Spectroscopy of a Balmer-dominated filament in the Cygnus Loop with the Hopkins Ultraviolet Telescope

Details Spectroscopy of a Balmer-dominated filament in the Cygnus Loop with the Hopkins Ultraviolet Telescope Spectroscopy of a Balmer-dominated filament in the Cygnus Loop with the Hopkins Ultraviolet Telescope

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...400..214l&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 400, no. 1, p. 214-221.

Astronomy and Astrophysics

Astronomy

49

Balmer Series, Cygnus Constellation, Interstellar Matter, Supernova Remnants, Ultraviolet Spectroscopy, Space Shuttles, Spaceborne Astronomy, Ultraviolet Telescopes

Scientific paper

A fair UV spectrum of a nonradiative filament in the Cygnus Loop covering the wavelength range 830-1860 A at 3.5-A resolution was obtained using the Hopkins Ultraviolet Telescope (HUT) on the Astro-1 space shuttle mission. Nonradiative shock models which include a more sophisticated treatment of Lyman line transfer are calculated. It is found that the HUT spectrum can be explained in terms of a shock with velocity 175-185 km/s propagating into a low-density medium. This shock velocity can be reconciled with the 135-km/s width of the broad component of H-alpha in this filament if equilibration of the postshock electron and ion temperatures proceeds much more rapidly than Coulomb equilibration time scales. The time required for a 180-km/s shock to develop a partial recombination zone is short, about 200 yr if n is approximately equal to 2/cu cm. This suggests that the shock is decelerating as it encounters denser material. The current analysis patently favors rapid equilibration of electrons and ions behind the shock.

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