2010A&A...516A..69D


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST16:59:45

2010A&A...516A..69D - Astronomy and Astrophysics, volume 516, A69-69 (2010/6-2)

Circumstellar molecular composition of the oxygen-rich AGB star IK Tauri. II. In-depth non-LTE chemical abundance analysis.

DECIN L., DE BECK E., BRUENKEN S., MUELLER H.S.P., MENTEN K.M., KIM H., WILLACY K., DE KOTER A. and WYROWSKI F.

Abstract (from CDS):

The interstellar medium is enriched primarily by matter ejected from evolved low and intermediate mass stars. The outflow from these stars creates a circumstellar envelope in which a rich gas-phase chemistry takes place. Complex shock-induced non-equilibrium chemistry takes place in the inner wind envelope, dust-gas reactions and ion-molecule reactions alter the abundances in the intermediate wind zone, and the penetration of cosmic rays and ultraviolet photons dissociates the molecules in the outer wind region. Little observational information exists on the circumstellar molecular abundance stratifications of many molecules. Furthermore, our knowledge of oxygen-rich envelopes is not as profound as for the carbon-rich counterparts. The aim of this paper is therefore to study the circumstellar chemical abundance pattern of 11 molecules and isotopologs (12CO, 13CO, SiS, 28SiO, 29SiO, 30SiO, HCN, CN, CS, SO, SO2) in the oxygen-rich evolved star IK Tau. We have performed an in-depth analysis of a large number of molecular emission lines excited in the circumstellar envelope around IK Tau. The analysis is done based on a non-local thermodynamic equilibrium (non-LTE) radiative transfer analysis, which calculates the temperature and velocity structure in a self-consistent way. The chemical abundance pattern is coupled to theoretical outer wind model predictions including photodestruction and cosmic ray ionization. Not only the integrated line intensities, but also the line shapes are used as diagnostic tool to study the envelope structure. The deduced wind acceleration is much slower than predicted from classical theories. SiO and SiS are depleted in the envelope, possibly due to the adsorption onto dust grains. For HCN and CS a clear difference with respect to inner wind non-equilibrium predictions is found, either indicating uncertainties in the inner wind theoretical modeling or the possibility that HCN and CS (or the radical CN) participate in the dust formation. The low signal-to-noise profiles of SO and CN prohibit an accurate abundance determination; the modeling of high-excitation SO2 lines is cumbersome, possibly related to line misidentifications or problems with the collisional rates. The SiO isotopic ratios (29SiO/28SiO and 30SiO/28SiO) point toward an enhancement in 28SiO compared to results of classical stellar evolution codes. Predictions for H2O emission lines in the spectral range of the Herschel/HIFI mission are performed.

Abstract Copyright:

Journal keyword(s): astrochemistry - molecular processes - radiative transfer - submillimeter: stars - stars: AGB and post-AGB - stars: mass-loss

Simbad objects: 12

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Number of rows : 12

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 V* BD Cam Sy* 03 42 09.3284345030 +63 13 00.463126693 8.56 6.74 5.11 3.49 2.11 S3.5/2 197 0
2 V* IK Tau Mi* 03 53 28.8884898148 +11 24 21.865959095 16.99 17.03 13.39 7.29 3.20 M7-11 570 0
3 * omi Ori S* 04 52 31.9660398278 +14 15 02.326990690   6.458 4.721     M3SIII 203 0
4 V* TX Cam Mi* 05 00 51.1569959503 +56 10 54.093107078       14.02   M9-9.5 328 0
5 IRC +50137 Mi* 05 11 19.4489549676 +52 52 33.222548186           M10 169 0
6 V* VY CMa s*r 07 22 58.32877 -25 46 03.2355 12.01 10.19 7.95     M5Iae 996 0
7 IRC +10216 C* 09 47 57.40632 +13 16 43.5648     10.96     C9,5e 2134 0
8 * i Dra LP? 13 51 25.9393781 +64 43 23.772696 8.12 6.23 4.66 3.05 1.69 M3.5III 110 0
9 IRC +10365 Mi* 18 37 19.2595666948 +10 25 42.492197977           M9 133 0
10 * chi Cyg S* 19 50 33.9243904 +32 54 50.609683 7.02 6.06 4.24 1.81 -0.01 S6-9/1-2e 663 0
11 * bet Peg LP* 23 03 46.45746 +28 04 58.0336 6.05 4.09 2.42 0.92 -0.40 M2.5II-III 579 0
12 V* R Cas Mi* 23 58 24.8700291935 +51 23 19.691977266 6.71 6.63 4.80     M6.5-9e 677 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-16:59:45

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