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The resolved magnetic fields of the quiescent cloud GRSMC 45.60+0.30

Published online by Cambridge University Press:  05 March 2015

Michael D. Pavel ,
Robert C. Marchwinski  and
Dan P. Clemens
Michael D. Pavel
Affiliation:
Institute for Astrophysical Research, Boston University, Boston, MA 02215, USA email: pavelmi@astro.as.utexas.edu
Robert C. Marchwinski
Affiliation:
Institute for Astrophysical Research, Boston University, Boston, MA 02215, USA email: pavelmi@astro.as.utexas.edu
Dan P. Clemens
Affiliation:
Institute for Astrophysical Research, Boston University, Boston, MA 02215, USA email: pavelmi@astro.as.utexas.edu
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Marchwinski et al. (2012) mapped the magnetic field strength across the quiescent cloud GRSMC 45.60+0.30 (shown in Figure 1 subtending 40x10 pc at a distance of 1.88 kpc) with the Chandrasekhar-Fermi method CF; Chandrasekhar & Fermi 1953) using near-infrared starlight polarimetry from the Galactic Plane Infrared Polarization Survey (Clemens et al.2012a, b) and gas properties from the Galactic Ring Survey (Jackson et al.2006). The large-scale magnetic field is oriented parallel to the gas-traced ‘spine’ of the cloud. Seven ‘magnetic cores’ with high magnetic field strength were identified and are coincident with peaks in the gas column density. Calculation of the mass-to-flux ratio (Crutcher 1999) shows that these cores are exclusively magnetically subcritical and that magnetostatic pressure can support them against gravitational collapse.

Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 10 , Highlights H16: Highlights of Astronomy , August 2012 , pp. 615
Copyright
Copyright © International Astronomical Union 2015 

References

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