Modeling Large-Scale Magnetic Fields in the Milky Way - ESA

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Spiral arm ridges: separable?synch total Isynch PIsynch PI/Idust total Idust PIdust PI/IRMJaffe et al. (2013)T. Jaffe @ ESAC, 30 May 2013
Arm modulation?• Model of shock compression in spiral arms predicts roughly a factor of four ratiobetween pre- and post-shock for the component of the fields parallel to the shock,for the gas and dust, and at least that for the CREs.• This is not observed in synchrotron in external galaxies (e.g. M51) but it’s not clearwhether the observations have the resolution given that the shock region could befairly narrow.• CRE sources are also not uniformly distributed, and the CREs may remain highlyinhomogeneous if the diffusion is highly anisotropic. Two effects, one in shock and onedownstream, effectively smoothing it out?M51 and field by Fletcher et al. (2011)T. Jaffe @ ESAC, 30 May 2013Effenberger et al. (2012)
Page 1 and 2: Modeling Galactic Magnetic Fieldswi
Page 3 and 4: CMB foregrounds: Planck view(ESA, H
Page 5 and 6: External galaxies: other examplesNG
Page 7 and 8: Small-scale field: TurbulenceEMLS I
Page 9 and 10: GeometryCoherent• Coherent contri
Page 11 and 12: A very brief review of recent workT
Page 13 and 14: Field reversals?• Reversals => dy
Page 15 and 16: Local structure?• Sky visibly dom
Page 17 and 18: Modeling: hammurabi• Hammurabi Co
Page 19 and 20: Cartoon example:T. Jaffe @ ESAC, 30
Page 21 and 22: Cartoon example:coherent+ isotropic
Page 23 and 24: Cartoon example:coherent+ isotropic
Page 25 and 26: First results:• 8 parameters fit:
Page 27 and 28: CRE results:0.408 GHz(total I)2.3 G
Page 29: Spiral arm ridges: separable?Spiral
Page 33 and 34: Small scales: turbulence and depola
Page 35 and 36: Radio spurs, microwave haze, and Fe
Page 37 and 38: Prospects:• C-Band All Sky Survey
Page 39 and 40: SKA!SKA will allow Faraday RM measu

Modeling Large-Scale Magnetic Fields in the Milky Way - ESA

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