Dissipation of magnetic fields in very dense interstellar clouds. I - Formulation and conditions for efficient dissipation

Details Dissipation of magnetic fields in very dense interstellar clouds. I - Formulation and conditions for efficient dissipation Dissipation of magnetic fields in very dense interstellar clouds. I - Formulation and conditions for efficient dissipation

Feb 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986mnras.218..663n&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 218, Feb. 15, 1986, p. 663-684. Research supported by t

Astronomy and Astrophysics

Astronomy

86

Energy Dissipation, Interstellar Magnetic Fields, Interstellar Matter, Molecular Clouds, Particle Motion, Charged Particles, Cosmic Gases, Density Distribution, Drift Rate, Equations Of Motion, Gas Ionization, Ohmic Dissipation, Plasma Drift, Resistance Heating

Scientific paper

The present determination of the drift velocity V(B) of magnetic fields relative to a fluid, by solving the motions of a large variety of charged particles, notes that any closed curve moving with V(B) has a constant magnetic flux whose velocity contains the effects of both plasma drift and Joule dissipation. While v(B) is at least one order of magnitude smaller than the free fall velocity u(f) at a hydrogen density n(H) of less than about 10 to the 11th/cu cm (so that field dissipation is inefficient), n(H) greater than 10 to the 12th/cu cm and temperatures lower than 1000 K result in v(B) exceeding u(f) despite inefficient thermal ionization.

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