On the interpretation of the betap relation in interstellar clouds

Details On the interpretation of the betap relation in interstellar clouds On the interpretation of the betap relation in interstellar clouds

Oct 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986inpr.conf..166k&link_type=abstract

In NASA. Ames Research Center Summer School on Interstellar Processes: Abstracts of Contributed Papers p 166-168 (SEE N87-15043

Computer Science

Field Strength, Gas Density, Interstellar Gas, Interstellar Magnetic Fields, Molecular Clouds, Stellar Gravitation, Gravitational Effects, Particle Density (Concentration), Taylor Instability, Thermal Instability

Scientific paper

Troland and Heiles (1986) have recently presented an updated compilation of observational data concerning the relationship between the interstellar magnetic field strength B and the gas density rho (or, equivalently, the particle density n). One of the main findings of their survey was that B remains constant over the density range 0.1 - approx. 100 cu. cm and shows evidence for increase only a higher densities. They compared this result with theoretical predictions based on the Parker-instability scenario for the formation and evolution of interstellar clouds in the presence of the galactic magnetic field. In this picture, low-density gas is driven by the magnetic Rayleigh-Taylor instability into magnetic valleys, where it accumulates into denser concentrations. The gas initially flows along the magnetic field lines and there is little increase of the field strength with density; B only starts to rise when n becomes large enough for self-gravity to begin competing with the magnetic stresses. For a cloud mass of approx. 1,000M and the measured background field strength, the critical density for contraction in approx. 75 cu. cm. Troland and Heiles therefore concluded that this scenario is basically consistent with the observations. This conclusion is debated.

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