2002/12/06 by You‐Hua Chu, You-Hua Chu, R. A. Gruendl +6
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics (astro-ph) #Astrophysics and Star Formation Studies #FOS: Physical sciences #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0212152
6 pages, 8 figures, to appear in Proceeedings of the Conference "Winds, Bubbles & Explosions", Patzchuaro, Mexico, Honouring J. Dyson. To be published in Rev. Mex. A&A, ed. Jane Arthur
arxiv created 2002/12/06 · openalex publication_date 2002/12/06 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Fast stellar winds can sweep up ambient media and form bubbles. The evolution of a bubble is largely controlled by the content and physical conditions of the shocked fast wind in its interior. This hot gas was not clearly observed until the recent advent of Chandra and XMM-Newton X-ray observatories. To date, diffuse X-ray emission has been unambiguously detected from two circumstellar bubbles blown by WR stars, four planetary nebulae, and two superbubbles blown by young clusters. Model fits to the X-ray spectra show that the circumstellar bubbles are dominated by hot gas with low temperatures (<= 3x106 K), while the interstellar bubbles contain significant fractions of hotter gas (>= 5x106 K). In all cases, large discrepancies in the X-ray luminosity are found between observations and conventional models of bubbles. Future theoretical models of bubbles need to re-examine the validity of heat conduction and take into account realistic microscopic processes such as mass loading from dense clumps/knots and turbulent mixing. Chandra ACIS-S observation of NGC 6888 will shed light on these astrophysical processes.