Phase transition phenomenology with nonparametric representations of the neutron star equation of state

被引:25
作者
Essick, Reed [1 ,2 ,3 ,4 ]
Legred, Isaac [5 ,6 ]
Chatziioannou, Katerina [5 ,6 ]
Han, Sophia [7 ,8 ,9 ,10 ]
Landry, Philippe [1 ]
机构
[1] Univ Toronto, Canadian Inst Theoret Astrophys, Toronto, ON M5S 3H8, Canada
[2] Univ Toronto, Dept Phys, Toronto, ON M5S 1A7, Canada
[3] Univ Toronto, David A Dunlap Dept Astron, Toronto, ON M5S 3H4, Canada
[4] Perimeter Inst Theoret Phys, Waterloo, ON N2L 2Y5, Canada
[5] CALTECH, TAPIR, Pasadena, CA 91125 USA
[6] CALTECH, LIGO Lab, Pasadena, CA 91125 USA
[7] Shanghai Jiao Tong Univ, Tsung Dao Lee Inst, Shanghai 200240, Peoples R China
[8] Shanghai Jiao Tong Univ, Sch Phys & Astron, Shanghai 200240, Peoples R China
[9] Univ Washington, Inst Nucl Theory, Seattle, WA 98195 USA
[10] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA
基金
美国国家科学基金会;
关键词
MASSES;
D O I
10.1103/PhysRevD.108.043013
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Astrophysical observations of neutron stars probe the structure of dense nuclear matter and have the potential to reveal phase transitions at high densities. Most recent analyses are based on parametrized models of the equation of state with a finite number of parameters and occasionally include extra parameters intended to capture phase-transition phenomenology. However, such models restrict the types of behavior allowed and may not match the true equation of state. We introduce a complementary approach that extracts phase transitions directly from the equation of state without relying on, and thus being restricted by, an underlying parametrization. We then constrain the presence of phase transitions in neutron stars with astrophysical data. Current pulsar mass, tidal deformability, and mass-radius measurements disfavor only the strongest of possible phase transitions (latent energy per particle greater than or similar to 100 MeV). Weaker phase transitions are consistent with observations. We further investigate the prospects for measuring phase transitions with future gravitational-wave observations and find that catalogs of O(100) events will (at best) yield Bayes factors of similar to 10:1 in favor of phase transitions even when the true equation of state contains very strong phase transitions. Our results reinforce the idea that neutron star observations will primarily constrain trends in macroscopic properties rather than detailed microscopic behavior. Fine-tuned equation of state models will likely remain unconstrained in the near future.
引用
收藏
页数:30
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