THE JINA REACLIB DATABASE: ITS RECENT UPDATES AND IMPACT ON TYPE-I X-RAY BURSTS

By Richard H. Cyburt, A. Amthor, Ryan M. Ferguson, Z. Meisel, Karl Smith, S. Warren, Alexander Heger, R. Hoffman, T. Rauscher, A. Sakharuk and 3 more. Astrophysical Journal Supplement Series, 2010

788 citations recorded by the source corpus.

We present results from the JINA REACLIB project, an ongoing effort to maintain a current and accurate library of thermonuclear reaction rates for astrophysical applications. Ongoing updates are transparently documented and version tracked, and any set of rates is publicly available and can be downloaded via a Web interface at http://groups.nscl.msu.edu/jina/reaclib/db/. We discuss here our library V1.0, a snapshot of recommended rates for stable and explosive hydrogen and helium burning. We show that the updated reaction rates lead to modest but significant changes in full network, one-dimensional X-ray burst model calculations, compared with calculations with previously used reaction rate sets. The late time behavior of X-ray burst light curves shows significant changes, suggesting that the previously found small discrepancies between model calculations and observations may be solved with a better understanding of the nuclear input. Our X-ray burst model calculations are intended to serve as a benchmark for future model comparisons and sensitivity studies, as the complete underlying nuclear physics is fully documented and publicly available.

Subfields: Nuclear and High Energy Physics, Radiation

View Paper: https://www.semanticscholar.org/paper/02e9705f8ba74a1eb8e7cdf974e24f100a77af3c

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Citations in the corpus

The mass spectrum of compact remnants from the parsec stellar evolution tracks (2015, methodology): “The main hydrogen and helium burning reactions are included as recommended in the JINA data base (Cyburt et al. 2010) with electron screening factors taken from Dewitt, Graboske & Cooper (1973) and Graboske et al. (1973).”
parsec: stellar tracks and isochrones with the PAdova and TRieste Stellar Evolution Code (2012, background): “These are the recommended rates in the JINA reaclib database (Cyburt et al. 2010), from which we also take theQ-value of each reaction.”
MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, methodology): “Nuclear Network We import the nuclear reaction rates directly from the JINA REACLIB database,9 a compilation of the latest reaction rates in the literature (Cyburt et al. 2010).”
Signatures of hypermassive neutron star lifetimes on r-process nucleosynthesis in the disc ejecta from neutron star mergers (2017, methodology): “The strong reaction rates are taken from the JINA REACLIB database (Cyburt et al. 2010), but only the forward rates are used and the inverse rates are computed from detailed balance.”
r-PROCESS LANTHANIDE PRODUCTION AND HEATING RATES IN KILONOVAE (2015, methodology): “We run SkyNet with nuclear reaction rates from the JINA REACLIB database3 (Cyburt et al. 2010).”
Constraints from Gravitational-wave Detections of Binary Black Hole Mergers on the 12C(α, γ)16O Rate (2020, background): “Reverse nuclear reaction rates are computed from detailed balance based on the NACRE/REACLIB reaction rate, instead of consistently from the STARLIB rate.”
PRODUCTION OF ALL THE r-PROCESS NUCLIDES IN THE DYNAMICAL EJECTA OF NEUTRON STAR MERGERS (2014, methodology): “Experimental rates, when available, are taken from the latest versions of REACLIB7 (Cyburt et al. 2010) and Nuclear Wallet Cards.8 Otherwise, the theoretical estimates of fusion rates9 (TALYS; Goriely et al. 2008) and β-decay half-lives (GT2; Tachibana et al. 1990) are adopted, where both are based…”
Sub-Chandrasekhar-mass White Dwarf Detonations Revisited (2017, neutral): “…use a 41-isotope network comprised of neutrons, 1H, 4He, 11B, 12C, 13−14N, 16−17O, 20,22Ne, 23Na, 24−26Mg, 27Al, 28−30Si, 30−31P, 31−32S, 35Cl, 36−39Ar, 39K, 40Ca, 43Sc, 44Ti, 47V, 48Cr, 51Mn, 52,56Fe, 55Co, and 56,58−59Ni, with 190 interlinking reactions from JINA’s REACLIB (Cyburt et al. 2010).”
Merging black hole binaries with the SEVN code (2018, methodology): “The nuclear reaction rates from the JINA REACLIB database (Cyburt et al. 2010) have been updated to their recommended values of April 6, 2015 (Fu et al. 2018).”
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA) (2010, methodology): “…by reactions is derived from the nuclear masses in chem , taken from the JINA Reaclib database (Rauscher & Thielemann 2000; Sakharuk et al. 2006; Cyburt et al. 2010), and accounts for positron annihilations and energy lost to weak neutrinos, using Bahcall (1997, 2002) for the hydrogen burning…”
New PARSEC evolutionary tracks of massive stars at low metallicity: testing canonical stellar evolution in nearby star-forming dwarf galaxies (2014, methodology): “The reaction rates and the corresponding Q-values are taken from the recommended rates in the JINA database (Cyburt et al. 2010).”
STARLIB: A NEXT-GENERATION REACTION-RATE LIBRARY FOR NUCLEAR ASTROPHYSICS (2011, methodology): “For example, the JINA REACLIB Table 2 Summary of STARLIB Rates and Assumption for Uncertainties Rate Evaluation Number Uncertainties Monte Carlo (experimental) 63 Individual NACRE 24 Individual Big bang 9 Individual β-decays (experimental) 2225 Individual β-decays (theoretical) 5556 Individual TALYS”
Improving PARSEC models for very low mass stars (2014, background): “2.1 by Alan W. Irwin 1; • revised opacities from AESOPUS (Marigo & Aringer 2009)2 and the OPAL group (Iglesias & Rogers 1996)3; • adoption of the revised Caffau et al. (2008, 2009) solar chemical abundances; • extended nuclear networks and the reaction rates recommended in the updated JINA REACLIB D”
THE DEUTERIUM-BURNING MASS LIMIT FOR BROWN DWARFS AND GIANT PLANETS (2010, methodology): “Still, the recent release of the Reaclib Database (Cyburt et al. 2010) by the Joint Institute for Nuclear Astrophysics (JINA) uses the Caughlan & Fowler (1988) rate.”
Modules for Experiments in Stellar Astrophysics (MESA): Time-dependent Convection, Energy Conservation, Automatic Differentiation, and Infrastructure (2022, background): “This affects reactions with uncertain nuclear masses; for instance, the reaction 55Cu (γ, p) 54Ni has a Q = 0.293 MeV (exothermic) from “rpsm” (Rauscher 1999, priv. comm) and a Q = −0.07256 MeV (endothermic) from “ths8”7 (Cyburt et al. 2010).”
Evolution of thermally pulsing asymptotic giant branch stars - I. The COLIBRI code (2013, methodology): “For all of them we adopt analytic relations, with fitting coefficients taken from the JINA reaclib database (Cyburt et al. 2010).”