1996/06/01 by E. A. Magnier, Eugene A. Magnier, You‐Hua Chu +5 · 2 citations
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Solar and Space Plasma Dynamics #astro-ph
paper · pdf · doi:10.1086/177368
published as ApJ 464, 829 · 15 pages, LaTeX + psfig, 1 tex file, 2 sty files, 7 PS files, also available at: http://www.astro.washington.edu/gene/papers/papers.html
openalex publication_date 1996/06/01 · arxiv created 1996/06/13 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We have used optical echelle spectra along with ROSAT and ASCA X-ray spectra to test the hypothesis that the southern portion of the N44 X-ray bright region is the result of a blowout structure. Three pieces of evidence now support this conclusion. First, the filamentary optical morphology corresponding with the location of the X-ray bright South Bar suggests the blowout description (Chu et al. 1993). Second, optical echelle spectra show evidence of high-velocity (90 km s-1^) gas in the region of the blowout. Third, X-ray spectral fits show a lower temperature for the South Bar than the main superbubble region of shell 1. Such a blowout can affect the evolution of the superbubble and explain some of the discrepancy discussed by Oey & Massey (1995) between the observed shell diameter and the diameter predicted on the basis of the stellar content and the pressure-driven bubble model of Weaver et al. (1977).