Two Models of Magnetic Support for Photoevaporated Molecular Clouds

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 con...

Full description

Saved in:
Bibliographic Details
Published inAstrophysics and space science Vol. 298; no. 1-2; pp. 183 - 190
Main Authors Ryutov, D D, Kane, J O, Mizuta, A, Pound, M W, Remington, B A
Format Journal Article
LanguageEnglish
Published Dordrecht Springer Nature B.V 01.06.2005
Subjects
Astrophysics
Magnetic fields
Online AccessGet full text

Cover

More Information
Summary: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.
Bibliography:ObjectType-Article-1
SourceType-Scholarly Journals-1
ObjectType-Feature-2
content type line 23
ObjectType-Article-2
ObjectType-Feature-1
ISSN:0004-640X
1572-946X
DOI:10.1007/s10509-005-3930-4