2004/07/16 by Yue Shen, Yu-Qing Lou · 5 citations
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/424006
published as Astrophys.J. 611 (2004) L117-L120 · ApJL accepted
arxiv created 2004/07/16 · openalex publication_date 2004/07/26 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/31
We propose self-similar shocked flow models for certain dynamical evolution phases of young stellar objects, "champagne flows" of H II regions surrounding OB stars, and shaping processes of planetary nebulae. We analyze an isothermal fluid of spherical symmetry and construct families of self-similar shocked flow solutions that feature (1) either a core expansion with a finite central density or a core accretion at a constant rate with a density scaling proportional to r -3/2 (a free-fall state); (2) a shock moving outward at a constant speed (a wind, a breeze, or an accretion flow); and (3) a preshock gas approaching a constant speed at large r with a density scaling proportional to r -2 . In addition to testing numerical codes, our models can accommodate diverse shocked flows with or without a core collapse or outflow and with or without an envelope expansion or contraction. As an application, we introduce our model analysis to observations of Bok globule B335.