Results 31 to 40 of about 115,270 (322)
Statistical theory of thermal evolution of neutron stars [PDF]
, 2015 Thermal evolution of neutron stars is known to depend on the properties of superdense matter in neutron star cores. We suggest a statistical analysis of isolated cooling middle-aged neutron stars and old transiently accreting quasi-stationary neutron ...
Beznogov, M. V., Yakovlev, D. G.
core +1 more source
Protoneutron stars and neutron stars [PDF]
International Astronomical Union Colloquium, 2000 Abstract We find constraints on minimum and maximum mass of ordinary neutron stars imposed by their early evolution (protoneutron star stage). We calculate models of protoneutron stars using a realistic standard equation of state of hot, dense matter valid for both supranuclear and subnuclear densities.
D. Gondek-Rosinska +2 more
openaire +3 more sources
Detecting supersymmetric Q-balls with neutron stars [PDF]
, 1998 Supersymmetric Q-balls trapped in neutron stars or white dwarfs may cause the stars to explode. Trapping of Q-balls in neutron stars is shown to be less likely, but trapping in neutron star progenitors more likely than hitherto assumed, making neutron ...
Coleman +15 more
core +2 more sources
Detectability of Continuous Gravitational Waves from Magnetically Deformed Neutron Stars
Galaxies, 2021 Neutron stars are known to contain extremely powerful magnetic fields. Their effect is to deform the shape of the star, leading to the potential emission of continuous gravitational waves.
Jacopo Soldateschi, Niccolò Bucciantini
doaj +1 more source
How to identify a Strange Star [PDF]
, 1998 Contrary to young neutron stars, young strange stars are not subject to the r-mode instability which slows rapidly rotating, hot neutron stars to rotation periods near 10 ms via gravitational wave emission.
A. Goyal +22 more
core +2 more sources
EPJ Web of Conferences, 2010 Several aspects related to astrophysics of isolated neutron stars are discussed. We start with an introduction into the “new zoo” of young isolated neutron stars.
Popov S.
doaj +1 more source
Quark Deconfinement in Rotating Neutron Stars
Universe, 2017 In this paper, we use a three flavor non-local Nambu–Jona-Lasinio (NJL) model, an improved effective model of Quantum Chromodynamics (QCD) at low energies, to investigate the existence of deconfined quarks in the cores of neutron stars.
Richard D. Mellinger +4 more
doaj +1 more source
QCD equations of state and speed of sound in neutron stars
AAPPS Bulletin, 2021 Neutron stars are cosmic laboratories to study dense matter in quantum chromodynamics (QCD). The observable mass-radius relations of neutron stars are determined by QCD equations of state and can reflect the properties of QCD phase transitions.
Toru Kojo
doaj +1 more source
Neutron skins and neutron stars [PDF]
AIP Conference Proceedings, 2013 The neutron-skin thickness of heavy nuclei provides a fundamental link to the equation of state of neutron-rich matter, and hence to the properties of neutron stars. The Lead Radius Experiment ("PREX") at Jefferson Laboratory has recently provided the first model-independence evidence on the existence of a neutron-rich skin in 208Pb.
openaire +3 more sources
The Masses of Neutron Stars [PDF]
, 2016 We present in this article an overview of the problem of neutron star masses. After a brief appraisal of the methods employed to determine the masses of neutron stars in binary systems, the existing sample of measured masses is presented, with a highlight on some very well-determined cases.
Jorge Ernesto Horvath, R. Valentim
openaire +4 more sources