Speaker
Description
The interstellar gas is a key component for understanding cosmic-ray (CR)
physics as it is the target for the generation of secondary CR particles
and the high-energy interstellar emission. Observations of the spectra and
abundances of these secondary particles are used to decipher the
propagation history of CRs and to decode possible signatures of new physics.
Until now, most calculations of CR propagation have used 2D
cylindrically symmetric models for the distribution of the interstellar gas.
This is partly due to the inevitable difficulties in determination of the 3D
gas distributions. We present a method for determination of the 3D
distribution of interstellar gas and our preliminary results. We discuss the
effect these new 3D models may have on the analysis and interpretation of CR
propagation and high-energy interstellar emissions.
