X-rays from superbubbles in the large magellanic cloud. IV. The blowout structure of N44

Eugene A. Magnier, You Hua Chu, Sean D. Points, Una Hwang, R. Chris Smith

Research output: Contribution to journalArticlepeer-review

Abstract

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).

Original languageEnglish (US)
Pages (from-to)829-835
Number of pages7
JournalAstrophysical Journal
Volume464
Issue number2 PART I
DOIs
StatePublished - 1996

Keywords

  • H II regions
  • ISM: bubbles
  • ISM: individual (LMC N44)
  • ISM: jets and outflows
  • Magellanic Clouds
  • X-rays: ISM

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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