Extension to cosmic scales of the magnetic field versus gas density relationship

Details Extension to cosmic scales of the magnetic field versus gas density relationship Extension to cosmic scales of the magnetic field versus gas density relationship

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...239...57v&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 239, no. 1-2, Nov. 1990, p. 57-62.

Astronomy and Astrophysics

Astrophysics

24

Cosmology, Galactic Clusters, Intergalactic Media, Interstellar Magnetic Fields, Spiral Galaxies, Gravitational Collapse, H I Regions, Linear Polarization, Milky Way Galaxy

Scientific paper

Using linear polarization data, a magnetic field versus gas density relationship is obtained here for the first time, from interstellar bubbles (100 pc) to superclusters of galaxies (50 Mpc). The present study obtains a good fit for the general form B equal to about N exp k, where k is about 0.2 for these scales (50 Mpc or 100 pc). Using circular polarization observations, the relationship between the magnetic field B and the gas density N has been well studied before in the Milky Way galaxy for H I clouds and molecular complexes down to maser clumps. These earlier studies have found a magnetic field B versus gas density N relationship of the general form B equal to about N exp k, where k is about 0.4 for these scales (10 pc to 0.001 pc). The larger scales exhibit the widespread turbulences often found in dynamos in the universe on many scales (100 pc to 50 Mpc), while the smaller scales exhibit frozen-in magnetic fields and virial equilibrium in clouds and clumps (10 pc to 0.001 pc).

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