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A Detailed Analysis of the Dust Formation Zone of IRC+10216 Derived from Mid-Infrared Bands of C2H2 and HCN

AutorFonfría, José Pablo ; Cernicharo, José ; Richter, Matthew J.; Lacy, John H.
Palabras claveline: identification
line: profiles
stars: AGB and post-AGB
stars: carbon
stars: individual(IRC+10216)
Fecha de publicación20-ene-2008
EditorAmerican Astronomical Society
CitaciónFonfría et al., 2008, ApJ, 673, 445
ResumenA spectral survey of IRC+10216 has been carried out in the range 11 to 14 um with a spectral resolution of about 4 km/s. We have identified a forest of lines in six bands of C2H2 involving the vibrational states from the ground to 3nu5 and in two bands of HCN, involving the vibrational states from the ground up to 2nu2. Some of these transitions are observed also in H13CCH and H13CN. We have estimated the kinetic, vibrational, and rotational temperatures, and the abundances and column densities of C2H2 and HCN between 1 and 300 R* (~ 1.5x10^16 cm) by fitting about 300 of these ro-vibrational lines. The envelope can be divided into three regions with approximate boundaries at 0.019" (the stellar photosphere), 0.1" (the inner dust formation zone), and 0.4" (outer dust formation zone). Most of the lines might require a large microturbulence broadening. The derived abundances of C2H2 and HCN increase by factors of 10 and 4, respectively, from the innermost envelope outwards. The derived column densities for both C2H2 and HCN are ~ 1.6x10^19 cm^-2. Vibrational states up to 3000 K above ground are populated, suggesting pumping by near-infrared radiation from the star and innermost envelope. Low rotational levels can be considered under LTE while those with J>20-30 are not thermalized. A few lines require special analysis to deal with effects like overlap with lines of other molecules.
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