2002
DOI: 10.1051/0004-6361:20020833
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Probing the mass loss history of carbon stars using CO line and dust continuum emission

Abstract: Abstract. An extensive modelling of CO line emission from the circumstellar envelopes around a number of carbon stars is performed. By combining radio observations and infrared observations obtained by ISO the circumstellar envelope characteristics are probed over a large radial range. In the radiative transfer analysis the observational data are consistently reproduced assuming a spherically symmetric and smooth wind expanding at a constant velocity. The combined data set gives better determined envelope para… Show more

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Cited by 58 publications
(74 citation statements)
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“…According to that, if the radio continuum emission detected is generated by a jet-driven wind, the mass-loss rate derived would be only a reliable upper limit of the ionized gas in the high-velocity outflow. During the AGB phase, the mass-loss rates estimated from observations are typically in the range between 10 −8 M yr −1 -10 −4 M yr −1 , with average expansion velocity of v exp ∼ 15 km s −1 (e.g Schöier et al 2002;Ramstedt et al 2008). It is thought that such high mass-loss rates decrease to its minima due to the exhaustion of the Hydrogen stellar atmosphere, once its mass is ≈ 10 −2 M (Habing & Olofsson 2003).…”
Section: Velocity Field and Mass-loss Ratesmentioning
confidence: 99%
“…According to that, if the radio continuum emission detected is generated by a jet-driven wind, the mass-loss rate derived would be only a reliable upper limit of the ionized gas in the high-velocity outflow. During the AGB phase, the mass-loss rates estimated from observations are typically in the range between 10 −8 M yr −1 -10 −4 M yr −1 , with average expansion velocity of v exp ∼ 15 km s −1 (e.g Schöier et al 2002;Ramstedt et al 2008). It is thought that such high mass-loss rates decrease to its minima due to the exhaustion of the Hydrogen stellar atmosphere, once its mass is ≈ 10 −2 M (Habing & Olofsson 2003).…”
Section: Velocity Field and Mass-loss Ratesmentioning
confidence: 99%
“…In addition, the dust temperature structure is calculated self-consistently. The modelling procedure is described in more detail in Schöier et al (2002) and Ramstedt et al (2008). For χ Cyg the dust condensation temperature is only constrained to ≤1300 K and we adopt a characteristic value of 900 K where the dust condensation is assumed to be essentially complete.…”
Section: Dust Radiative Transfer and Dynamical Modellingmentioning
confidence: 99%
“…These objects have for some time now been considered as possible transition objects from M-type (O-rich) AGB stars (C/O < 1) to carbon (C-rich) stars (C/O >1), and are as such particularly interesting to study from a chemical point of view. However, there is a lack of observational data (in part due to their low relative number compared to the two other chemical types) A&A 530, A83 (2011) A combined modelling of CO rotational lines in the farinfrared (from J = 14 → 13 up to J = 37 → 36 observed using the ISO satellite) and in the mm and sub-mm bands (from J = 1 → 0 up to J = 4 → 3 observed using ground-based instruments) of extreme carbon stars was performed by Ryde et al (1999) and Schöier et al (2002). The various excitation conditions of the observed lines allow the circumstellar envelope (CSE) characteristics to be probed over a large radial range.…”
Section: Introductionmentioning
confidence: 99%
“…Being a simple diatomic molecule with a well understood energy diagram, CO has been successfully used to study the structure of the CSEs around evolved stars (e.g., Schöier et al 2002;Decin et al 2006). Different transitions can be used to investigate different regions of the envelope, probing the density, the temperature, and the velocity of the CSE.…”
Section: Thermodynamical Structure Of the Envelopementioning
confidence: 99%