Neutron stars and the dense matter equation of state
Creators
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1.
California Institute of Technology
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2.
National Academy of Sciences
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3.
United States Naval Research Laboratory
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4.
Los Alamos National Laboratory
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5.
Pennsylvania State University
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6.
University of Tennessee at Knoxville
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7.
Oak Ridge National Laboratory
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8.
University of Amsterdam
Abstract
The past two decades have witnessed tremendous progress in understanding the properties of neutron stars, their maximum mass and radii, and the properties of the dense matter in their cores, made possible by electromagnetic observations of neutron stars and the detection of gravitational waves from their mergers. These observations have provided novel constraints on neutron-star structure that are intimately related to the properties of dense neutron-rich matter described by the nuclear equation of state. Nevertheless, constraining the equation of state over the wide range of densities probed by astrophysical observations is still challenging, as the physics involved is broad and the system spans many orders of magnitude in density. Theoretical approaches to calculate and model the neutron-star equation of state in various regimes of densities are reviewed, and the related consequent properties of neutron stars are discussed. How the equation of state at low densities can be calculated from nuclear interactions that are constrained and benchmarked by nuclear experiments is described. Neutron-star observations, with a particular emphasis on information provided by gravitational-wave signals and electromagnetic observations, are reviewed. Finally, future challenges and opportunities in the field are discussed.
Copyright and License
© 2025 American Physical Society.
Acknowledgement
K. C. acknowledges support from the U.S. Department of Energy under Award No. DE-SC0023101 and the Sloan Foundation. A. L. W. acknowledges support from ERC Consolidator Grant No. 865768 AEONS and NWO ENW-XL Grant No. OCENW.XL21.XL21.038, “Probing the phase diagram of quantum chromodynamics.” D. R. acknowledges funding from the U.S. Department of Energy, Office of Science, Division of Nuclear Physics, under Awards No. DE-SC0021177 and No. DE-SC0024388; from the National Science Foundation under Grants No. PHY-2011725, No. PHY-2020275, No. PHY-2116686, and No. AST-2108467; and from the Sloan Foundation. The work of S. G. and I. T. is supported by the U.S. Department of Energy, Office of Nuclear Physics, under Contract No. DE-AC52-06NA25396, and by the Office of Advanced Scientific Computing Research, Scientific Discovery, through the Advanced Computing (SciDAC) NUCLEI program. S. G. is also supported by the Network for Neutrinos, Nuclear Astrophysics and Symmetries (N3AS), through National Science Foundation Physics Frontier Center Award No. PHY-2020275. H. T. C. acknowledges support from the U.S. Naval Research Laboratory, where basic research in pulsar astronomy is supported by ONR 6.1 funding. A. W. S. acknowledges support from NSF Grants No. PHY-2116686 and No. AST 22-06322 and the U.S. DOE, Office of Nuclear Physics.
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Additional details
Additional titles
- Alternative title
- Neutron stars and the dense matter equation of state: from microscopic theory to macroscopic observations
Related works
- Is new version of
- Discussion Paper: arXiv:2407.11153 (arXiv)
Funding
- United States Department of Energy
- DE-SC0023101
- Alfred P. Sloan Foundation
- European Research Council
- 865768 AEONS
- Dutch Research Council
- OCENW.XL21.XL21.038
- United States Department of Energy
- DE-SC0021177
- United States Department of Energy
- DE-SC0024388
- National Science Foundation
- PHY-2011725
- National Science Foundation
- PHY-2020275
- National Science Foundation
- PHY-2116686
- National Science Foundation
- AST-2108467
- United States Department of Energy
- DE-AC52-06NA25396
- United States Naval Research Laboratory
- National Science Foundation
- AST 22-06322