Astronomy and Astrophysics – Astronomy
Scientific paper
May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004apj...606..900s&link_type=abstract
The Astrophysical Journal, Volume 606, Issue 2, pp. 900-910.
Astronomy and Astrophysics
Astronomy
7
Ism: Individual: Name: Vela Supernova Remnant, Shock Waves, Ism: Supernova Remnants, Ultraviolet: Ism
Scientific paper
We present Far Ultraviolet Spectroscopic Explorer (FUSE) data on O VI absorption lines observed toward nine stars behind the Vela supernova remnant (SNR). The O VI observations are compared with International Ultraviolet Explorer (IUE) observations of C IV absorption toward the same stars. All of these stars are B stars, which generally have complex continua, making the extraction of absorption lines difficult. However, four of the stars, HD 72088, HD 72089, HD 72350, and HD 72537, are rapid rotators (vsini>~150 km s-1), making the derivation of absorption column densities much easier. We present O VI and C IV column densities for the ``main component'' (i.e., the low-velocity component) for these stars. In the FUSE spectra of three of the rapid rotators (HD 72088, HD 72089, and HD 72537) we find high-velocity components of O VI at ~150 km s-1 that we attribute to the SNR shock. HD 72350 has very strong H2 absorption, which obscures any possible high-velocity O VI absorption. To detect the high-velocity O VI absorption in HD 72088 requires employing a technique for removing the H2 line at 1032.35 Å (121.6 km s-1 relative to O VI). The O VI data are consistent with steady radiative shock models with vs~150 km s-1, but we do not detect C IV at the same velocities. Instead we find high-velocity C IV at lower velocities (~100 km s-1). We discuss the implications of our results for models of the evolution of the Vela SNR.
Blair William Patrick
Nichols Joy S.
Slavin Jonathan D.
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