======= 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)]]|||||
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===== 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 |||||