2010/03/30 by N. Crimier, Nicolas Crimier, C. Ceccarelli +13 · 86 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysics and Star Formation Studies #Envelope (radar) #Millimeter #Molecular cloud #Protostar #Star formation #Stellar, planetary, and galactic studies #Type (biology) #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/200913112
published in Astronomy and Astrophysics 519, A65 (EDP Sciences)
arxiv created 2010/03/30 · openalex publication_date 2010/05/05 · arxiv updated 2015/05/18 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
<i>Context. <i/>The low mass protostar IRAS16293-2422 is a prototype Class 0 source in studies of the chemical structure during the initial phases of life of solar type stars.<i>Aims. <i/>To derive the chemical structure accurately, a precise determination of the source physical structure is required. The goal of this study is to derive the structure of IRAS16293-2422.<i>Methods. <i/>We reanalyzed all available continuum data (single dish and interferometric, from millimeter to MIR) to derive accurate density and dust temperature profiles. Using ISO observations of water, we also reconstructed the gas temperature profile.<i>Results. <i/>Our analysis shows that the envelope surrounding IRAS16293-2422 is described well by the Shu “inside-out” collapsing envelope model or a single power-law density profile with index equal to 1.8. In contrast to some previous studies, our analysis does not show evidence of a large (<i>≥<i/><i>800<i/> AU in diameter) cavity.<i>Conclusions. <i/>Although IRAS16293-2422 is a multiple system composed of two or three objects, our reconstruction will be useful in deriving the chemical structure of the large cold envelope surrounding these objects and the warm component, treated here as a single source, from single-dish observations of molecular emission.