FUSE Observations of the Cygnus Loop: OVI Emission from a Nonradiative Shock

Details FUSE Observations of the Cygnus Loop: OVI Emission from a Nonradiative Shock FUSE Observations of the Cygnus Loop: OVI Emission from a Nonradiative Shock

2001-09-28

arxiv.org/abs/astro-ph/0109556v1

Astronomy and Astrophysics

Astrophysics

LaTeX uses aaspp4.sty, 18 pages + 5 PostScript figures. Accepted for publication in the Astrophysical Journal

Scientific paper

10.1086/324603

We present Far Ultraviolet Spectroscopic Explorer (FUSE) observations of a Balmer filament in the northeast region of the Cygnus Loop supernova remnant. The data consist of one spectrum obtained through the 30"x30" (LWRS) aperture and three spectra at adjacent positions obtained through the 4"x20" (MDRS) aperture. The nonradiative shocks in the region giving rise to these faint optical filaments produce strong OVI 1032,1038 emission, which is detected in all the spectra. The OVI emission is resolved by FUSE into a strong component centered at 0 km/s, and weaker components centered at +/- 140 km/s. The MDRS spectra allow us to study the variation of OVI emission in the post-shock structure. We find that the zero velocity emission is associated directly with the Balmer filament shock, while the high velocity emission comes from a more uniformly distributed component elsewhere along the line of sight. We also find that the shocks producing the emission at +/- 140 km/s have velocities between 180 km/s and 220 km/s, if we assume that the ram pressure driving them is the same as for the zero velocity component shock. In the context of the cavity model for the Cygnus Loop, the interaction of the blast wave with the spherical shell that forms most of the cavity wall can naturally give rise to the similar red and blue-shifted components that are observed.

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