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The Symmetry Energy: Current Status of Ab Initio Predictions vs. Empirical Constraints. Symmetry (Basel) 2023. [DOI: 10.3390/sym15020450] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/10/2023] Open
Abstract
Infinite nuclear matter is a suitable laboratory to learn about nuclear forces in many-body systems. In particular, modern theoretical predictions of neutron-rich matter are timely because of recent and planned experiments aimed at constraining the equation of state of isospin-asymmetric matter. For these reasons, we have taken a broad look at the equation of state of neutron-rich matter and the closely related symmetry energy, which is the focal point of this article. Its density dependence is of paramount importance for a number of nuclear and astrophysical systems, ranging from neutron skins to the structure of neutron stars. We review and discuss ab initio predictions in relation to recent empirical constraints. We emphasize and demonstrate that free-space nucleon–nucleon data pose stringent constraints on the density dependence of the neutron matter equation of state, which essentially determines the slope of the symmetry energy at saturation.
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Abstract
The neutron lifetime anomaly has been used to motivate the introduction of new physics with hidden-sector particles coupled to baryon number, and on which neutron stars provide powerful constraints. Although the neutron lifetime anomaly may eventually prove to be of mundane origin, we use it as motivation for a broader review of the ways that baryon number violation, be it real or apparent, and dark sectors can intertwine and how neutron star observables, both present and future, can constrain them.
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Abstract
We calculate the nonzero-temperature correction to the beta equilibrium condition in nuclear matter under neutron star merger conditions, in the temperature range 1mEv < T ≲ 5 mEv. We improve on previous work using a consistent description of nuclear matter based on the IUF and SFHo relativistic mean field models. This includes using relativistic dispersion relations for the nucleons, which we show is essential in these models. We find that the nonzero-temperature correction can be of order 10 to 20 MeV, and plays an important role in the correct calculation of Urca rates, which can be wrong by factors of 10 or more if it is neglected.
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Abstract
We study the cooling of isolated neutron stars with particular regard to the importance of nuclear pairing gaps. A microscopic nuclear equation of state derived in the Brueckner-Hartree-Fock approach is used together with compatible neutron and proton pairing gaps. We then study the effect of modifying the gaps on the final deduced neutron star mass distributions. We find that a consistent description of all current cooling data can be achieved and a reasonable neutron star mass distribution can be predicted employing the (slightly reduced by about 40%) proton 1S0 Bardeen-Cooper-Schrieffer (BCS) gaps and no neutron 3P2 pairing.
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Tajima H, Hatsuda T, van Wyk P, Ohashi Y. Superfluid Phase Transitions and Effects of Thermal Pairing Fluctuations in Asymmetric Nuclear Matter. Sci Rep 2019; 9:18477. [PMID: 31811255 PMCID: PMC6897924 DOI: 10.1038/s41598-019-54010-7] [Citation(s) in RCA: 14] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/05/2019] [Accepted: 10/30/2019] [Indexed: 11/09/2022] Open
Abstract
We investigate superfluid phase transitions of asymmetric nuclear matter at finite temperature (T) and density (ρ) with a low proton fraction (Yp ≤ 0.2), which is relevant to the inner crust and outer core of neutron stars. A strong-coupling theory developed for two-component atomic Fermi gases is generalized to the four-component case, and is applied to the system of spin-1/2 neutrons and protons. The phase shifts of neutron-neutron (nn), proton-proton (pp) and neutron-proton (np) interactions up to k = 2 fm-1 are described by multi-rank separable potentials. We show that the critical temperature [Formula: see text] of the neutron superfluidity at Yp = 0 agrees well with Monte Carlo data at low densities and takes a maximum value [Formula: see text]= 1.68 MeV at [Formula: see text] with ρ0 = 0.17 fm-3. Also, the critical temperature [Formula: see text] of the proton superconductivity for Yp ≤ 0.2 is substantially suppressed at low densities due to np-pairing fluctuations, and starts to dominate over [Formula: see text] only above [Formula: see text](0.77) for Yp = 0.1(0.2), and (iii) the deuteron condensation temperature [Formula: see text] is suppressed at Yp ≤ 0.2 due to a large mismatch of the two Fermi surfaces.
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Affiliation(s)
- Hiroyuki Tajima
- Quantum Hadron Physics Laboratory, RIKEN Nishina Center, Wako, Saitama, 351-0198, Japan.
| | - Tetsuo Hatsuda
- Quantum Hadron Physics Laboratory, RIKEN Nishina Center, Wako, Saitama, 351-0198, Japan.,Interdisciplinary Theoretical and Mathematical Sciences Program (iTHEMS), RIKEN, Wako, Saitama, 351-0198, Japan
| | - Pieter van Wyk
- Department of Physics, Keio University, Hiyoshi, Kohoku-ku, Yokohama, 223-8522, Japan
| | - Yoji Ohashi
- Department of Physics, Keio University, Hiyoshi, Kohoku-ku, Yokohama, 223-8522, Japan
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Marczenko M, Blaschke D, Redlich K, Sasaki C. Chiral symmetry restoration by parity doubling and the structure of neutron stars. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.98.103021] [Citation(s) in RCA: 31] [Impact Index Per Article: 5.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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9
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Vidaña I. Hyperons: the strange ingredients of the nuclear equation of state. Proc Math Phys Eng Sci 2018; 474:20180145. [PMID: 30333699 PMCID: PMC6189596 DOI: 10.1098/rspa.2018.0145] [Citation(s) in RCA: 27] [Impact Index Per Article: 4.5] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/01/2018] [Accepted: 08/15/2018] [Indexed: 11/12/2022] Open
Abstract
We review the role and properties of hyperons in finite and infinite nuclear systems. In particular, we present different production mechanisms of hypernuclei, as well as several aspects of hypernuclear γ-ray spectroscopy, and the weak decay modes of hypernuclei. Then we discuss the construction of hyperon-nucleon and hyperon-hyperon interactions on the basis of the meson-exchange and chiral effective field theories. Recent developments based on the so-called V low k approach and lattice quantum chromodynamics will also be addressed. Finally, we go over some of the effects of hyperons on the properties of neutron and proto-neutron stars with an emphasis on the so-called 'hyperon puzzle', i.e. the problem of the strong softening of the equation of state, and the consequent reduction of the maximum mass, induced by the presence of hyperons, a problem which has become more intriguing and difficult to solve due the recent measurements of approximately 2M ⊙ millisecond pulsars. We discuss some of the solutions proposed to tackle this problem. We also re-examine the role of hyperons on the cooling properties of newly born neutron stars and on the development of the so-called r-mode instability.
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Affiliation(s)
- Isaac Vidaña
- Istituto Nazionale di Fisica Nucleare, Dipartimento di Fisica, Università di Catania, Via Santa Sofia 64, 95123, Catania, Italy
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Brown EF, Cumming A, Fattoyev FJ, Horowitz CJ, Page D, Reddy S. Rapid Neutrino Cooling in the Neutron Star MXB 1659-29. PHYSICAL REVIEW LETTERS 2018; 120:182701. [PMID: 29775364 DOI: 10.1103/physrevlett.120.182701] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/20/2017] [Revised: 12/20/2017] [Indexed: 06/08/2023]
Abstract
We show that the neutron star in the transient system MXB 1659-29 has a core neutrino luminosity that substantially exceeds that of the modified Urca reactions (i.e., n+n→n+p+e^{-}+ν[over ¯]_{e} and inverse) and is consistent with the direct Urca (n→p+e^{-}+ν[over ¯]_{e} and inverse) reaction occurring in a small fraction of the core. Observations of the thermal relaxation of the neutron star crust following 2.5 yr of accretion allow us to measure the energy deposited into the core during accretion, which is then reradiated as neutrinos, and infer the core temperature. For a nucleonic core, this requires that the nucleons are unpaired and that the proton fraction exceeds a critical value to allow the direct Urca reaction to proceed. The neutron star in MXB 1659-29 is the first with a firmly detected thermal component in its x-ray spectrum that needs a fast neutrino-cooling process. Measurements of the temperature variation of the neutron star core during quiescence would place an upper limit on the core specific heat and serve as a check on the fraction of the neutron star core in which nucleons are unpaired.
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Affiliation(s)
- Edward F Brown
- Department of Physics and Astronomy, Michigan State University, 567 Wilson Road, East Lansing, Michigan 48864, USA
| | - Andrew Cumming
- Department of Physics and McGill Space Institute, McGill University, 3600 rue University, Montreal, Quebec, Canada H3A 2T8
| | - Farrukh J Fattoyev
- Center for Exploration of Energy and Matter and Department of Physics, Indiana University, Bloomington, Indiana 47405, USA
| | - C J Horowitz
- Center for Exploration of Energy and Matter and Department of Physics, Indiana University, Bloomington, Indiana 47405, USA
| | - Dany Page
- Instituto de Astronomía, Universidad Nacional Autónoma de México, México, CDMX 04510, Mexico
| | - Sanjay Reddy
- Institute for Nuclear Theory, University of Washington, Seattle, Washington 98195, USA
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13
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Nuclear Equation of State for Compact Stars and Supernovae. THE PHYSICS AND ASTROPHYSICS OF NEUTRON STARS 2018. [DOI: 10.1007/978-3-319-97616-7_6] [Citation(s) in RCA: 21] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/05/2022]
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14
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Paschalidis V, Stergioulas N. Rotating stars in relativity. LIVING REVIEWS IN RELATIVITY 2017; 20:7. [PMID: 29225510 PMCID: PMC5707374 DOI: 10.1007/s41114-017-0008-x] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/08/2016] [Accepted: 10/03/2017] [Indexed: 05/13/2023]
Abstract
Rotating relativistic stars have been studied extensively in recent years, both theoretically and observationally, because of the information they might yield about the equation of state of matter at extremely high densities and because they are considered to be promising sources of gravitational waves. The latest theoretical understanding of rotating stars in relativity is reviewed in this updated article. The sections on equilibrium properties and on nonaxisymmetric oscillations and instabilities in f-modes and r-modes have been updated. Several new sections have been added on equilibria in modified theories of gravity, approximate universal relationships, the one-arm spiral instability, on analytic solutions for the exterior spacetime, rotating stars in LMXBs, rotating strange stars, and on rotating stars in numerical relativity including both hydrodynamic and magnetohydrodynamic studies of these objects.
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Affiliation(s)
- Vasileios Paschalidis
- Theoretical Astrophysics Program, Departments of Astronomy and Physics, University of Arizona, Tucson, AZ 85721 USA
- Department of Physics, Princeton University, Princeton, NJ 08544 USA
| | - Nikolaos Stergioulas
- Department of Physics, Aristotle University of Thessaloniki, 54124 Thessaloniki, Greece
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18
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Timashev SF. Initiating nuclear-chemical transformations in native systems: Phenomenology. RUSSIAN JOURNAL OF PHYSICAL CHEMISTRY A 2016. [DOI: 10.1134/s0036024416100253] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/22/2022]
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19
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Kryvdyk V. Generation of high-energy particles, neutrino and fotons in magnetosphere of collapsing star. EPJ WEB OF CONFERENCES 2014. [DOI: 10.1051/epjconf/20147000056] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
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Passamonti A, Gaertig E, Kokkotas KD, Doneva D. Evolution of thef-mode instability in neutron stars and gravitational wave detectability. Int J Clin Exp Med 2013. [DOI: 10.1103/physrevd.87.084010] [Citation(s) in RCA: 27] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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22
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Alford MG, Reddy S, Schwenzer K. Bridging the gap by squeezing superfluid matter. PHYSICAL REVIEW LETTERS 2012; 108:111102. [PMID: 22540455 DOI: 10.1103/physrevlett.108.111102] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/27/2011] [Indexed: 05/31/2023]
Abstract
Cooper pairing between fermions in dense matter leads to the formation of a gap in the fermionic excitation spectrum and typically exponentially suppresses transport properties. However, we show here that reactions involving conversion between different fermion species, such as Urca reactions in nuclear matter, become strongly enhanced and approach their ungapped level when the matter undergoes density oscillations of sufficiently large amplitude. We study both the neutrino emissivity and the bulk viscosity due to direct Urca processes in hadronic, hyperonic, and quark matter and discuss different superfluid and superconducting pairing patterns.
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Affiliation(s)
- Mark G Alford
- Department of Physics, Washington University, St. Louis, Missouri 63130, USA
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Chamel N, Haensel P. Physics of Neutron Star Crusts. LIVING REVIEWS IN RELATIVITY 2008; 11:10. [PMID: 28163609 PMCID: PMC5255077 DOI: 10.12942/lrr-2008-10] [Citation(s) in RCA: 39] [Impact Index Per Article: 2.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 09/05/2008] [Indexed: 05/28/2023]
Abstract
The physics of neutron star crusts is vast, involving many different research fields, from nuclear and condensed matter physics to general relativity. This review summarizes the progress, which has been achieved over the last few years, in modeling neutron star crusts, both at the microscopic and macroscopic levels. The confrontation of these theoretical models with observations is also briefly discussed.
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Affiliation(s)
- Nicolas Chamel
- Institut d’Astronomie et d’Astrophysique, Université Libre de Bruxelles, CP226, Boulevard du Triomphe, B-1050 Brussels, Belgium
| | - Pawel Haensel
- Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Bartycka 18, 00-716 Warszawa, Poland
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25
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Le Fèvre A, Auger G, Begemann-Blaich ML, Bellaize N, Bittiger R, Bocage F, Borderie B, Bougault R, Bouriquet B, Charvet JL, Chbihi A, Dayras R, Durand D, Frankland JD, Galichet E, Gourio D, Guinet D, Hudan S, Immé G, Lautesse P, Lavaud F, Legrain R, Lopez O, Łukasik J, Lynen U, Müller WFJ, Nalpas L, Orth H, Plagnol E, Raciti G, Rosato E, Saija A, Schwarz C, Seidel W, Sfienti C, Tamain B, Trautmann W, Trzciński A, Turzó K, Vient E, Vigilante M, Volant C, Zwiegliński B, Botvina AS. Isotopic scaling and the symmetry energy in spectator fragmentation. PHYSICAL REVIEW LETTERS 2005; 94:162701. [PMID: 15904219 DOI: 10.1103/physrevlett.94.162701] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/20/2004] [Indexed: 05/02/2023]
Abstract
Isotopic effects in the fragmentation of excited target residues following collisions of 12C on (112,124)Sn at incident energies of 300 and 600 MeV per nucleon were studied with the INDRA 4pi detector. The measured yield ratios for light particles and fragments with atomic number Z < or = 5 obey the exponential law of isotopic scaling. The deduced scaling parameters decrease strongly with increasing centrality to values smaller than 50% of those obtained for the peripheral event groups. Symmetry-term coefficients, deduced from these data within the statistical description of isotopic scaling, are near gamma = 25 MeV for peripheral and gamma < 15 MeV for central collisions.
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Affiliation(s)
- A Le Fèvre
- Gesellschaft für Schwerionenforschung mbH, D-64291 Darmstadt, Germany
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26
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Villain L, Bonazzola S, Haensel P. Inertial modes in stratified rotating neutron stars: An evolutionary description. Int J Clin Exp Med 2005. [DOI: 10.1103/physrevd.71.083001] [Citation(s) in RCA: 9] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Abstract
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 10(10) kelvin, opaqueness to neutrinos, and magnetic fields in excess of 10(13) Gauss. Here, we describe the formation, structure, internal composition, and evolution of neutron stars. Observations that include studies of pulsars in binary systems, thermal emission from isolated neutron stars, glitches from pulsars, and quasi-periodic oscillations from accreting neutron stars provide information about neutron star masses, radii, temperatures, ages, and internal compositions.
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Affiliation(s)
- J M Lattimer
- Department of Physics and Astronomy, State University of New York, Stony Brook, NY 11794-3800, USA.
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29
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Reisenegger A, Bonacić A. Millisecond pulsars with r-modes as steady gravitational radiators. PHYSICAL REVIEW LETTERS 2003; 91:201103. [PMID: 14683350 DOI: 10.1103/physrevlett.91.201103] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 03/14/2003] [Indexed: 05/21/2023]
Abstract
Millisecond pulsars (MSPs) probably achieve their fast rotation by mass transfer from their companion stars in low-mass x-ray binaries (LMXBs). The lack of MSPs and LMXBs rotating near breakup has been attributed to the accretion torque being balanced, at fast rotation, by gravitational radiation, perhaps caused by an unstable oscillation mode. It has been argued that internal dissipation involving hyperons may cause LMXBs to evolve into a quasisteady state, with nearly constant rotation rate, temperature, and mode amplitude. We show that MSPs descending from these LMXBs spend a long time in a similar state, as extremely steady sources of gravitational waves and thermal x rays, while they spin down due to gravitational radiation and the standard magnetic torque. Observed MSP braking torques already place meaningful constraints on this scenario.
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Affiliation(s)
- Andreas Reisenegger
- Departamento de Astronomía y Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Casilla 306, Santiago 22, Chile.
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30
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Abstract
Rotating relativistic stars have been studied extensively in recent years, both theoretically and observationally, because of the information they might yield about the equation of state of matter at extremely high densities and because they are considered to be promising sources of gravitational waves. The latest theoretical understanding of rotating stars in relativity is reviewed in this updated article. The sections on the equilibrium properties and on the nonaxisymmetric instabilities in f-modes and r-modes have been updated and several new sections have been added on analytic solutions for the exterior spacetime, rotating stars in LMXBs, rotating strange stars, and on rotating stars in numerical relativity. ELECTRONIC SUPPLEMENTARY MATERIAL Supplementary material is available for this article at 10.12942/lrr-2003-3.
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Affiliation(s)
- Nikolaos Stergioulas
- Department of Physics, Aristotle University of Thessaloniki, Thessaloniki, 54124 Greece
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31
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Li BA. Probing the high density behavior of the nuclear symmetry energy with high energy heavy-ion collisions. PHYSICAL REVIEW LETTERS 2002; 88:192701. [PMID: 12005628 DOI: 10.1103/physrevlett.88.192701] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/14/2001] [Indexed: 05/23/2023]
Abstract
High energy heavy-ion collisions are proposed as a novel means to constrain stringently the high density (HD) behavior of nuclear symmetry energy. Within an isospin-dependent hadronic transport model, it is shown for the first time that the isospin asymmetry of the HD nuclear matter formed in high energy heavy-ion collisions is uniquely determined by the HD behavior of the nuclear symmetry energy. Experimental signatures in two sensitive probes, i.e., pi(-) to pi(+) ratio and neutron-proton differential collective flow, are also investigated.
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Affiliation(s)
- Bao-An Li
- Department of Chemistry and Physics, P.O. Box 419, Arkansas State University, State University, Arkansas 72467-0419, USA.
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32
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Khalilov VR. Macroscopic effects in cold magnetized nucleons and electrons with anomalous magnetic moments. Int J Clin Exp Med 2002. [DOI: 10.1103/physrevd.65.056001] [Citation(s) in RCA: 39] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Prakash M, Lattimer JM, Pons JA, Steiner AW, Reddy S. Evolution of a Neutron Star from Its Birth to Old Age. ACTA ACUST UNITED AC 2001. [DOI: 10.1007/3-540-44578-1_14] [Citation(s) in RCA: 7] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 03/06/2023]
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34
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Li BA. Neutron-proton differential flow as a probe of isospin-dependence of the nuclear equation of state. PHYSICAL REVIEW LETTERS 2000; 85:4221-4224. [PMID: 11060603 DOI: 10.1103/physrevlett.85.4221] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/08/2000] [Indexed: 05/23/2023]
Abstract
The neutron-proton differential flow is shown to be a very useful probe of the isospin-dependence of the nuclear equation of state (EOS). This novel approach utilizes constructively both the isospin fractionation and the nuclear collective flow as well as their sensitivities to the isospin-dependence of the nuclear EOS. It also avoids effectively uncertainties associated with other dynamical ingredients of heavy-ion reactions at intermediate energies.
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Affiliation(s)
- BA Li
- Department of Chemistry and Physics, Arkansas State University, P.O. Box 419, State University, Arkansas 72467-0419, USA
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35
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Page D, Prakash M, Lattimer JM, Steiner AW. Prospects of detecting baryon and quark superfluidity from cooling neutron stars. PHYSICAL REVIEW LETTERS 2000; 85:2048-2051. [PMID: 10970460 DOI: 10.1103/physrevlett.85.2048] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/09/2000] [Indexed: 05/23/2023]
Abstract
Baryon and quark superfluidity in the cooling of neutron stars are investigated. Future observations will allow us to constrain combinations of the neutron or Lambda-hyperon pairing gaps and the star's mass. However, in a hybrid star with a mixed phase of hadrons and quarks, quark gaps larger than a few tenths of an MeV render quark matter virtually invisible for cooling. If the quark gap is smaller, quark superfluidity could be important, but its effects will be nearly impossible to distinguish from those of other baryonic constituents.
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Affiliation(s)
- D Page
- Instituto de Astronomia, UNAM, Mexico D.F. 04510, Mexico
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36
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Voskresensky DN, Khodel VA, Zverev MV, Clark JW. Rearrangement of the Fermi Surface of Dense Neutron Matter and the Direct Urca Cooling of Neutron Stars. THE ASTROPHYSICAL JOURNAL 2000; 533:L127-L130. [PMID: 10770706 DOI: 10.1086/312607] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/19/2000] [Accepted: 03/08/2000] [Indexed: 05/23/2023]
Abstract
It is proposed that a rearrangement of single-particle degrees of freedom may occur in a portion of the quantum-fluid interior of a neutron star. Such a rearrangement is associated with the pronounced softening of the spin-isospin collective mode which, under increasing density, leads to pion condensation. Arguments and estimates based on fundamental relations of many-body theory show that one realization of this phenomenon could produce very rapid cooling of the star via a direct nucleon Urca process displaying a T5 dependence on temperature.
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37
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Yakovlev DG, Levenfish KP, Shibanov YA. Cooling of neutron stars and superfluidity in their cores. ACTA ACUST UNITED AC 1999. [DOI: 10.3367/ufnr.0169.199908a.0825] [Citation(s) in RCA: 45] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/01/2022]
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38
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Bandyopadhyay D, Chakrabarty S, Dey P, Pal S. Rapid cooling of magnetized neutron stars. Int J Clin Exp Med 1998. [DOI: 10.1103/physrevd.58.121301] [Citation(s) in RCA: 38] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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39
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Abstract
Because of the information they can yield about the equation of state of matter at extremely high densities and because they are one of the more possible sources of detectable gravitational waves, rotating relativistic stars have been receiving significant attention in recent years. We review the latest theoretical and numerical methods for modeling rotating relativistic stars, including stars with a strong magnetic field and hot proto-neutron stars. We also review nonaxisymmetric oscillations and instabilities in rotating stars and summarize the latest developments regarding the gravitational wave-driven (CFS) instability in both polar and axial quasi-normal modes.
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Affiliation(s)
- Nikolaos Stergioulas
- Department of Physics, University of Wisconsin-Milwaukee, PO Box 413, Milwaukee, WI 53201 USA
- Max Planck Institute for Gravitational Physics (Albert-Einstein-Institute), D-14473 Potsdam, Germany
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Lazzari G, Pizzochero PM, Broglia RA. Superfluidity and thermal response of neutron star crusts. PHYSICAL REVIEW. D, PARTICLES AND FIELDS 1996; 53:4226-4231. [PMID: 10020418 DOI: 10.1103/physrevd.53.4226] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
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42
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Schaffner J, Mishustin IN. Hyperon-rich matter in neutron stars. PHYSICAL REVIEW. C, NUCLEAR PHYSICS 1996; 53:1416-1429. [PMID: 9971080 DOI: 10.1103/physrevc.53.1416] [Citation(s) in RCA: 12] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/22/2023]
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43
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Knorren R, Prakash M, Ellis PJ. Strangeness in hadronic stellar matter. PHYSICAL REVIEW. C, NUCLEAR PHYSICS 1995; 52:3470-3482. [PMID: 9970892 DOI: 10.1103/physrevc.52.3470] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/22/2023]
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