======= 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. ===== Exercise #1: Model-S models ====== ^Package ^Date ^Author ^Description ^Format ^Download | ^wp121130_ex0-smodels|21/01/2019 | J. Christensen-Daalsgard | Model-S| gong, amdl | ([[https://drive.google.com/file/d/1wt9k343_fRFg29rr5EGGQ8ieAzxbIpdt/view?usp=sharing| ex0-smodels.tar.gz]]) | ^wp121130_ex0-omodels|21/01/2019 | ALL | oscillations| (tbd) |(tbd) | ^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 "low" value of LUNA's N14+p ||||| ^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://ui.adsabs.harvard.edu/abs/2008Ap%26SS.316...13C/abstract|Christensen-Dalsgaard(2008)]] [[https://ui.adsabs.harvard.edu/abs/2021LRSP...18....2C/abstract|Christensen-Dalsgaard (2021)]]||||| ---- ===== Exercise #0: Garstec models ====== ^Package ^Date ^Author ^Description ^Format ^Download | ^wp121130_ex0-smodels|21/01/2019 | A. Serenelli | stellar interior models| gong, amdl | ([[https://drive.google.com/file/d/1wt9k343_fRFg29rr5EGGQ8ieAzxbIpdt/view?usp=sharing| ex0-smodels.tar.gz]]) | ^wp121130_ex0-omodels|21/01/2019 | ALL | oscillations| (tbd) |(tbd) | ^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 "low" value of LUNA's N14+p ||||| ^Screening | Weak (Salpeter)/intermediate (Graboske et al. 1973, subgiants) ||||| ^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.) ||||| ^GARSTEC models |||||||| ^Model ^Mass ^[Fe/H] ^alpha ^ovsh ^Nshell ^Phase ^Notes| |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 | -| ^BaSTI models |||||||| |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| ---- ===== Exercise #0: BaSTI models ====== ^Package ^Date ^Author ^Description ^Format ^Link | ^wp121130_basti-smodels| 07/02/2019 | S. Cassisi | stellar interior models| fgong |([[https://drive.google.com/file/d/1oJpr5GuixQg0eE61LITjqzmmVt-EEcmZ/view?usp=sharing | ex0b-smodels.tar.gz]]) | ^wp121130_basti-omodels| (tbd)| (tbd)| oscillations| (tbd) |(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, and weak, following Dewitt et al. (1973) and Graboske et al. (1973) ||||| ^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 |||||