NSE abundance data

Odrzywołek, A.

doi:10.1016/j.adt.2012.06.002

Cited by 2 publications

(2 citation statements)

References 13 publications

(21 reference statements)

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“…Our ensemble contained a total of 728 nuclei, which were primarily selected to cover a decent number of possible inputs for astrophysical simulations (see table A of [24] and table B of [20] for the selection of these nuclei). For other recent discussions on nuclear abundance calculation, see [25][26][27][28][29]. There are at least two main features of the present calculation that distinguish it from NSE calculations of the past.…”

Section: Introductionmentioning

confidence: 83%

“…Section 2 briefly describes the formalism which was adopted to calculate the TDNPFs and nuclear abundances of all nuclei present in our pool. Section 3 discusses our results and also compares Fe G (12,14,16) G (12,14,16) G (12,14,16) G (18,20,22) G (18,20,22) G (18,20,22) G (24,26,28) G (24,26,28) G (24,26,28 our calculation with previous calculations. We finally conclude our findings in section 4.…”

Section: Introductionmentioning

confidence: 91%

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Temperature-dependent nuclear partition functions and abundances in the stellar interior

et al. 2016

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We calculate the temperature-dependent nuclear partition functions (TDNPFs) and nuclear abundances for 728 nuclei, assuming nuclear statistical equilibrium (NSE). The theories of stellar evolution support NSE. Discrete nuclear energy levels have been calculated microscopically, using the pn-QRPA theory, up to an excitation energy of 10 MeV in the calculation of the TDNPFs. This feature of our paper distinguishes it from previous calculations. Experimental data is also incorporated wherever available to ensure the reliability of our results. Beyond 10 MeV, we employ a simple Fermi gas model and perform integration over the nuclear level densities to approximate the TDNPFs. We calculate nuclidic abundances, using the Saha equation, as a function of three parameters: stellar density, stellar temperature and the lepton-tobaryon content of stellar matter. All these physical parameters are considered to be extremely important in the stellar interior. The results obtained in this paper show that the equilibrium configuration of nuclei remains unaltered by increasing the stellar density (only the calculated nuclear abundances increase by roughly the same order of magnitude). Increasing the stellar temperature smoothes the equilibrium configuration showing peaks at the neutron-number magic nuclei.

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Section: Introductionmentioning

confidence: 83%

Section: Introductionmentioning

confidence: 91%

Temperature-dependent nuclear partition functions and abundances in the stellar interior

et al. 2016

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Modules for Experiments in Stellar Astrophysics (Mesa): Binaries, Pulsations, and Explosions

Paxton¹,

Marchant²,

Schwab³

et al. 2015

ApJS

2,589

1,725

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We substantially update the capabilities of the open-source software instrument Modules for Experiments in Stellar Astrophysics (MESA). MESA can now simultaneously evolve an interacting pair of differentially rotating stars undergoing transfer and loss of mass and angular momentum, greatly enhancing the prior ability to model binary evolution. New MESA capabilities in fully coupled calculation of nuclear networks with hundreds of isotopes now allow MESA to accurately simulate advanced burning stages needed to construct supernova progenitor models. Implicit hydrodynamics with shocks can now be treated with MESA, enabling modeling of the entire massive star lifecycle, from pre-main sequence evolution to the onset of core collapse and nucleosynthesis from the resulting explosion. Coupling of the GYRE non-adiabatic pulsation instrument with MESA allows for new explorations of the instability strips for massive stars while also accelerating the astrophysical use of asteroseismology data. We improve treatment of mass accretion, giving more accurate and robust near-surface profiles. A new MESA capability to calculate weak reaction rates "on-the-fly" from input nuclear data allows better simulation of accretion induced collapse of massive white dwarfs and the fate of some massive stars. We discuss the ongoing challenge of chemical diffusion in the strongly coupled plasma regime, and exhibit improvements in MESA that now allow for the simulation of radiative levitation of heavy elements in hot stars. We close by noting that the MESA software infrastructure provides bit-for-bit consistency for all results across all the supported platforms, a profound enabling capability for accelerating MESA's development.

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NSE abundance data

Cited by 2 publications

References 13 publications

Temperature-dependent nuclear partition functions and abundances in the stellar interior

Temperature-dependent nuclear partition functions and abundances in the stellar interior

Modules for Experiments in Stellar Astrophysics (Mesa): Binaries, Pulsations, and Explosions

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