POSADA AGUIRRE, Nelson Camilo, Jan HLADÍK and Zdeněk STUCHLÍK. Dynamical stability of the modified Tolman VII solution. Physical Review D. 2021, vol. 103, No 10, p. "104067-1"-"104067-9", 9 pp. ISSN 2470-0010. Available from: https://dx.doi.org/10.1103/PhysRevD.103.104067.
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Basic information
Original name Dynamical stability of the modified Tolman VII solution
Authors POSADA AGUIRRE, Nelson Camilo (170 Colombia, guarantor, 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, 2021, 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 Journal web
RIV identification code RIV/47813059:19630/21:A0000126
Organization unit Institute of physics in Opava
Doi http://dx.doi.org/10.1103/PhysRevD.103.104067
UT WoS 000655909400019
Keywords in English modified Tolman VII solution; stability; radial oscilations
Tags International impact, Reviewed
Changed by Changed by: RNDr. Jan Hladík, Ph.D., učo 25379. Changed: 18/6/2021 12:59.
Abstract
Studies of neutron stars are at their peak after the multimessenger observation of the binary merger event GW170817, which strongly constrains the stellar parameters like tidal deformability, masses, and radii. Although current and future observations will provide stronger limits on the neutron stars parameters, knowledge of explicit interior solutions to Einstein's equations, which connect observed parameters with the internal structure, are crucial to have a satisfactory description of the interior of these compact objects. A well-known exact solution, which has shown a relatively good approximation to a neutron star, is the Tolman VII solution. In order to provide a better fitting for the energy density profile, with the realistic equations of state for neutron stars, recently, Jiang and Yagi proposed a modified version of this model, which introduces an additional parameter a, reflecting the interplay of the quadratic and the newly added quartic term in the energy density profile. Here we study the dynamical stability of this modified Tolman VII solution using the theory of infinitesimal and adiabatic radial oscillations developed by Chandrasekhar. For this purpose, we determine values of the critical adiabatic index, for the onset of instability, considering configurations with varying compactness and a. We found that the new models are stable against radial oscillations for a considerable range of values of compactness and the new parameter a, thus supporting their applicability as a physically plausible approximation of realistic neutron stars.
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