POSADA AGUIRRE, Nelson Camilo, Jan HLADÍK and Zdeněk STUCHLÍK. New interior model of neutron stars. Physical Review D. 2022, vol. 105, No 10, p. "104020-1"-"104020-10", 10 pp. ISSN 2470-0010. Available from: https://dx.doi.org/10.1103/PhysRevD.105.104020.
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Basic information
Original name New interior model of neutron stars
Authors POSADA AGUIRRE, Nelson Camilo (170 Colombia, belonging to the institution), Jan HLADÍK (203 Czech Republic, belonging to the institution) and Zdeněk STUCHLÍK (203 Czech Republic, belonging to the institution).
Edition Physical Review D, 2022, 2470-0010.
Other information
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher United States of America
Confidentiality degree is not subject to a state or trade secret
WWW URL
RIV identification code RIV/47813059:19630/22:A0000205
Organization unit Institute of physics in Opava
Doi http://dx.doi.org/10.1103/PhysRevD.105.104020
UT WoS 000807653700009
Keywords in English neutron stars;Tolman VII solution; tidal Love number;tidal deformability
Tags FÚ, RIV23
Tags International impact, Reviewed
Changed by Changed by: Mgr. Pavlína Jalůvková, učo 25213. Changed: 7/3/2023 13:54.
Abstract
The Tolman VII solution is considered by some as one of the few analytical solutions to Einstein???s equations, which describes approximately well the interior of neutron stars (NSs). This solution is characterized by the mass M, radius R, and an energy density that varies quadratically with the radial coordinate r. Recently, Jiang and Yagi proposed a modification of this solution, the so-called modified Tolman VII (MTVII) solution, by introducing an additional quartic term to the energy density radial profile. The MTVII solution is an approximate solution to Einstein???s equation, which includes a new parameter ?? that allows the solution to have a better agreement with the energy density profiles for realistic NSs. Here we consider the MTVII solution, showing that for certain values of the parameter ?? and compactness C this solution manifests a region of negative pressure near the surface which leads to negative values of the tidal Love number. To alleviate these drawbacks, we introduce an exact version of the MTVII solution obtained by solving numerically Einstein???s equations for the MTVII energy density profile. As an application of our new exact MTVII (EMTVII) solution, we calculate the tidal Love number and tidal deformability, as a function of C, for different values of the parameter ??. We find that the EMTVII solution predicts a positive tidal Love number for the whole range of allowed values of parameters ??C; ????, in agreement with previous results for realistic NSs.
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