Dynamical stability of the modified Tolman VII solution
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F47813059%3A19630%2F21%3AA0000126" target="_blank" >RIV/47813059:19630/21:A0000126 - isvavai.cz</a>
Result on the web
<a href="https://journals.aps.org/prd/abstract/10.1103/PhysRevD.103.104067" target="_blank" >https://journals.aps.org/prd/abstract/10.1103/PhysRevD.103.104067</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1103/PhysRevD.103.104067" target="_blank" >10.1103/PhysRevD.103.104067</a>
Alternative languages
Result language
angličtina
Original language name
Dynamical stability of the modified Tolman VII solution
Original language description
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.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
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Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2021
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Physical Review D
ISSN
2470-0010
e-ISSN
2470-0029
Volume of the periodical
103
Issue of the periodical within the volume
10
Country of publishing house
US - UNITED STATES
Number of pages
9
Pages from-to
„104067-1“-„104067-9“
UT code for WoS article
000655909400019
EID of the result in the Scopus database
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