The structure and emission spectrum of a nonradiative shock wave in the Cygnus Loop

Details The structure and emission spectrum of a nonradiative shock wave in the Cygnus Loop The structure and emission spectrum of a nonradiative shock wave in the Cygnus Loop

Dec 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983apj...275..636r&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 275, Dec. 15, 1983, p. 636-644.

Astronomy and Astrophysics

Astrophysics

84

Abundance, Cygnus Constellation, Emission Spectra, Shock Heating, Supernova Remnants, Ultraviolet Spectra, Balmer Series, Coulomb Collisions, H Lines, Ionized Gases, Plasma Equilibrium, Propagation Velocity

Scientific paper

The ultraviolet spectrum of a Balmer-line filament located just outside the main body of optical filaments in the Cygnus Loop confirms the nonradiative shock wave theory for its origin. This theory is extended to include the hydrogen two-photon continuum, and the possibility of slow electron-ion equilibration in the postshock gas is considered. The shock velocity is inferred from the H-alpha profile. Comparison of model calculations with optical and ultraviolet spectra favors Coulomb equilibration behind a 170 km/s shock over models with rapid equilibration due to plasma turbulence. Elemental abundances in the preshock gas are found to be typical of diffuse interstellar clouds. The ram pressure behind the shock is higher than the pressures inferred for bright optical filaments. It is suggested that the bright optical filaments are regions of thermally unstable cooling behind shocks faster than the shock velocities inferred from their optical and ultraviolet spectra.

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