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Galactic structure and turbulence, pulsar distances, and the intergalactic medium

Published online by Cambridge University Press:  20 March 2013

J. M. Cordes
J. M. Cordes*
Affiliation:
Astronomy Department, Cornell University email: jmc33@cornell.edu
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Abstract

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This paper summarizes how multi-wavelength measurements will be aggregated to determine Galactic structure in the interstellar medium (ISM) and produce the next-generation electron density model. Fluctuations in density and magnetic field from parsec scales down to about 1000 km cause a number of propagation effects in both radio waves and cosmic rays. Density microstructure appears to include Kolmogorov-like turbulence. The next generation electron-density model, NE2012, will include about double the number of lines of sight with dispersion and scattering measurements and it will be anchored with a much larger number of pulsar parallax distances. The foreground Galactic model is crucial for inferring similar ionized structures in the intergalactic medium (IGM) from scattering measurements on high-z objects. Intergalactic scattering is discussed with reference to distant sources of radio bursts. In particular, the cosmological radio scattering horizon is defined along with its analog for the ISM.

Keywords

plasmasturbulencestars: neutronpulsars: generalISM: magnetic fieldsGalaxy: structure
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S291: Neutron Stars and Pulsars: Challenges and Opportunities after 80 years , August 2012 , pp. 211 - 216
Copyright
Copyright © International Astronomical Union 2013

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