EAS Publications Series
Volume 56, 2012The Role of the Disk-Halo Interaction in Galaxy Evolution: Outflow vs. Infall?
|Page(s)||81 - 86|
|Section||Structure and Components of the ISM in Galaxies|
|Published online||17 September 2012|
Miguel A. de Avillez (ed)
EAS Publications Series, 56 (2012) 81–86
Magnetic Milky Way
Herzberg Institute of Astrophysics, National Research Council Canada, 5071 West Saancih Road, Victoria, BC V9E 2E7, Canada
Spiral arm shapes, locations, and velocities can be well determined, when model pitfalls are avoided (Vallée 2008a). Similarly, circularly orbiting gas and magnetic field lines can cross the spiral arms, when observational pitfalls are avoided (Vallée 2008b).
© EAS, EDP Sciences, 2012