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Title:
Optical and Far-Ultraviolet Spectroscopy of Knot D in the Vela Supernova Remnant
Authors:
Sankrit, Ravi; Blair, William P.; Raymond, John C.
Affiliation:
AA(Johns Hopkins University, Department of Physics and Astronomy, 3400 North Charles Street, Baltimore, MD 21218; , ), AB(Johns Hopkins University, Department of Physics and Astronomy, 3400 North Charles Street, Baltimore, MD 21218; , ), AC(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; )
Publication:
The Astrophysical Journal, Volume 589, Issue 1, pp. 242-252. (ApJ Homepage)
Publication Date:
05/2003
Origin:
UCP
ApJ Keywords:
ISM: Individual: Name: Vela Supernova Remnant, Shock Waves, ISM: Supernova Remnants, Ultraviolet: ISM
DOI:
10.1086/374591
Bibliographic Code:
2003ApJ...589..242S

Abstract

We present spectra of optical filaments associated with the X-ray knot D in the Vela supernova remnant. It has been suggested that knot D is formed by a bullet of supernova ejecta, that it is a breakout of the shock front of the Vela supernova remnant, and also that it is an outflow from the recently discovered remnant RX J0852.0-4622. We find that knot D is a bow shock propagating into an interstellar cloud with normal abundances and typical cloud densities (nH~4-11 cm-3). Optical long-slit spectra show that the [S II] λλ6716, 6731 to Hα line ratio is greater than unity, proving that the optical filaments are shock excited. The analysis of far-ultraviolet spectra obtained with the Hopkins Ultraviolet Telescope and with the Far Ultraviolet Spectroscopic Explorer (FUSE) LWRS aperture show that slower shocks (~100 km s-1) produce most of the low-ionization lines such as O III] λ1662, while faster shocks (~180 km s-1) produce the O VI λλ1032, 1038 and other high-ionization lines. C III and O VI lines are also detected in the FUSE MDRS aperture, which was located on an X-ray-bright region away from the optical filaments. The lines have two velocity components consistent with ~150 km s-1 shocks on the near and far sides of the knot. The driving pressure in the X-ray knot, P/kB~1.8×107 cm-3 K, is derived from the shock properties. This is over an order of magnitude larger than the characteristic X-ray pressure in the Vela supernova remnant. The velocity distribution of the emission and the overpressure support the idea that knot D is a bow shock around a bullet or cloud that originated near the center of the Vela remnant.
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