2006/07/21 by C. J. Wareing, Albert A. Zijlstra, A. A. Zijlstra +16
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Asymptotic giant branch #Bow shock (aerodynamics) #Galaxy #Gamma-ray bursts and supernovae #Heliosphere #Interstellar medium #Mechanics #Molecular cloud #Physics #Plasma #Shock wave #Solar wind #Star formation #Stars #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1111/j.1745-3933.2006.00227.x
published as Mon.Not.Roy.Astron.Soc.Lett. 372 (2006) L63-L67 · 5 pages, 3 colour figures, submitted to MNRAS letters, revised version after referee's comments
arxiv created 2006/07/21 · openalex publication_date 2006/09/05 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Abstract New Spitzer imaging observations have revealed the structure around the Mira variable star R Hya to be a one-sided parabolic arc 100 arcsec to the west, stretching from north to south. We successfully model R Hya and its surroundings in terms of an interaction of the stellar wind from an asymptotic giant branch (AGB) star with the interstellar medium (ISM) the star moves through. Our three-dimensional hydrodynamic simulation reproduces the structure as a bow shock into the oncoming ISM. We propose this as another explanation of detached shells around such stars, which should be considered alongside current theories of internal origin. The simulation predicts the existence of a tail of ram-pressure-stripped AGB material stretching downstream. Indications for such a tail behind R Hya are seen in IRAS maps.