The magnetic field in a protostellar cloud

The present investigation of both the isothermal and nonisothermal regions' B-rho relation gives attention to the magnetic dissipation, which can occur by way of either ambipolar diffusion or Ohmic dissipation. It is found that magnetic flux begins to dissipate via ambipolar diffusion at a neut...

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Bibliographic Details
Published in:	Astrophysics and space science Vol. 164; no. 2; pp. 213 - 229
Main Author:	EL-NAWAWY, M. S
Format:	Journal Article
Language:	English
Published:	Dordrecht Kluwer 01-02-1990
Subjects:	Astronomy Earth, ocean, space Exact sciences and technology Star formation Stars Stellar characteristics and properties Theoretical study Interstellar cloud Ionization Magnetic field Proto stellar nebula Ambipolar diffusion
Online Access:	Get full text
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Summary:	The present investigation of both the isothermal and nonisothermal regions' B-rho relation gives attention to the magnetic dissipation, which can occur by way of either ambipolar diffusion or Ohmic dissipation. It is found that magnetic flux begins to dissipate via ambipolar diffusion at a neutral density above 3 x 10 to the 9th/cu cm; this process remains in effect until densities above 10 to the 11th are reached, where Ohmic dissipation dominates. The rates of heating by both Ohmic dissipation and ambipolar diffusion are smaller than the rate of compressional heating in the case of magnetic dissipation. (O.C.)
Bibliography:	ObjectType-Article-2 SourceType-Scholarly Journals-1 ObjectType-Feature-1 content type line 23
ISSN:	0004-640X 1572-946X
DOI:	10.1007/BF00658825