Stellar turbulent convection - A new model and applications

Canuto, V.; Mazzitelli, I.

doi:10.1086/169815

Cited by 544 publications

(451 citation statements)

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“…Convection has been treated according to the Full Spectrum of Turbulence model (Canuto & Mazzitelli 1991). We used the opacity tables from the OPAL website , and for the low temperature opacities we followed Ferguson et al (2005).…”

Section: Evolutionary Modelsmentioning

confidence: 99%

The mosaic multiple stellar populations in ω Centauri: the horizontal branch and the main sequence

Tailo

Criscienzo

D’Antona

et al. 2016

Mon. Not. R. Astron. Soc.

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We interpret the stellar population of ω Centauri by means of a population synthesis analysis, following the most recent observational guidelines for input metallicities, helium and [(C+N+O)/Fe] contents. We deal at the same time with the main sequences, sub-giant and horizontal branch data. The reproduction of the observed color magnitude features is very satisfying and bears interesting hints concerning the evolutionary history of this peculiar stellar ensemble. Our main results are: 1) no significant spread in age is required to fit the colour-magnitude diagram. Indeed we can use coeval isochrones for the synthetic populations, and we estimate that the ages fall within a ∼ 0.5 Gyr time interval; in particular the most metal rich population can be coeval (in the above meaning) with the others, if its stars are very helium-rich (Y∼0.37) and with the observed CNO enhancement ([(C+N+O)/Fe] = + 0.7); 2) a satisfactory fit of the whole HB is obtained, consistent with the choice of the populations providing a good reproduction of the main sequence and sub giant data. 3) the split in magnitude observed in the red HB is well reproduced assuming the presence of two stellar populations in the two different sequences observed: a metal poor population made of stars evolving from the blue side (luminous branch) and a metal richer one whose stars are in a stage closer to the zero age HB (dimmer branch). This modelization also fits satisfactorily the period and the [Fe/H] distribution of the RR Lyrae stars.

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Section: Evolutionary Modelsmentioning

confidence: 99%

The mosaic multiple stellar populations in ω Centauri: the horizontal branch and the main sequence

Tailo

Criscienzo

D’Antona

et al. 2016

Mon. Not. R. Astron. Soc.

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“…The OPAL equation of state (Rogers, Swenson & Iglesias 1996) was used to construct the model and convective flux was calculated using the the formulation of Canuto and Mazzitelli (1991). The radius of the model is 695.78 Mm (Antia 1998).…”

Section: Resultsmentioning

confidence: 99%

Solar Cycle Variation in Solar F-Mode Frequencies and Radius

Antia

Basu

Pintar

et al. 2000

Helioseismic Diagnostics of Solar Convection and Activity

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Abstract. Using data from the Global Oscillation Network Group (GONG) covering the period from 1995 to 1998, we study the change with solar activity in solar f-mode frequencies. The results are compared with similar changes detected from the Michelson Doppler Imager (MDI) data. We find variations in f-mode frequencies which are correlated with solar activity indices. If these changes are due to variation in solar radius then the implications are that the solar radius decreases by about 5 km from minimum to maximum activity.

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“…Colour changes also occur, being the object redder when fainter. The photometric changes have spectacular spectroscopic fallout: molecular and atomic lines develop in emission during the fading to turn back in absorption when the star recovers the bright state (Whitelock et al 2006;Clayton 1996).…”

Section: Introductionmentioning

confidence: 99%

“…Feast et al 1997;Clayton 1996). The advent of several infrared satellites improved the wavelength coverage of the energy distribution and stimulated the use of mid infrared colour-colour diagrams to select new candidates, (Tisserand 2012;Tisserand et al 2013;Miller et al 2012;Lee 2015).…”

Section: Introductionmentioning

confidence: 99%

The variable V381 Lac and its possible connection with the R CrB phenomenon

Rossi¹,

Dell’Agli²,

Paola³

et al. 2015

Mon. Not. R. Astron. Soc.

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We have performed new medium resolution spectroscopy, optical and near infrared photometry to monitor the variability of the AGB carbon star V 381 Lac. Our observations revealed rapid and deep changes in the spectrum and extreme variability in the optical and near infrared bands. Most notably we observed the change of NaI D lines from deep absorption to emission, and the progressive growing of the [N ii] doublet 6548-6584Å emission, strongly related to the simultaneous photometric fading. V381 Lac occupies regions of 2MASS and WISE colour-colour diagrams typical of stars with dust formation in the envelope. The general framework emerging from the observations of V381 Lac is that of a cool AGB carbon star undergoing episodes of high mass ejection and severe occultation of the stellar photosphere reminiscent of those characterising the RCB phenomenon.Comparing the Spectral Energy Distribution obtained with the theoretical model for AGB evolution with dust in the circumstellar envelope, we can identify V381 Lac as the descendant of a star of initial mass ∼2M , in the final AGB phases, evolved into a carbon star by repeated Third Dredge Up episodes. According to our model the star is moderately obscured (τ 10 ∼ 0.22) by dust, mainly formed by amorphous carbon (∼ 80%) and SiC (∼ 20%), with dust grain dimensions around ∼ 0.2µm and 0.08µm respectively.

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Stellar turbulent convection - A new model and applications

Cited by 544 publications

References 0 publications

The mosaic multiple stellar populations in ω Centauri: the horizontal branch and the main sequence

The mosaic multiple stellar populations in ω Centauri: the horizontal branch and the main sequence

Solar Cycle Variation in Solar F-Mode Frequencies and Radius

The variable V381 Lac and its possible connection with the R CrB phenomenon

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