data:models
Table of Contents
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 | ( 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) | ||||
Exercise #0: Garstec models
| 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 |
—-
Exercise #0: BaSTI models
| 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 | ||||
data/models.txt · Last modified: 2022/12/22 14:33 by 127.0.0.1