Calculation of (12)C(16)O and (13)C(16)O X(1)Sigma(+) rovibrational intensities for V less than or equal to 20 and J less than or equal to 150

Goorvitch, D.; Chackerian, C.

doi:10.1086/191945

Cited by 73 publications

(56 citation statements)

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“…The oscillator strength of the R(2) vibration-rotation f uHl CO line at 4.6 km is 6.1 ] 10~6 (Kirby-Docken & Liu 1978 provide oscillator strengths, which for our transitions are consistent with Chackerian 1994 and&Hure Roue † 1996 ;4 see also Table 2). Thus, from equation (1) we Ðnd that the mass-loss rate as deduced from the emitted intensity from the R(2) line of CO, and assuming k B 1.2, is…”

Section: Discussionsupporting

confidence: 71%

Mira’s Wind Explored in Scattering Infrared CO Lines

Ryde¹,

Gustafsson²,

Eriksson³

et al. 2000

ApJ

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We have observed the intermediate regions of the circumstellar envelope of Mira (o Ceti) in photospheric light scattered by three vibration-rotation transitions of the fundamental band of CO, from lowexcited rotational levels of the ground vibrational state, at an angular distance of b D 2@@È7A away from the star. The data were obtained with the Phoenix spectrometer mounted on the 4 m Mayall telescope at Kitt Peak. The spatial resolution is approximately and seeing limited. Our observations provide 0A .5 absolute Ñuxes, leading to an independent new estimate of the mass-loss rate of approximately 3 ] 10~7 yr~1, as derived from a simple analytic wind model. We Ðnd that the scattered intensity from the M _ wind of Mira for decreases as b~3, which suggests a time constant mass-loss rate, when 2@@ [ b [ 7@@ averaged over 100 yr, over the past 1200 yr.

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Section: Discussionsupporting

confidence: 71%

Mira’s Wind Explored in Scattering Infrared CO Lines

Ryde¹,

Gustafsson²,

Eriksson³

et al. 2000

ApJ

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“…For both 12 CO and 13 CO energy levels, transition frequencies and Einstein A coefficients were taken from Goorvitch & Chackerian (1994). Transitions in the ground and first vibrational state were included up to J = 40.…”

Section: Appendix A: Molecular Line Datamentioning

confidence: 99%

“…The SiO linelist of Langhoff & Bauschlicher (1993) was used to extract the frequencies, energy levels and (vibra-)rotational radiative rates for 28 SiO,29 SiO, Goorvitch & Chackerian (1994). and 30 SiO.…”

Section: Appendix A: Molecular Line Datamentioning

confidence: 99%

Circumstellar molecular composition of the oxygen-rich AGB star IK Tauri

Decin

Beck²,

Brünken

et al. 2010

A&A

105

212

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Context. 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 nonequilibrium 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. Aims. 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 ( 12 CO, 13 CO, SiS, 28 SiO, 29 SiO, 30 SiO, HCN, CN, CS, SO, SO 2 ) in the oxygen-rich evolved star IK Tau. Methods. 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. Results. 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 SO 2 lines is cumbersome, possibly related to line misidentifications or problems with the collisional rates.

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“…To get precise estimates of T eff , additional model atmospheres were produced that resulted in a grid spacing of ΔT = 10 K. All the main molecular opacities typical of C-stars were included: CO (Goorvitch & Chackerian 1994), C 2 (Querci et al 1974), HCN (Harris et al 2006), CN (Jørgensen 1997) in the form of line lists, and C 2 H 2 and C 3 (Jorgensen et al 1989) as OS data. CS is not included due to the lack of line lists and OS data.…”

Section: Hydrostatic Modelsmentioning

confidence: 99%

Catching the fish – Constraining stellar parameters for TX Piscium using spectro-interferometric observations

Klotz

Paladini

Hron

et al. 2013

A&A

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Context. Stellar parameter determination is a challenging task when dealing with galactic giant stars. The combination of different investigation techniques has proven to be a promising approach. Aims. We analyse archive spectra obtained with the Short Wavelength Spectrometer (SWS) onboard ISO, and new interferometric observations from the Very Large Telescope MID-infrared Interferometric instrument (VLTI/MIDI) of a very well studied carbon-rich giant: TX Psc. The aim of this work is to determine stellar parameters using spectroscopy and interferometry. Methods. The observations are used to constrain the model atmosphere, and eventually the stellar evolutionary model in the region where the tracks map the beginning of the carbon star sequence. Two different approaches are used to determine stellar parameters: (i) the "classic" interferometric approach where the effective temperature is fixed by using the angular diameter in the N-band (from interferometry) and the apparent bolometric magnitude; (ii) parameters are obtained by fitting a grid of state-of-the-art hydrostatic models to spectroscopic and interferometric observations. Results. We find good agreement between the parameters of the two methods. The effective temperature and luminosity clearly place TX Psc in the carbon-rich AGB star domain in the H-R-diagram. Current evolutionary tracks suggest that TX Psc became a C-star just recently, which means that the star is still in a "quiet" phase compared to the subsequent strong-wind regime. This agrees with the C/O ratio being only slightly greater than one.

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Calculation of (12)C(16)O and (13)C(16)O X(1)Sigma(+) rovibrational intensities for V less than or equal to 20 and J less than or equal to 150

Cited by 73 publications

References 0 publications

Mira’s Wind Explored in Scattering Infrared CO Lines

Mira’s Wind Explored in Scattering Infrared CO Lines

Circumstellar molecular composition of the oxygen-rich AGB star IK Tauri

Catching the fish – Constraining stellar parameters for TX Piscium using spectro-interferometric observations

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