Neutron stars and the cosmological constant problem

被引：0

作者：

Ventagli, Giulia ^{[1
]}

Fernandes, Pedro G. S. ^{[2
,3
]}

Maselli, Andrea ^{[4
,5
]}

Padilla, Antonio ^{[6
,7
]}

Sotiriou, Thomas P. ^{[6
,7
,8
]}

机构：

[1] Czech Acad Sci, Inst Phys, CEICO, Slovance 2, Prague 8, Czech Republic

[2] Univ Southern Denmark, Origins CP3, Campusvej 55, DK-5230 Odense M, Denmark

[3] Heidelberg Univ, Inst fir Theoret Phys, Philosophenweg 16, D-69120 Heidelberg, Germany

[4] Gran Sasso Sci Inst GSSI, I-67100 Laquila, Italy

[5] INFN, Lab Nazl Gran Sasso, I-67100 Assergi, Italy

[6] Univ Nottingham, Nottingham Ctr Grav, Univ Pk, Nottingham NG7 2RD, England

[7] Univ Nottingham, Sch Phys & Astron, Univ Pk, Nottingham NG7 2RD, England

[8] Univ Nottingham, Sch Math Sci, Univ Pk, Nottingham NG7 2RD, England

来源：

PHYSICAL REVIEW D | 2025年 / 111卷 / 02期

关键词：

ROTATING RELATIVISTIC STARS; EQUATION-OF-STATE; SKYRME PARAMETRIZATION; SUBNUCLEAR; MODELS; MATTER;

D O I：

10.1103/PhysRevD.111.024001

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Phase transitions can play an important role in the cosmological constant problem, allowing the underlying vacuum energy, and therefore the value of the cosmological constant, to change. Deep within the core of neutron stars, the local pressure may be sufficiently high to trigger the QCD phase transition, thus generating a shift in the value of the cosmological constant. The gravitational effects of such a transition should then be imprinted on the properties of the star. Working in the framework of general relativity, we provide a new model of the stellar interior, allowing for a QCD and a vacuum energy phase transition. We determine the impact of a vacuum energy jump on mass-radius relations, tidal deformabilityradius relations, I-Love-Q relations, and on the combined tidal deformability measured in neutron star binaries.

引用

页数：21

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