GW170817: Joint Constraint on the Neutron Star Equation of State from Multimessenger Observations [PDF]
, 2017 Gravitational waves detected from the binary neutron star (NS) merger GW170817 constrained the NS equation of state by placing an upper bound on certain parameters, describing the binary’s tidal interactions.
D. Radice +3 more
semanticscholar +1 more source
Ability of LIGO and LISA to probe the equation of state of the early Universe [PDF]
Journal of Cosmology and Astroparticle Physics, 2019 The expansion history of the Universe between the end of inflation and the onset of radiation-domination (RD) is currently unknown. If the equation of state during this period is stiffer than that of radiation, w > 1/3, the gravitational wave (GW ...
Daniel G. Figueroa, Erwin H. Tanin
semanticscholar +1 more source
Potential Energy Landscape Equation of State
, 2002 Depth, number, and shape of the basins of the potential energy landscape are the key ingredients of the inherent structure thermodynamic formalism introduced by Stillinger and Weber [F. H. Stillinger and T. A. Weber, Phys. Rev. A 25, 978 (1982)].
A. Heuer +29 more
core +1 more source
History of the Equation of State of Seawater [PDF]
Oceanography, 2010 As one of few who have been involved in the equation of state of seawater over the last 40 years, the author was invited to review some of the history behind its early development and also the more recent thermodynamic equation of state.
Frank J. Millero
doaj
Cosmological imprint of an energy component with general equation of state [PDF]
, 1997 We examine the possibility that a significant component of the energy density of the Universe has an equation of state different from that of matter, radiation, or cosmological constant ({Lambda} ).
R. Caldwell, R. Dave, P. Steinhardt
semanticscholar +1 more source
Towards a precision calculation of the effective number of neutrinos Neff in the Standard Model: the QED equation of state [PDF]
Journal of Cosmology and Astroparticle Physics, 2019 We revisit and quantify in this work several aspects of Standard Model physics at finite temperature that drive the theoretical value of the cosmological parameter, the effective number of neutrinos Neff, away from 3 in the early universe.
Jack J. Bennett +3 more
semanticscholar +1 more source
Neutron-star tidal deformability and equation-of-state constraints [PDF]
General Relativity and Gravitation, 2020 Despite their long history and astrophysical importance, some of the key properties of neutron stars are still uncertain. The extreme conditions encountered in their interiors, involving matter of uncertain composition at extreme density and isospin ...
K. Chatziioannou
semanticscholar +1 more source
Revisiting Barrow's graduated inflationary universe: A warm perspective
Physics Letters B, 2022 It is presumed that thermal fluctuations present during inflationary epoch can make inflaton scalar field to interact with other fields resulting in the existence of a thermal component during the inflationary period.
Subhra Bhattacharya
doaj
On the asymptotic limit of steady state Poisson--Nernst--Planck equations with steric effects [PDF]
arXiv, 2022 When ions are crowded, the effect of steric repulsion between ions becomes significant and the conventional Poisson--Boltzmann (PB) equation (without steric effect) should be modified. For this purpose, we study the asymptotic limit of steady state Poisson--Nernst--Planck equations with steric effects (PNP-steric equations).
arxiv
Equation of state and singularities in FLRW cosmological models [PDF]
J.Phys.Conf.Ser.229:012037,2010, 2010 We consider FLRW cosmological models with standard Friedmann equations, but leaving free the equation of state. We assume that the dark energy content of the universe is encoded in an equation of state $p=f(\rho)$, which is expressed with most generality in the form of a power expansion.
arxiv +1 more source