Modelling the atmosphere of the carbon-rich Mira RU Virginis

Rau, Gioia; Paladini, C.; Hron, J.; Aringer, B.; Groenewegen, M. A. T.; Nowotny, W.

doi:10.1051/0004-6361/201526418

Cited by 18 publications

(25 citation statements)

References 54 publications

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“…6.1.1. The model SED shows an emission bump around 14 µm, which is not seen in the observed spectrum, as also noticed by Rau et al (2015). The origin of this feature predicted by the model, is due to C 2 H 2 and HCN, as mentioned by Loidl (2001), and discussed in Sect 6.1.2.…”

Section: Mira Starssupporting

confidence: 69%

“…A detailed description of the modeling approach can be found in Höfner & Dorfi (1997), Höfner (1999), Höfner et al (2003), and Höfner et al (2016). Applications to observations are described in Loidl et al (1999), Gautschy-Loidl et al (2004), Nowotny et al (2010), Nowotny et al (2011), Sacuto et al (2011), and Rau et al (2015.…”

Section: Overview Of the Darwin Modelsmentioning

confidence: 99%

“…SiC is added artificially a posteriori with COMA. Following Rau et al (2015) and Sacuto et al (2011), the percentage of condensed material is distributed as follows: 90% amorphous carbon, using data from Rouleau & Martin (1991), and 10% silicon carbide, based on Pegourie (1988). Some experiments that change this configuration are presented in Sect.…”

Section: Overview Of the Darwin Modelsmentioning

confidence: 99%

“…In our previous work (Rau et al 2015), we studied the atmosphere of the C-rich AGB star RU Vir, comparing, in a systematic way, spectroscopic-, photometric-and interferometric data with the grid of DARWIN models from Mattsson et al (2010) and Eriksson et al (2014) .…”

Section: Introductionmentioning

confidence: 99%

“…From those, only very few have made use of time-dependent self-consistent dynamic models (Sacuto et al 2011;Rau et al 2015). As suggested by Höfner et al (2003), this is the only way to acquire knowledge about the influence of the dynamic processes on the atmospheric structure at different spatial scales.…”

Section: Introductionmentioning

confidence: 99%

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The adventure of carbon stars

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Paladini

et al. 2017

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Context. Modeling stellar atmospheres is a complex and intriguing task in modern astronomy. A systematic comparison of models with multi-technique observations is the only efficient way to constrain the models. Aims. We intend to perform self-consistent modeling of the atmospheres of six carbon-rich AGB stars (R Lep, R Vol, Y Pav, AQ Sgr, U Hya, and X TrA) with the aim of enlarging the knowledge of the dynamic processes occurring in their atmospheres. Methods. We used VLTI/MIDI interferometric observations, in combination with spectro-photometric data, and compared them with self-consistent, dynamic model atmospheres. Results. We found that the models can reproduce spectral energy distribution (SED) data well at wavelengths longer than 1 µm, and the interferometric observations between 8 µm and 10 µm. Discrepancies observed at wavelengths shorter than 1 µm in the SED, and longer than 10 µm in the visibilities, could be due to a combination of data-and model-related effects. The models best fitting the Miras are significantly extended, and have a prominent shell-like structure. On the contrary, the models best fitting the non-Miras are more compact, showing lower average mass loss. The mass loss is of episodic or multi-periodic nature but causes the visual amplitudes to be notably larger than the observed ones. A number of stellar parameters were derived from the model fitting: T Ross , L Ross , M, C/O, andṀ. Our findings agree well with literature values within the uncertainties. T Ross , and L Ross are also in good agreement with the temperature derived from the angular diameter T (θ (V−K) ) and the bolometric luminosity from the SED fitting L bol , except for AQ Sgr. The possible reasons are discussed in the text. Finally, θ Ross and θ (V−K) agree with one another better for the Miras than for the nonMiras targets, which is probably connected to the episodic nature of the latter models. We also located the stars in the H-R diagram, comparing them with evolutionary tracks. We found that the main derived properties (L, T eff , C/O ratios and stellar masses) from the model fitting are in good agreement with TP-AGB evolutionary calculations for carbon stars carried out with the COLIBRI code.

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Section: Mira Starssupporting

confidence: 69%

Section: Overview Of the Darwin Modelsmentioning

confidence: 99%

Section: Overview Of the Darwin Modelsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The adventure of carbon stars

Rau

Hron

Paladini

et al. 2017

A&A

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The Carbon Stars Adventure

et al. 2015

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We compare in a systematic way spectrometric, photometric and mid-infrared (VLTI/MIDI) interferometric measurements with different types of model atmospheres. Self-consistent dynamic model atmospheres in particular were used to interpret in a consistent way the dynamic behavior of gas and dust. The results underline how the joint use of different kind of observations, as photometry, spectroscopy and interferometry, is essential to understand the atmospheres of pulsating C-rich AGB stars. The sample of C-rich stars discussed in this work provides crucial constraints for the atmospheric structure.

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