The Physics of Neutron Stars

  title={The Physics of Neutron Stars},
  author={James M. Lattimer and Manju Prakash},
  pages={536 - 542}
Neutron stars are some of the densest manifestations of massive objects in the universe. They are ideal astrophysical laboratories for testing theories of dense matter physics and provide connections among nuclear physics, particle physics, and astrophysics. Neutron stars may exhibit conditions and phenomena not observed elsewhere, such as hyperon-dominated matter, deconfined quark matter, superfluidity and superconductivity with critical temperatures near 1010 kelvin, opaqueness to neutrinos… 
Neutron stars and the dense matter equation of state
Neutron stars provide a unique laboratory with which to study cold, dense matter. The observational quantities of primary astrophysics interest are the maximum mass and the typical radius of a
Neutron Star Physics and EOS
Neutron stars are important because measurement of their masses and radii will determine the dense matter equation of state. They will constrain the nuclear matter symmetry energy, which controls the
Shapiro delay measurement of a two solar mass neutron star
Neutron stars are composed of the densest form of matter known to exist in our universe, and thus provide a unique laboratory for exploring the properties of cold matter at supranuclear density.
Physics of strongly magnetized neutron stars
There has recently been growing evidence for the existence of neutron stars possessing magnetic fields with strengths that exceed the quantum critical field strength of 4.4 × 1013 G, at which the
Imposing multi-physics constraints at different densities on the neutron Star Equation of State
Neutron star matter spans a wide range of densities, from that of nuclei at the surface to exceeding several times normal nuclear matter density in the core. While terrestrial experiments, such as
The Nuclear Equation of State and Neutron Star Masses
Neutron stars are valuable laboratories for the study of dense matter. Recent observations have uncovered both massive and low-mass neutron stars and have also set constraints on neutron star radii.
Evidence for quark-matter cores in massive neutron stars
The theory governing the strong nuclear force—quantum chromodynamics—predicts that at sufficiently high energy densities, hadronic nuclear matter undergoes a deconfinement transition to a new phase
Multi-Physics Constraints at Different Densities to Probe Nuclear Symmetry Energy in Hyperonic Neutron Stars
The appearance of strangeness in the form of hyperons within the inner core of neutron stars is expected to affect its detectable properties, such as its global structure or gravitational wave


▪ Abstract We review recent progress in the theory of neutron stars and compare its predictions with the observational data on masses, radii, and temperatures. The theory of neutron stars made up of
Neutron Stars Are Giant Hypernuclei
Neutron stars are studied in the framework of Lagrangian field theory of interacting nucleons, hyperons, and mesons, which is solved in the mean field approximation. The theory is constrained to
Compact Stars: Nuclear Physics, Particle Physics, and General Relativity
General relativity compact stars - from dwarfs to black holes relativistic nuclear field theory neutron stars structure and stability of rotating neutron stars limiting rotational period of neutron
Physics of Neutron Stars
Since the first identification of neutron stars, in pulsars, a decade ago, theoretical and observational knowledge of these unusual objects has grown at a rapid rate. In this article we describe
Neutron Star Structure and the Equation of State(Nuclear Astrophysics,New Frontiers in QCD 2010-Exotic Hadron Systems and Dense Matter-)
The structure of neutron stars is considered from theoretical and observational perspectives. We demonstrate an important aspect of neutron star structure: the neutron star radius is primarily
Model atmospheres for cooling neutron stars
A number of investigators have computed the surface temperature of a cooling neutron star as a function of time after its birth and of the physics of the high-density interior. Einstein observations
Gravitationally redshifted absorption lines in the X-ray burst spectra of a neutron star
The discovery of significant absorption lines in the spectra of 28 bursts of the low-mass X-ray binary EXO0748-676 is reported, which is completely consistent with models of neutron stars composed of normal nuclear matter, while it excludes some models in which the neutron stars are made of more exotic matter.
Neutrino pair emission from finite-temperature neutron superfluid and the cooling of young neutron stars
The neutrons inside neutron stars are almost certainly superfluid below a critical temperature T/subc/approx.10/sup 10/ K. Below T/subc/, pairs of excited neutron quasiparticles may recombine,
Crustal Heating and Quiescent Emission from Transiently Accreting Neutron Stars
Nuclear reactions occurring at densities ≈ 1012 g cm-3 in the crust of a transiently accreting neutron star efficiently maintain the core at a temperature ≈ (5-10)×107 K. When accretion halts, the
▪ Abstract Even the elusive neutrinos are trapped in matter, albeit transiently, in several astrophysical circumstances. Their interactions with the ambient matter not only reveal the properties of