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Pacilio C, Maselli A, Fasano M, Pani P. Ranking Love Numbers for the Neutron Star Equation of State: The Need for Third-Generation Detectors. PHYSICAL REVIEW LETTERS 2022; 128:101101. [PMID: 35333071 DOI: 10.1103/physrevlett.128.101101] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 04/26/2021] [Revised: 01/22/2022] [Accepted: 02/10/2022] [Indexed: 06/14/2023]
Abstract
Gravitational-wave measurements of the tidal deformability in neutron-star binary coalescences can be used to infer the still unknown equation of state (EOS) of dense matter above the nuclear saturation density. By employing a Bayesian-ranking test, we quantify the ability of current and future gravitational-wave observations to discriminate among families of nuclear-physics based EOS which differ in particle content and ab initio microscopic calculations. While the constraining power of GW170817 is limited, we show that even twenty coalescences detected by LIGO-Virgo at design sensitivity are not enough to discriminate between EOS with similar softness but distinct microphysics. However, just a single detection with a third-generation detector such as the Einstein Telescope or Cosmic Explorer will rule out several families of EOS with very strong statistical significance and can discriminate among models which feature similar softness, hence, constraining the properties of nuclear matter to unprecedented levels.
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Affiliation(s)
- Costantino Pacilio
- Dipartimento di Fisica, "Sapienza" Università di Roma, Piazzale Aldo Moro 5, 00185 Roma, Italy
- INFN, Sezione di Roma, Piazzale Aldo Moro 2, 00185 Roma, Italy
| | - Andrea Maselli
- Gran Sasso Science Institute (GSSI), I-67100 L'Aquila, Italy
- INFN, Laboratori Nazionali del Gran Sasso, I-67100 Assergi, Italy
| | - Margherita Fasano
- Dipartimento di Fisica, "Sapienza" Università di Roma, Piazzale Aldo Moro 5, 00185 Roma, Italy
| | - Paolo Pani
- Dipartimento di Fisica, "Sapienza" Università di Roma, Piazzale Aldo Moro 5, 00185 Roma, Italy
- INFN, Sezione di Roma, Piazzale Aldo Moro 2, 00185 Roma, Italy
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Ghoroku K, Kashiwa K, Nakano Y, Tachibana M, Toyoda F. Equation of state for holographic nuclear matter as instanton gas. EPJ WEB OF CONFERENCES 2022. [DOI: 10.1051/epjconf/202225807005] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
In a holographic model, which was used to investigate the color superconducting phase of QCD, a dilute gas of instantons is introduced to study the nuclear matter. The free energy of the nuclear matter is computed as a function of the baryon chemical potential in the probe approximation. Then the equation of state is obtained at low temperature. Using the equation of state for the nuclear matter, the Tolman-Oppenheimer-Volkov equations for a cold compact star are solved. We find the mass-radius relation of the star, which is similar to the one for quark star. This similarity implies that the instanton gas given here is a kind of self-bound matter.
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Estimating the Variation of Neutron Star Observables by Dense Symmetric Nuclear Matter Properties. UNIVERSE 2019. [DOI: 10.3390/universe5060153] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.4] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
Recent multi-channel astrophysics observations and the soon-to-be published new measured electromagnetic and gravitation data provide information on the inner structure of the compact stars. These macroscopic observations can significantly increase our knowledge on the neutron star enteriors, providing constraints on the microscopic physical properties. On the other hand, due to the masquarade problem, there are still uncertainties on the various nuclear-matter models and their parameters as well. Calculating the properties of the dense nuclear matter, effective field theories are the most widely-used tools. However, the values of the microscopical parameters need to be set consistently to the nuclear and astrophysical measurements. In this work, we investigate how uncertainties are induced by the variation of the microscopical parameters. We use a symmetric nuclear matter in an extended σ - ω model to see the influence of the nuclear matter parameters. We calculate the dense matter equation of state and give the mass-radius diagram for a simplistic neutron star model. We present that the Landau mass and compressibility modulus of the nuclear matter have definite linear relation to the maximum mass of a Schwarzschild neutron star.
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Yagi K, Yunes N. I-Love-Q: Unexpected Universal Relations for Neutron Stars and Quark Stars. Science 2013; 341:365-8. [DOI: 10.1126/science.1236462] [Citation(s) in RCA: 274] [Impact Index Per Article: 24.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- Kent Yagi
- Department of Physics, Montana State University, Bozeman, MT 59717, USA
| | - Nicolás Yunes
- Department of Physics, Montana State University, Bozeman, MT 59717, USA
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Ozel F. Surface emission from neutron stars and implications for the physics of their interiors. REPORTS ON PROGRESS IN PHYSICS. PHYSICAL SOCIETY (GREAT BRITAIN) 2013; 76:016901. [PMID: 23234858 DOI: 10.1088/0034-4885/76/1/016901] [Citation(s) in RCA: 10] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/27/2023]
Abstract
Neutron stars are associated with diverse physical phenomena that take place in conditions characterized by ultrahigh densities as well as intense gravitational, magnetic and radiation fields. Understanding the properties and interactions of matter in these regimes remains one of the challenges in compact object astrophysics. Photons emitted from the surfaces of neutron stars provide direct probes of their structure, composition and magnetic fields. In this review, I discuss in detail the physics that governs the properties of emission from the surfaces of neutron stars and their various observational manifestations. I present the constraints on neutron star radii, core and crust composition, and magnetic field strength and topology obtained from studies of their broadband spectra, evolution of thermal luminosity, and the profiles of pulsations that originate on their surfaces.
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Affiliation(s)
- Feryal Ozel
- Department of Astronomy, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA.
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Faber JA, Rasio FA. Binary Neutron Star Mergers. LIVING REVIEWS IN RELATIVITY 2012; 15:8. [PMID: 28163622 PMCID: PMC5255524 DOI: 10.12942/lrr-2012-8] [Citation(s) in RCA: 15] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Accepted: 05/22/2012] [Indexed: 05/27/2023]
Abstract
We review the current status of studies of the coalescence of binary neutron star systems. We begin with a discussion of the formation channels of merging binaries and we discuss the most recent theoretical predictions for merger rates. Next, we turn to the quasi-equilibrium formalisms that are used to study binaries prior to the merger phase and to generate initial data for fully dynamical simulations. The quasi-equilibrium approximation has played a key role in developing our understanding of the physics of binary coalescence and, in particular, of the orbital instability processes that can drive binaries to merger at the end of their lifetimes. We then turn to the numerical techniques used in dynamical simulations, including relativistic formalisms, (magneto-)hydrodynamics, gravitational-wave extraction techniques, and nuclear microphysics treatments. This is followed by a summary of the simulations performed across the field to date, including the most recent results from both fully relativistic and microphysically detailed simulations. Finally, we discuss the likely directions for the field as we transition from the first to the second generation of gravitational-wave interferometers and while supercomputers reach the petascale frontier.
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Affiliation(s)
- Joshua A. Faber
- Center for Computational Relativity and Gravitation and School of Mathematical Sciences, Rochester Institute of Technology, 85 Lomb Memorial Drive, Rochester, NY 14623 USA
| | - Frederic A. Rasio
- Center for Interdisciplinary Exploration and Research in Astrophysics, and Department of Physics & Astronomy, Northwestern University, 2145 Sheridan Road, Evanston, IL 60208 USA
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Pagliara G, Hempel M, Schaffner-Bielich J. New possible quark-hadron mixed phase in protoneutron stars. PHYSICAL REVIEW LETTERS 2009; 103:171102. [PMID: 19905743 DOI: 10.1103/physrevlett.103.171102] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/16/2009] [Indexed: 05/28/2023]
Abstract
The transition from hadronic to quark matter at high density is a strong first order phase transition if the surface tension between the two phases is large. While this implies a constant-pressure mixed phase in cold neutron star matter this is not the case for the hot and lepton rich matter of protoneutron stars. By considering the global conservation of lepton number during the stage of neutrino trapping, we show that a new mixed phase with non-constant pressure could appear in protoneutron stars and it would gradually disappear during deleptonization. We discuss the peculiar properties of this mixed phase and its possible significant effects on the evolution of protoneutron stars and their neutrino emission.
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Affiliation(s)
- G Pagliara
- Institut für Theoretische Physik, Ruprecht-Karls-Universität, Philosophenweg 16, D-69120, Heidelberg, Germany
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Burgio GF, Plumari S. Structure of hybrid protoneutron stars within the Nambu–Jona-Lasinio model. Int J Clin Exp Med 2008. [DOI: 10.1103/physrevd.77.085022] [Citation(s) in RCA: 16] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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Pons JA, Steiner AW, Prakash M, Lattimer JM. Evolution of proto-neutron stars with quarks. PHYSICAL REVIEW LETTERS 2001; 86:5223-5226. [PMID: 11384463 DOI: 10.1103/physrevlett.86.5223] [Citation(s) in RCA: 11] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/01/2001] [Indexed: 05/23/2023]
Abstract
Neutrino fluxes from proto-neutron stars with and without quarks are studied. Observable differences become apparent after 10-20 s of evolution. Sufficiently massive stars containing negatively charged, strongly interacting, particles collapse to black holes during the first minute of evolution. Since the neutrino flux vanishes when a black hole forms, this is the most obvious signal that quarks (or other types of strange matter) have appeared. The metastability time scales for stars with quarks are intermediate between those containing hyperons and kaon condensates.
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Affiliation(s)
- J A Pons
- Department of Physics and Astronomy, SUNY at Stony Brook, Stony Brook, New York 11794-3800, USA
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Epsztein Grynberg S, Nemes MC, Rodrigues H, Chiapparini M, Duarte SB, Blin AH, Hiller B. Neutrino trapping and hybrid protoneutron star formation. Int J Clin Exp Med 2000. [DOI: 10.1103/physrevd.62.123003] [Citation(s) in RCA: 6] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
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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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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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Abstract
The unusual hard x-ray burster GRO J1744-28 recently discovered by the Compton Gamma-Ray Observatory can be modeled as a strange star with a dipolar magnetic field of </=10(11) gauss. According to this model, when the accreted mass of the star exceeds some critical mass, its crust breaks, resulting in the conversion of the accreted matter into strange matter and a release of energy. Subsequently, a fireball forms and expands relativistically outward. The expanding fireball interacts with the surrounding interstellar medium, causing its kinetic energy to be radiated in shock waves and producing a burst of x-ray radiation. The burst energy, duration, interval, and spectrum derived from such a model are consistent with the observations of GRO J1744-28.
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Affiliation(s)
- KS Cheng
- K. S. Cheng, Department of Physics, University of Hong Kong, Hong Kong, China. Z. G. Dai, Department of Astronomy, Nanjing University, Nanjing 210093, China. D. M. Wei, Purple Mountain Observatory, Nanjing 210008, China. T. Lu, Department of As
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Savage MJ, Wise MB. Hyperon masses in nuclear matter. PHYSICAL REVIEW. D, PARTICLES AND FIELDS 1996; 53:349-354. [PMID: 10019796 DOI: 10.1103/physrevd.53.349] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
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