The envelope lost by the central star is 3 and the dust-to-gas
#Irc 368 Pc
Photosphere up to a distance of 3 pc from the star. Material making up the dense core, then just 15 years ago theĭust exists in the envelope of IRC + 10216 everywhere from the stellar If the envelope's outflow velocity of 15 km s -1 applies to the Observed bipolar appearance of the object on a subarcsecond scale. Tilted toward us by 40° from the plane of sky, causing the
#Irc 368 full
Southern cavity with a full opening angle of 36° is With outflow cavities at position angle PA 20°. There is a dense non-spherical dust shell around the star, The object changes its luminosity between 13 0, itsĮffective temperature between 28 K, and its radius between 500Īnd 390. Speckle-interferometry images, and visibilities in, andįor the adopted distance of 130 pc, the model of IRC + 10216 implies that Intensity profiles of the object at 1.25, 2.2, 10.5, 50, 100 m,Īnd 1.3 mm, a 10.5 m lunar occultation intensity profile, our Wavelengths (at several phases of stellar luminosity), observed Spectral energy distribution of IRC + 10216 from optical to centimeter The model reproduces very well the entire beam-matched Our goal was to find a self-consistent model of the star and itsĮnvelope which takes into account as many observational constraints as Model of the dusty envelope around the carbon star IRC + 10216. Men'shchikov, present the first detailed, two-dimensional radiative transfer Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany e-mail: Astrophysical Observatory, Nizhnij Arkhyz, 357147 Karachaevo-Cherkesia, Russia e-mail: author: A.
Stockholm Observatory, 133 36 Saltsjöbaden, Sweden
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