Thermodynamic Functions of Dense Plasmas: Analytic Approximations for Astrophysical Applications
By A. Potekhin, G. Institute, Saint-Petersburg ENS-Lyon, C. Cnrs. 2010
164 citations recorded by the source corpus.
We briefly review analytic approximations of thermodynamic functions of fully ionized nonideal electronion plasmas, applicable in a wide range of plasma parameters, including the domains of nondegenerate and degenerate, nonrelativistic and relativistic electrons, weakly and strongly coupled Coulomb liquids, classical and quantum Coulomb crystals. We present improvements to previously published approximations. Our code for calculation of thermodynamic functions based on the reviewed approximations is made publicly available (© 2010 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)
Subfields: Atomic and Molecular Physics, and Optics, Geophysics
View Paper: https://www.semanticscholar.org/paper/cae203338dfd95841820af04842b17b1beac073e
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In Atomic and Molecular Physics, and Optics
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Citations in the corpus
- Modules for Experiments in Stellar Astrophysics (MESA): Pulsating Variable Stars, Rotation, Convective Boundaries, and Energy Conservation (2019, methodology): “RSP uses the same MESA opacity and equation of state (EOS) modules, inlist structure, profile and history output files, photo files for saving and restarting runs, run star extras extensions, and hooks for using externally supplied routines.”
- Modules for Experiments in Stellar Astrophysics (MESA): Time-dependent Convection, Energy Conservation, Automatic Differentiation, and Infrastructure (2022, background): “…effects of positrons, relativity, and electron degeneracy (Timmes & Swesty 2000; Baturin et al. 2019), Coulomb interactions (Ichimaru et al. 1987; Potekhin & Chabrier 2010; Potekhin & Chabrier 2000; DeWitt & Slattery 1999; Baiko et al. 2001; Farouki & Hamaguchi 1993), non-linear mixing effects…”
- Unified equations of state for cold non-accreting neutron stars with Brussels-Montreal functionals. I. Role of symmetry energy (2018, methodology): “A more accurate (but discontinuous) parametrization that fits even the steps in the P − n̄ curves is given by the analytical thermodynamic model of a fully ionized Coulomb plasma (e.g., Potekhin & Chabrier 2010) with the composition determined by Tables 3 – 6.”
- NEW EQUATIONS OF STATE IN SIMULATIONS OF CORE-COLLAPSE SUPERNOVAE (2011, background): “More elaborated approaches for the Coulomb energy of a multi-component plasma at finite temperature can, e.g., be found in Nadyozhin & Yudin (2005), Potekhin et al. (2009), and Potekhin & Chabrier (2010).”
- Unifying the observational diversity of isolated neutron stars via magneto-thermal evolution models. (2013, methodology): “For the specific heat, we use the latest version of the equation of state for a strongly magnetized, fully ionized electron-ion plasma (Potekhin & Chabrier 2010)6.”
- Neutron Stars—Cooling and Transport (2015, methodology): “Analytical fits for all above-mentioned contributions to the EoS of electron-ion plasmas were presented by Potekhin and Chabrier (2010, 2013).”
- MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA) (2010, methodology): “Outside the region covered by the MESA tables, the HELM (Timmes & Swesty 2000), and PC (Potekhin & Chabrier 2010) EOSs are employed.”
- MESA ISOCHRONES AND STELLAR TRACKS (MIST). I. SOLAR-SCALED MODELS (2016, methodology): “The HELM and PC tables (Potekhin & Chabrier 2010) are used at temperatures and densities outside the range covered by the OPAL + SCVH + MacDonald tables, and assume full ionization.”
- Constraints from Gravitational-wave Detections of Binary Black Hole Mergers on the 12C(α, γ)16O Rate (2020, methodology): “The EOS is a blend of the OPAL (Rogers & Nayfonov 2002), SCVH (Saumon et al. 1995), PTEH (Pols et al. 1995), HELM (Timmes & Swesty 2000), and PC (Potekhin & Chabrier 2010) EOSs.”