2007/06/28 by Y. Libert, E. Gérard, E. Gerard +1 · 2 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2007.12154.x
Accepted for publication in Monthly Notices of the Royal Astronomical Society
arxiv created 2007/06/28 · openalex publication_date 2007/09/10 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28
Y CVn is a carbon star surrounded by a detached dust shell that has been imaged by the Infrared Space Observatory at 90 μm. With the Nançay Radio Telescope, we have studied the gaseous counterpart in the 21-cm H i emission line. New data have been acquired and allow to improve the signal-to-noise ratio on this line. The high spectral resolution line profiles obtained at the position of the star and at several offset positions set strong constraints on the gas temperature and kinematics within the detached shell; the bulk of the material should be at ∼100–200 K and in expansion at ∼1−2 km s−1. In addition, the line profile at the central position shows a quasi-rectangular pedestal that traces an 8 km s−1 outflow of ∼1.0 × 10−7 M⊙ yr−1, stable for about 2 × 104 yr, which corresponds to the central outflow already studied with CO rotational lines. We present a model in which the detached shell results from the slowing down of the stellar wind by surrounding matter. The inner radius corresponds to the location where the stellar outflow is abruptly slowed down from ∼8 to 2 km s−1 (termination shock). The outer radius corresponds to the location where external matter is compressed by the expanding shell (bow shock). In this model, the mass-loss rate of Y CVn has been set constant, at the same level of 1.0 × 10−7 M⊙ yr−1, for ∼4.5 × 105 yr. The gas temperature varies from ∼1800 K at the inner limit to 165 K at the interface between circumstellar matter and external matter. Our modelling shows that the presence of a detached shell around an asymptotic giant branch star may not mean that a drastic reduction of the mass-loss rate has occurred in the past. The inner radius of such a shell might only be the effect of a termination shock rather than of an interruption of the mass-loss process.