Magnetic Fields and Dispersion of Polarization Angles: IRAS Vela Shell

Details Magnetic Fields and Dispersion of Polarization Angles: IRAS Vela Shell Magnetic Fields and Dispersion of Polarization Angles: IRAS Vela Shell

Sep 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..784..743p&link_type=abstract

MAGNETIC FIELDS IN THE UNIVERSE: From Laboratory and Stars to Primordial Structures. AIP Conference Proceedings, Volume 784, pp

Computer Science

1

Stellar Polarimetry, Interstellar Molecular Clouds, Magnetic Fields, Polarimetry, Magnetic And Electric Fields, Polarization Of Starlight, Molecular Clouds, H2 Clouds, Dense Clouds, And Dark Clouds

Scientific paper

The dispersion of polarization position angles can provide an estimate of the ratio of kinetic energy density to magnetic energy density (ρkin/ρmag) and the local magnetic field strength in the interstellar medium, as first suggested by Chandrasekhar and Fermi (CF). Nevertheless, a relatively large number of data points are necessary in order to obtain a reasonable estimate. We use a recently published catalog of several hundreds of objects toward the western side of IRAS Vela Shell in order to investigate the distribution of the local magnetic field in small (~pc) scales across an ionization front (I-front). We find variations of ρkin/ρmag of one order magnitude along the I-front, with the magnetic pressure generally dominating over the turbulent motions. In a few cases the polarization angle appears to change randomly, suggesting that the kinetic energy may dominate. These findings suggest that the magnetic component has a significant contribution to the dynamical balance of this region. Along I-front, the mean magnetic field on the plane of the sky is (0.3 +/- 0.2) mgauss and the full range of variation is (0.2 - 1.1) mgauss.

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