Dynamical stability of the modified Tolman VII solution

@article{51261,
   author = {Posada Aguirre, Nelson Camilo and Hladík, Jan and Stuchlík, Zdeněk},
   article_number = {10},
   doi = {http://dx.doi.org/10.1103/PhysRevD.103.104067},
   keywords = {modified Tolman VII solution; stability; radial oscilations},
   language = {eng},
   issn = {2470-0010},
   journal = {Physical Review D},
   title = {Dynamical stability of the modified Tolman VII solution},
   url = {https://journals.aps.org/prd/abstract/10.1103/PhysRevD.103.104067},
   volume = {103},
   year = {2021}
}

TY  - JOUR
ID  - 51261
AU  - Posada Aguirre, Nelson Camilo - Hladík, Jan - Stuchlík, Zdeněk
PY  - 2021
TI  - Dynamical stability of the modified Tolman VII solution
JF  - Physical Review D
VL  - 103
IS  - 10
SP  - "104067-1"-"104067-9"
EP  - "104067-1"-"104067-9"
SN  - 24700010
KW  - modified Tolman VII solution
KW  - stability
KW  - radial oscilations
UR  - https://journals.aps.org/prd/abstract/10.1103/PhysRevD.103.104067
N2  - 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.
ER  - 

POSADA AGUIRRE, Nelson Camilo, Jan HLADÍK a Zdeněk STUCHLÍK. Dynamical stability of the modified Tolman VII solution. \textit{Physical Review D}. roč.~103, č.~10, s.~''104067-1''-''104067-9'', 9 s. ISSN~2470-0010. doi:10.1103/PhysRevD.103.104067. 2021.