VLA OH Zeeman Magnetic Field Detections Toward Five Galactic Supernova Remnants. C. L. Brogan 1 , D. A. Frail 2 , W. M. Goss 2 , & T. H. Troland 1. ( 1 University of Kentucky; 2 National Radio Astronomy Observatory).
Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.
VLA OH Zeeman Magnetic Field Detections Toward Five Galactic Supernova Remnants
C. L. Brogan1, D. A. Frail2, W. M. Goss2, & T. H. Troland1
(1 University of Kentucky; 2 National Radio Astronomy Observatory)
Abstract: We have observed the OH (1720 MHz) line in five galactic SNRs with the VLA to measure their magnetic field strengths using the Zeeman effect. Our estimated fields range from 0.2 to 2 mG. The magnetic field strengths are consistent with the hypothesis that ambient molecular cloud magnetic fields are compressed via the SNR shock to the observed values. Magnetic fields of this magnitude exert a considerable influence on the the cloud with the magnetic pressures (10-7 - 10-9 erg cm-3) exceeding the pressure in the ISM or even the thermal pressure of the hot gas interior to the remnant.
Figure 3: Cartoon of SNR/molecular cloud interaction. In this picture, X-rays (from the SNR) and cosmic rays excite the Lyman-Werner bands of H2 which in turn re-radiate in the FUV (see Wardle 1999). This weak FUV flux can then dissociate ~ 1% of the H2O synthesized in the C-type shock to produce the OH abundance needed for maser production in the postshock gas. Comparison of estimates for the pre and postshock densities suggest that the postshock magnetic fields are amplified from their preshock values by simple shock compression (i.e. rps/ro ~ Bps /Bo).
Figure 1: Continuum images of the observed SNRs along with a Table of our OH (1720 MHz) maser Zeeman magnetic field detections. Note that field values were calculated using the “thermal” Zeeman equation so that the listed field strengths could overestimate the total field strength by up to a factor of five (e.g. Elitzur 1996). The maser locations in each SNR are marked by plus symbols or crosses.
Figure 2: Sample fits of the Zeeman magnetic field strengths for W51. The upper panels show the VLA Stokes I profiles (solid histograms), and the lower panels show the VLA Stokes V profiles (solid histograms) with the fitted derivative of Stokes I shown as smooth dotted curves.
Preprint available at http://www.pa.uky.edu/~brogan