Neutron Stars 1 : Equation of State and Structure

By P. Haensel, A. Potekhin, D. Yakovlev. 2007

1,300 citations recorded by the source corpus.

View Paper: https://www.semanticscholar.org/paper/f836051af4b133e357f0c19d6277c423e109e0b8

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In Astronomy and Astrophysics

Citations in the corpus

EQUATION OF STATE AND NEUTRON STAR PROPERTIES CONSTRAINED BY NUCLEAR PHYSICS AND OBSERVATION (2013, background): “…in a sea of electrons at low densities in the outer crust, to increasingly neutron-rich structures in the inner crust, to the extremely neutron-rich uniform matter in the outer core, and possibly exotic states of matter at high densities in the inner core (Haensel et al. 2006; Lattimer 2012).”
Neutron stars and the nuclear equation of state (2021, background): “Neutron stars (NS) harbor unique conditions that challenge the physical theories of dense matter [1].”
Theoretical foundations of quantum hydrodynamics for plasmas (2017, background): “teriors of giant planets, white and brown dwarfs, stellar cores, and the outer envelope of neutron stars are examples of matter in the state of a partially degenerate dense plasma (warm dense matter) [11, 12]. Experimental studies of dense plasmas include the free electron laser excited plasmas [13]”
Neutron Stars—Cooling and Transport (2015, methodology): “The latter parameter has been fitted as function of density for modern BSk models of nuclear matter (Potekhin et al. 2013) and for some other models (Appendix B in Haensel et al. 2007).”
Thermodynamic Functions of Dense Plasmas: Analytic Approximations for Astrophysical Applications (2010, methodology): “hat in applications, as long as the electrons are relativistic, their exchange and correlation contributions are orders of magnitude smaller than the other contributions to the EOS of EIP (see, e.g., [8,13]). 4 One-component plasma 4.1 Coulomb liquid For the reduced free energy of the ion-ion intera”
From hadrons to quarks in neutron stars: a review (2017, background): “At nB 10n0 (∼3 × 107 g cm−3) the equations of state are unaffected by magnetic fields as strong as 1014 G, and by temperatures 109 K [1].”
Ab initio simulation of warm dense matter (2019, background): “[8–13] and the outer crust of neutron stars [14, 15].”
Unified equations of state for cold non-accreting neutron stars with Brussels-Montreal functionals. I. Role of symmetry energy (2018, background): “The unified treatment of all three regions of neutron stars that we present in this paper therefore does not include these outermost parts, which do not in any case involve any new nuclear physics, and have been extensively discussed by Haensel et al. (2007).”
Extreme states of matter on Earth and in space (2009, neutral): “Under the conditions of a neutron star, the Coulomb force represents a weak perturbation with respect to the magnetic one, and for typical stellar temperatures the electrons reside at the Landau level [7, 224].”