Pulsars as Astrophysical Laboratories for Nuclear and Particle Physics

By F. Weber, R. Negreiros, P. Rosenfield, M. Stejner. 2006

553 citations recorded by the source corpus.

Abstract A forefront of research concerns the exploration of the properties of hadronic matter under extreme conditions of temperature and density, and the determination of the equation of state–the relation between pressure, temperature and density–of such matter. Experimentally, relativistic heavy-ion collision experiments enable physicists to cast a brief glance at hot and ultra-dense matter for times as small as about 10−22 s. Complementary to this, the matter that exists in the cores of neutron stars, observed as radio pulsars, X-ray pulsars, and magnetars, is at low temperatures but compressed permanently to ultra-high densities that may be more than an order of magnitude higher than the density of atomic nuclei. This makes pulsars superb astrophysical laboratories for medium and high-energy nuclear physics, as discussed in this paper.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/cd0d294579f71c549d88c9b7260ec9852d6abecc

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Citations in the corpus

Composition and stability of hybrid stars with hyperons and quark color-superconductivity (2011, methodology): “The nuclear equation of state, as is well known, can be constructed starting from a number of principles, see,.g., Weber (1999) and Sedrakian (2007).”
Neutrino emission from neutron stars (2000, background): “(3) The third hypothesis predicts a phase transition to the strange quark matter composed of almost free u, d and s quarks with small admixture of electrons (see Weber 1999 for review).”
An Exact Anisotropic Quark Star Model (2002, background): “Anisotropic fluid sphere configurations have been analyzed, using various additional assmptions, in Bayin (1982) and Cosenza et al. (1981) (Krori et al. 1984; Maharaj & Maartens 1989; Stewart 1982; Singh et al. 1992; Magli & Kijowski 1992; Magli 1993; Bondi 1992; Chan et al. 1993; Herrera & Ponce de”
CORE-COLLAPSE SUPERNOVA EXPLOSIONS TRIGGERED BY A QUARK–HADRON PHASE TRANSITION DURING THE EARLY POST-BOUNCE PHASE (2010, background): “…configuration, because quark stars (or hybrid stars with extended strange quark cores) are energetically self bound objects, the total internal energy becomes larger than the gravitational binding energy, at the densities considered here (for a detailed discussion, see e.g. § 18 in Weber 1999).”
Strange quark matter and compact stars (2004, methodology): “Figure 1: Competing structures and novel phases of subatomic matter predicted by theory to make their appearance in the cores (R < ∼ 8 km) of neutron stars [2].”
Progress in Constraining Nuclear Symmetry Energy Using Neutron Star Observables Since GW170817 (2021, background): “The symmetry energy Esym(ρ) at supra-saturation densities and the possible hadron-quark phase transition are among the most uncertain parts of the EOS of dense neutron-rich matter [11,12,14, 28].”
Superfluidity in nuclear systems and neutron stars (2018, background): “star interiors is discussed, for example, in [74], [75], and [76].”
Unified equations of state for cold non-accreting neutron stars with Brussels-Montreal functionals. I. Role of symmetry energy (2018, background): “At higher densities, other particles such as hyperons might appear (Haensel et al. 2007; Weber et al. 2007), but we do not consider this possibility here.”
Quark phases in neutron stars and a third family of compact stars as signature for phase transitions (2000, methodology): “3) for μn ≥ μ([2]) n we can construct the full EOS in the form p = p( ).”
Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions (2006, background): “…level) for PSR J0751+1807 and of 2.0± 0.1 M⊙ from the innermost stable circular orbit for 4U 1636-536, the baryon mass - gravitational mass relationships from Pulsar B in J0737-3039 and the mass-radius relationships from quasiperiodic brightness oscillations in 4U 0614+09 and from the thermal…”
Equations of state for supernovae and compact stars (2016, background): “Theoretically, slowly rotating stars can be described in the Hartle and Thorne approximation (Hartle and Thorne, 1968), see, e.g., the textbook by Weber (1999).”
Implications from GW170817 and I-Love-Q relations for relativistic hybrid stars (2017, background): “In general, there exist two prescriptions for matching the low-density nucleonic EOS to the quark matter EOS; which one is realized in nature depends on the surface tension between nuclear and quark matter [72,73].”
Equation-of-state dependence of the gravitational-wave signal from the ring-down phase of neutron-star mergers (2012, background): “[2, 3, 53] for details and for observational consequences discriminating this scenario from ordinary NS; see [37, 61] for the consequences of this hypothetical state of matter in the context of compact binary mergers).”
The cooling of compact stars (2005, methodology): “Figure 1 shows two sample models for the EOS of neutron star matter (protons and neutrons only) which are obtained from variational calculations based on the Urbana V14 two-nucleon interaction supplemented with the three-body interactions UVII (left curve) and TNI (right curve) [11].”