Neutron stars phenomenology with scalar–tensor inflationary attractors
In this work we shall study the implications of a subclass of E-models cosmological attractors, namely of a-attractors, on hydrodynamically stable slowly rotating neutron stars. Specifically, we shall present the Jordan frame theory of the a-attractors, and by using a conformal transformation we sha...
| Autores: | , |
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| Tipo de recurso: | artículo |
| Estado: | Versión aceptada para publicación |
| Fecha de publicación: | 2021 |
| País: | España |
| Institución: | Consejo Superior de Investigaciones Científicas (CSIC) |
| Repositorio: | DIGITAL.CSIC. Repositorio Institucional del CSIC |
| OAI Identifier: | oai:digital.csic.es:10261/249633 |
| Acceso en línea: | http://hdl.handle.net/10261/249633 |
| Access Level: | acceso abierto |
| Palabra clave: | Neutron stars Scalar-tension theories Alpha attractors Inflationary attractos |
| Sumario: | In this work we shall study the implications of a subclass of E-models cosmological attractors, namely of a-attractors, on hydrodynamically stable slowly rotating neutron stars. Specifically, we shall present the Jordan frame theory of the a-attractors, and by using a conformal transformation we shall derive the Einstein frame theory. We discuss the inflationary context of a-attractors in order to specify the allowed range of values for the free parameters of the model based on the latest cosmic-microwave-background-based Planck 2018 data. Accordingly, using the notation and physical units frequently used in theoretical astrophysics contexts, we shall derive the Tolman–Oppenheimer–Volkoff equations in the Einstein frame. Assuming a piecewise polytropic equation of state, the lowest density part of which shall be chosen to be the WFF1, or APR or the SLy EoS, we numerically solve the Tolman–Oppenheimer–Volkoff equations using a double shooting python-based “LSODA” numerical code. The resulting picture depends on the value of the parameter a characterizing the a-attractors. As we show, for large values of a, which do not produce a viable inflationary era, the M–R graphs are nearly identical to the general relativistic result, and these two are discriminated at large central densities values. Also, for large a-values, the WFF1 equation of state is excluded, due to the GW170817 constraints on the radius of an M∼1.6M neutron star, which must be larger than R=10.68km and on the radius corresponding to the maximum mass which must be larger than R=9.6km. In addition, the small a cases produce larger masses and radii compared to the general relativistic case and are compatible with the GW170817 constraints on the radii of neutron stars. A notable feature is that as the parameter a decreases, the radii of the static hydrodynamically stable neutron stars increase. Our results indicate deep and not yet completely understood connections between non-minimal inflationary attractors and neutron stars phenomenology in scalar–tensor theory. |
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