An Additional Source of Turbulence in the Warm ISM of the Inner Galactic Plane ?

Details An Additional Source of Turbulence in the Warm ISM of the Inner Galactic Plane ? An Additional Source of Turbulence in the Warm ISM of the Inner Galactic Plane ?

Feb 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004mim..proc...87h&link_type=abstract

The Magnetized Interstellar Medium, Proceedings of the conference, held in Antalya, Turkey, September 8 - 12, 2003, Eds: B. Uyan

Physics

1

Scientific paper

We present structure functions of the rotation measure (RM) of diffuse Galactic synchrotron emission and of the emission measure (EM) of Hα emission in a test region for the Southern Galactic Plane Survey. The structure functions of RM and EM are remarkably similar: both show a break at a scale of approximately 4 arcmin, where the structure function flattens to a slope of about 0.2 at scales larger than the break. At scales r ⪆ 1 degree, the structure functions show an anisotropy with position angle on the sky which is believed to be created by a large-scale gradient in thermal electron density and possibly magnetic field across the observed region. The break and flattening of the spectrum can be explained if the radiation propagates through two Faraday screens, most likely the Carina and Local spiral arms. In this interpretation, it can be inferred from the position of the break in the structure function that the warm ISM exhibits structure up to an outer scale of a few parsec. We propose that the observed fluctuations in RM and EM are mainly caused by HII regions around late-type B stars, which are typically a few parsecs in size and sufficiently abundant. These HII regions may constitute the dominant source of turbulence in the inner Galactic plane, as opposed to the Kolmogorov-like turbulence out to scales of hundreds of parsecs observed at high Galactic latitudes.

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