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OPTICAL AND FAR-ULTRAVIOLET SPECTROSCOPY OF KNOT D IN THE VELA SUPERNOVA REMNANT
 

Summary: OPTICAL AND FAR-ULTRAVIOLET SPECTROSCOPY OF KNOT D IN THE VELA
SUPERNOVA REMNANT
Ravi Sankrit and William P. Blair
Johns Hopkins University, Department of Physics and Astronomy, 3400 North Charles Street, Baltimore, MD 21218;
ravi@pha.jhu.edu, wpb@pha.jhu.edu
and
John C. Raymond
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138; jraymond@cfa.harvard.edu
Received 2002 July 29; accepted 2003 January 31
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 J0852.04622. We find that knot D is a bow shock propagating into an interstellar cloud with normal
abundances and typical cloud densities (nH $ 4 11 cm3). Optical long-slit spectra show that the [S ii]
6716, 6731 to H 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 Ultravio-
let Spectroscopic Explorer (FUSE) LWRS aperture show that slower shocks ($100 km s1) produce most of
the low-ionization lines such as O iii] 1662, while faster shocks ($180 km s1) produce the O vi 1032,
1038 and other high-ionization lines. C iii and O vi lines are also detected in the FUSE MDRS aperture,

  

Source: Henry, Richard C.- Department of Physics and Astronomy, Johns Hopkins University

 

Collections: Physics