data:models
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| + | ======= Models ======== | ||
| + | The table below organises the data used in each exercise. Data consists in packages compresses with .tar.gz or zip, which can be downloaded by clicking on the provided links. | ||
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| + | ===== Exercise #1: Model-S models ====== | ||
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| + | ^Package ^Date ^Author ^Description | ||
| + | ^wp121130_ex0-smodels|21/ | ||
| + | ^wp121130_ex0-omodels|21/ | ||
| + | ^Physics|||||| | ||
| + | ^Code | ASTEC (ongoing updates)||||| | ||
| + | ^Convection| Boehm-Vitense 1958 MLT, solar calibrated (alpha = 2.08984)||||| | ||
| + | ^Overshoot | None, for now ||||| | ||
| + | ^Extra mixing | None, for now||||| | ||
| + | ^gradT | N/A, for now||||| | ||
| + | ^Wind | None ||||| | ||
| + | ^Atmosphere | Fit to VAL C atmosphere ||||| | ||
| + | ^Nuclear rates | Adelberger et al. 2011, which includes de " | ||
| + | ^Screening | Weak (Salpeter) ||||| | ||
| + | ^EOS |Default: OPAL 2005 / Models _ceff_: CEFF ||||| | ||
| + | ^Opacities | OPAL + Ferguson 2005 for low temperatures ||||| | ||
| + | ^mDiffusion | Models _zdif_: He and heavy elements modelled as oxygen ||||| | ||
| + | ^rLevitation | No ||||| | ||
| + | ^Relevant constants|||||| | ||
| + | ^G | 6.67232e-8 (cgs) ||||| | ||
| + | ^References | [[https:// | ||
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| + | ---- | ||
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| + | ===== Exercise #0: Garstec models ====== | ||
| + | |||
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| + | ^Package ^Date ^Author ^Description | ||
| + | ^wp121130_ex0-smodels|21/ | ||
| + | ^wp121130_ex0-omodels|21/ | ||
| + | ^Physics|||||| | ||
| + | ^Code | Garstec (A- Wess rev., 2015)||||| | ||
| + | ^Convection| MLT, alpha = 1.801||||| | ||
| + | ^Overshoot | diffusion equation with exponential decay (Herwig type), including geometric limit applied to small convective cores (H_p towards the center makes overshoot regions too large). Proportion factor f = 0.02 (equivalent to 0.2 - 0.25 Hp in tradicional formulation) ||||| | ||
| + | ^Extra mixing | Under the convective envelope (Vandenberg et al. 2012) as a function of its mass. Free parameters calibration forced to reproduce the solar Li and chemical abundances observed in globular clusters (e.g. Korn et al. en NGC 6397).||||| | ||
| + | ^gradT | Temperature gradient in overshoot regions is radiative.||||| | ||
| + | ^Wind | 1e-13 Msun / yr to avoid depletion of He and metals (included in extra missing calibration) ||||| | ||
| + | ^Atmosphere | Eddington T-tau ||||| | ||
| + | ^Nuclear rates | Adelberger et al. 2011, which includes de " | ||
| + | ^Screening | Weak (Salpeter)/ | ||
| + | ^EOS |FreeEOS de Irwin ||||| | ||
| + | ^Opacities | OPAL + Ferguson 2005 for low temperatures ||||| | ||
| + | ^mDiffusion | For all chemical elements ||||| | ||
| + | ^rLevitation | No ||||| | ||
| + | ^Relevant constants|||||| | ||
| + | ^G | 6.67232e-8 (c.g.s.) ||||| | ||
| + | |||
| + | ^<color # | ||
| + | ^Model ^Mass ^[Fe/H] ^alpha | ||
| + | |0-001 |1.04 | +0.05 | 1.6 | 0.00 |3000 | MS | Representative of 16Cyg ~7Gyr (Travis et al. 2015)| | ||
| + | |0-002 |1.04 | +0.05 | 1.6 | 0.00 |4000 | SG | -| | ||
| + | |0-003 |1.50 | +0.00 | 1.6 | 0.00 |3000 | MS | Small convective core (around 8% of the stellar mass)| | ||
| + | |0-004 |1.50 | +0.00 | 1.6 | 0.00 |4000 | TAMS| -| | ||
| + | |0-005 |1.50 | +0.00 | 1.6 | 0.00 |4000 | SG | -| | ||
| + | ^<color # | ||
| + | |b-001 |1.00 | -0.08 | 1.6 | 0.00 |1314 | MS | Taken directly from BaSTI online HR utility| | ||
| + | |b-002 |1.00 | -0.08 | 1.6 | 0.00 |1719 | SG | Taken directly from BaSTI online HR utility| | ||
| + | ---- | ||
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| + | ===== Exercise #0: BaSTI models ====== | ||
| + | |||
| + | ^Package ^Date ^Author ^Description | ||
| + | ^wp121130_basti-smodels| 07/02/2019 | S. Cassisi | stellar interior models| fgong |([[https:// | ||
| + | ^wp121130_basti-omodels| (tbd)| | ||
| + | ^Physics|||||| | ||
| + | ^Code | BaSTI code last release||||| | ||
| + | ^Convection| MLT formalism in the superadiabatic layers; solar-calibrated mixing length||||| | ||
| + | ^Overshoot | Two sets of models have been provided: (1) No overshooting - (2) Overshooting with a maximum efficiency equal to lambda = 0.2 Hp. For models at the transition between stars with radiative core and stars with a well developed convective core an accurate scheme has been adopted based on check on the size of the canonical convective core and a linear ramping of the overshoot efficiency (see the document for details) ||||| | ||
| + | ^Extra mixing | No ||||| | ||
| + | ^gradT |In the overshooting region the radiative gradient is adopted ||||| | ||
| + | ^Wind | Two sets of models 1) NO mass loss - 2) Mass loss according to the Reimer’s prescription with the efficiency calibrated on aster-seismic constraints (see the document for details)||||| | ||
| + | ^Atmosphere | Vernazza T(tau) in the regime of low mass stars - Boundary conditions from Phoenix model atmosphere for VLM stellar models (a lot of care has been devoted to allow a smooth transition in the two stellar regimes) ||||| | ||
| + | ^Nuclear rates |Last NACRE updates + updates for some specific nuclear process as N14 + p (see the attached document) ||||| | ||
| + | ^Screening |Electron screening is calculated according to the appropriate choice among strong, intermediate, | ||
| + | ^EOS |Freeos (Irwin and collaboration) in EOS 1 (more accurate option) ||||| | ||
| + | ^Opacities |Radiative - High T opacity OPAL - low T opacity Ferguson - Conductive opacity (Cassisi et al. 2007)||||| | ||
| + | ^mDiffusion |Two sets of models: 1) No diffusion 2) Diffusion accounted for by using the scheme by Thouls et al. (1994) ||||| | ||
| + | ^rLevitation | No ||||| | ||