10,000 Standard Solar Models: A Monte Carlo Simulation

By J. Bahcall, A. Serenelli, S. Basu. 2005

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We have evolved 10,000 solar models using 21 input parameters that are randomly drawn for each model from separate probability distributions for every parameter. We use the results of these models to determine the theoretical uncertainties in the predicted surface helium abundance, the profile of the sound speed versus radius, the profile of the density versus radius, the depth of the solar convective zone, the eight principal solar neutrino fluxes, and the fractions of nuclear reactions that occur in the CNO cycle or in the three branches of the p-p chains. We also determine the correlation coefficients of the neutrino fluxes for use in analysis of solar neutrino oscillations. Our calculations include the most accurate available input parameters, including radiative opacity, equation of state, and nuclear cross sections. We incorporate both the recently determined heavy element abundances recommended by Asplund et al. and the older (higher) heavy element abundances recommended by Grevesse & Sauval. We present best estimates of many characteristics of the standard solar model for both sets of recommended heavy element compositions.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/0906d38c492b7d7ec9a884e75ecaa07782ccd583

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Citations in the corpus

Helioseismology and Solar Abundances (2007, methodology): “Also, for the models in the Monte Carlo study of (Bahcall et al. 2006), it is found that the average mean molecular weight in the inner 2% of the Sun by radius is 0.7203 ± 0.0029 models with GS98 composition and 0.7088 ± 0.0029 for models with the AGS05 composition (Chaplin et al. 2007b).”
NEW SOLAR COMPOSITION: THE PROBLEM WITH SOLAR MODELS REVISITED (2009, methodology): “This is also consistent with the adoption of meteoritic scales in previous works on solar models (e.g. Bahcall et al. 2005, 2006).”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, background): “17 As noted by Bahcall et al. (2006), there is some ambiguity in the exact definition of the “age of the Sun” as the PMS contraction is estimated to last approximately 0.04 Gyr.”
Solar fusion cross sections II: the pp chain and CNO cycles (2010, methodology): “The prediction of Park et al. (2003) was used by Bahcall et al. (2006) and by Peña-Garay and Serenelli (2008) in their latest determinations of the hep neutrino flux, φν(hep) = (8.22 ± 1.23) × 103 cm−2 s−1, where the error reflects again the 15% uncertainty quoted above.”
Scaled solar tracks and isochrones in a large region of the Z-Y plane I. From the ZAMS to the TP-A (2008, methodology): “Bahcall et al.(2006) used Monte Carlo simulations to determine the uncertainties in solar model predictions of parameters measured by helioseismology (depth of the convective zon , the surface helium abundance, the profiles of the sound speed and density versus radius) and provided determinations…”
Quantifying the uncertainties of chemical evolution studies II. Stellar yields (2010, background): “However, this is incorrect, since the photosphericabundances are no longer representative of the original composition of the Sun at birth, because of the effects of diffusion (e.g. Bahcall et al. 2006).”
New constraints on the chemical evolution of the solar neighbourhood and galactic disc(s) - improved astrophysical parameters for the Geneva-Copenhagen Survey (2011, background): “2 i.e. with best photometric detection http://www.ipac.caltech.edu/ 2mass/releases/allsky/doc/sec16b.html#phqual 3 In this work we takeL⊙ = 3.842× 1033ergs−1 (Bahcall et al. 2006).”
SOLAR MODELS WITH ACCRETION. I. APPLICATION TO THE SOLAR ABUNDANCE PROBLEM (2011, background): “…of the boundary of the convective envelope (RCZ), the sound speed and density profiles, and the presentday surface helium abundance (YS) predicted by SSMs using low (Z/X)⊙ all differ from the values extracted from helioseismology by amounts beyond accepted uncertainties (Bahcall et al. 2006).”
A New Generation of Standard Solar Models (2016, methodology): “Here, instead, we resort to using two sets of 1000 SSMs originally computed by Bahcall et al. (2006), with one set based on GS98 and the other one on AGS05 (Asplund et al. 2005) solar compositions.”
Accurate fundamental parameters for lower main‐sequence stars (2006, unknown): “The absolute bolometric magnitude for a star with luminosity, L, radius, R, and effective temperature, Teff, is MBol = −2.5 log ( L/L ) + MBol, = −2.5 log (R2T 4eff/R2 T 4eff, ) + MBol, , (13) where L = 4 πR2 σT4eff and L = 3.842 × 1033 erg s−1 (Bahcall et al. 2006).”