetic field inside the cloud and in the ionized outflow. We comment on the possible role of reconnection events and their observational signatures. We mention laboratory experiments where the most significant features of the models can be tested.

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