The velocity distribution of interstellar gas observed in strong UV absorption lines

Details The velocity distribution of interstellar gas observed in strong UV absorption lines The velocity distribution of interstellar gas observed in strong UV absorption lines

Aug 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978apj...223..876c&link_type=abstract

Astrophysical Journal, Part 1, vol. 223, Aug. 1, 1978, p. 876-883.

Mathematics

Probability

36

Absorption Spectra, Interstellar Extinction, Interstellar Gas, Ultraviolet Absorption, Velocity Distribution, Abundance, Detonation Waves, Galactic Structure, Probability Distribution Functions, Radial Velocity, Supernova Remnants

Scientific paper

Observations of three strong interstellar UV absorption lines of N I (1199 A), N II (1083 A), and Si III (1206 A) in 47 stars of widely varying distance and a variety of spectral types are analyzed to obtain a velocity distribution function for the interstellar gas. A technique based on the maximum and minimum velocities observed along a line of sight is adopted because of heavy line blending, and results are discussed for both power-law and exponential distribution functions. The expected distribution of radiative-phase supernova remnants (SNRs) in the interstellar medium is calculated as a function of SNR birthrate and of the interstellar density in which they evolve. The results are combined with observed distance estimates, and it is shown that an interstellar density in excess of 0.1 per cu cm would be required to keep the SNRs sufficiently confined so that their cross sections are consistent with the observed number of components. The alternative possibility is considered that SNRs do not enter the radiative phase before escaping from the Galaxy or colliding with neighboring remnants.

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