Solar Models: Current Epoch and Time Dependences, Neutrinos, and Helioseismological Properties

By J. Bahcall, M. Pinsonneault, S. Basu. 2000

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We calculate accurate solar models and report the detailed time dependences of important solar quantities. We use helioseismology to constrain the luminosity evolution of the Sun and report the discovery of semiconvection in evolved solar models that include diffusion. In addition, we compare the computed sound speeds with the results of p-mode observations by BiSON, GOLF, GONG, LOWL, and MDI instruments. We contrast the neutrino predictions from a set of eight standard-like solar models and four deviant (or deficient) solar models with the results of solar neutrino experiments. For solar neutrino and helioseismological applications, we present present-epoch numerical tabulations of characteristics of the standard solar model as a function of solar radius, including the principal physical and composition variables, sound speeds, neutrino fluxes, and functions needed for calculating solar neutrino oscillations.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/e432edd23e4b72b0aad449e057467e7b09af9bcd

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Citations in the corpus

A Large Stellar Evolution Database for Population Synthesis Studies. I. Scaled Solar Models and Isochrones (2004, background): “It is well known (see, e.g., Bahcall & Pinsonneault 1992, 1995; Basu et al. 1996; Bahcall et al. 2001 and references therein) that solar models without microscopic diffusion cannot properly account for some features of the seismic Sun.”
HABITABLE ZONES AROUND MAIN-SEQUENCE STARS: NEW ESTIMATES (2013, positive): “(1) in Gough (1981) and Table 2 in Bahcall et al. (2001)).”
Origin of the Chemical Elements (2010, background): “Experiments measuring electron neutrinos thus show a smaller flux than initially emitted in the solar core (Bahcall 2001, Bahcall et al. 2001b, Fiorentini et al. 2001).”
Constraints on flavor-diagonal non-standard neutrino interactions from Borexino Phase-II (2019, neutral): “J H E P 0 2 ( 2 0 2 0 ) 0 3 8 For neutrinos coming from the center of the Sun, where the SSM predicts N e (r = 0) ≈ 10(2)NA = 6× 1025/cm3 [25, 26], the resonance energy is E res(0) ≈ ∆m(2)21 cos 2θ12 (1− ε′)2 √ 2GFN e (0)c(2)13 ≈ 2 MeV (1− ε′) , (2.”
Solar fusion cross sections II: the pp chain and CNO cycles (2010, background): “Bahcall and others argued (Bahcall et al., 2001) that helioseismology is a more severe and detailed test of the SSM than neutrino production, so that SSM success in reproducing c(r) made a particle-physics resolution of the solar neutrino problem more likely.”
Neutrino electromagnetic interactions: A window to new physics (2014, methodology): “…limit of 0.8% of the Standard Solar Model (SSM) neutrino flux in the range of energy from 8 to 20 MeV (Gando et al., 2003) by taking as a reference the BP00 SSM prediction φBP008B = 5.05×106 cm−2 s−1 for the solar 8B flux (Bahcall et al., 2001) and assuming an undistorted 8B spectrum for the ν̄e’s.”
Oscillations of neutrinos and mesons in quantum field theory (2001, background): “In the 90’s, the persistent deficit in solar neutrinos [10, 11] observed at Homestake was confirmed by several other experiments [12, 13, 14, 15] and, very recently, the Sudbury Neutrino Observatory announced the detection of a nonelectronic component in the solar neutrino flux [16].”
A New Generation of Standard Solar Models (2016, background): “…results was astonishingly good, it provided both strong support to stellar (solar) evolution theory and to a particle Email to: vinyoles@ice.csic.es, aldos@ice.csic.es physics solution for the problem of the missing neutrinos (Christensen-Dalsgaard et al. 1996; Bahcall et al. 1998, 2001).”
The onset and early evolution of life (2006, background): “Darwin’s “warm little pond,” if it was not swamped, would have been subject to deleterious hard UV at eight times the present fl ux (Canuto et al., 1982; Bahcall et al., 2001; Abe and Ooe, 2001).”
10,000 Standard Solar Models: A Monte Carlo Simulation (2005, background): “13 of Bahcall et al. 2001b or Fig.”