On the relation between CO and gamma-ray observations, cosmic rays, and the thickness of the galactic disk

Details On the relation between CO and gamma-ray observations, cosmic rays, and the thickness of the galactic disk On the relation between CO and gamma-ray observations, cosmic rays, and the thickness of the galactic disk

Oct 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975apj...201l...5w&link_type=abstract

Astrophysical Journal, vol. 201, Oct. 1, 1975, pt. 2, p. L5-L8.

Computer Science

Numerical Analysis

12

Cosmic Rays, Galactic Structure, Gamma Rays, Interstellar Gas, X Ray Astronomy, Galactic Nuclei, Gas Density, Numerical Analysis, Solar Atmosphere, Synchrotron Radiation, Turbulence Effects

Scientific paper

Recent CO observations suggest that dense clouds provide a high mean gas density (mostly H2) at approximately 5 kpc from the galactic center. Gamma-ray observations have been explained as resulting primarily from the interaction of cosmic rays with interstellar matter. The relationship between cosmic-ray density and mean gas density is discussed, and it is argued that the CO clouds must be dynamically independent of the gas that is observed in 21-cm line radiation. A plausible upper limit to the cosmic-ray density at 5 kpc from the galactic center is derived which is based on measurements of galactic-disk thickness and hydrogen turbulent velocities from 21-cm line data. An estimate is also made of the 'distributed' gas density which confines the cosmic rays to the disk. This upper limit is approximately five times the cosmic-ray density near the sun. Observations of the thickness of the galactic disk suggest that the cosmic-ray density increases with distributed gas density.

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