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.
| Package | Date | Author | Description | Format | Download |
|---|---|---|---|---|---|
| wp121130_ex0-smodels | 21/01/2019 | J. Christensen-Daalsgard | Model-S | gong, amdl | ( 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 | Christensen-Dalsgaard(2008) Christensen-Dalsgaard (2021) | ||||
| Package | Date | Author | Description | Format | Download |
|---|---|---|---|---|---|
| wp121130_ex0-smodels | 21/01/2019 | A. Serenelli | stellar interior models | gong, amdl | ( 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 |
—-
| Package | Date | Author | Description | Format | Link |
|---|---|---|---|---|---|
| wp121130_basti-smodels | 07/02/2019 | S. Cassisi | stellar interior models | fgong | ( 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 | ||||