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Scaling the magnetic field strength in interstellar clouds: resolution of the ''B versus n dilemma''

Journal Article · · Astrophys. J.; (United States)
DOI:https://doi.org/10.1086/160581· OSTI ID:6239745
The ''B versus n dilemma'' which Troland and Heiles associate with the near constancy of the magnetic field strength B (< or approx. =5 microgauss) based on H i Zeeman data over a range in gas densities 10/sup -1/ < or approx. =n(cm/sup -3/)< or approx. =10/sup 2/, can be resolved in terms of preferential mass flow along magnetic field lines as a result of a low thermal energy in these regions. Approximate relations for scaling the magetic field strength in interstellar clouds are found to be (n in cm/sup -3/): B(n> or approx. =100)roughly-equal3 microgauss and B(n< or approx. =100)roughly-equal3 microgauss (n/100)/sup 1/2/. It is the purpose of this paper to point out that the fiducial gas density for scaling the increasing magnetic field strength in interstellar clouds (calculated here to be approx.100 cm/sup -3/) is some two to three order of magnitude above the ''average'' interstellar density (0.1--1 cm/sup -3/) frequently (and erroneously) used to estimate B.
Research Organization:
Embry-Riddle Aeronautical University
OSTI ID:
6239745
Journal Information:
Astrophys. J.; (United States), Journal Name: Astrophys. J.; (United States) Vol. 264:1; ISSN ASJOA
Country of Publication:
United States
Language:
English

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Related Subjects

640105* -- Astrophysics &amp; Cosmology-- Galaxies
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
COSMIC GASES
COSMIC RADIO SOURCES
FLUID MECHANICS
FLUIDS
GASES
H1 REGIONS
HYDRODYNAMICS
INTERSTELLAR MAGNETIC FIELDS
MAGNETIC FIELDS
MECHANICS