Help FAQ History

Stellar observables Enter with the stellar observed parameters together with their 1σ errors (here assumed to be Gaussian): Name T _{eff} = ± K, [Fe/H]= ± dex Asteroseismic parameters: Warning: for PARSEC models, Δν are computed using scaling relations, while for MESA models, they come from individual radial-mode frequencies computed along the tracks.

Δν= ± μHz, ν_{max} = ± μHz Warning: ΔP is only taken into consideration for MESA models.

Period spacing: ΔP= ± s Spectroscopic log g: logg= ± dex Luminosity: L= ± L/L_{☉} Stellar models PARSEC isochrones from Bressan et al. (2012) , with scaled-solar composition and following the Y =0.2485+1.78Z relation. The solar metal content is Z _{☉} =0.0152. They include the pre-main sequence phase. Δν and ν_{max} are computed using scaling relations as in Rodrigues et al. (2014) . ΔP is not taken into consideration yet, only information of the evolutionary stage. PARSEC version 1.2s: available 0.0001≤Z ≤0.06 (-2.2≤[M/H]≤+0.5); for 0.0001≤Z ≤0.02 the mass range is 0.1≤M/M _{☉} <350; for 0.03≤Z ≤0.04 0.1≤M/M _{☉} <150, and for Z =0.06 0.1≤M/M _{☉} <20 (cf. Tang et al. (2014) for 0.001≤Z ≤0.004, and Chen et al. (2015) for other Z ). With revised and calibrated surface boundary conditions in low-mass dwarfs (Chen et al. (2014) ), and a slightly improved resolution. MESA isochrones from Rodrigues et al. (2017) , with scaled-solar composition and following the Y =0.2485+1.007Z relation. The solar metal content is Z _{☉} =0.01756 (Paxton et al. (2011) and Paxton et al. (2013) ). Individual radial-mode frequencies were calculated for each of the models in the grid, hence Δν were computed. ΔP were also computed along the grid of evolutionary tracks. ν_{max} is computed using scaling relation. MESA: available for 0.00176≤Z ≤0.05553 (-1.0≤[M/H]≤+0.5), in the range 0.6≤M/M _{☉} <2.5. With overshooting in low-mass stars. Mass-loss on RGB using the Reimers formula with η _{Reimers} = .

Solar values: Δν_{☉} = μHz, ν_{max} _{☉} = μHz

Bayesian priors Flat prior for age in the interval from yr to yr. Prior on mass -- initial mass function:
Salpeter (1955) with cutoff at 0.01 M☉
Chabrier (2001) exponential
Chabrier (2001) lognormal
Kroupa (1998) corrected for binaries
Kroupa (1998) non corrected for binaries
Prior on evolutionary stage: Unknown RGB core-He burners (RC) non-core He burners (RGB/AGB)

This service is mantained by Léo Girardi and Thaíse Rodrigues at the Osservatorio Astronomico di Padova . Questions, comments and special requests should be directed to leo.girardi@oapd·inaf·it . Last modified: Mon Jul 29 16:35:25 2019