TY - JOUR
ID - 1752
TI - The equilibrium configuration of rotating neutron stars
JO - Iranian Journal of Physics Research
JA - IJPR
LA - en
SN - 1682-6957
AU - Riahi, R
AU - Kalantari, S Z
AD - Department of Physics, Shahrekord Branch, Islamic Azad University, Shahrekord, Iran
AD - Department of Physics, Isfahan University of Technology, Isfahan, Iran
Y1 - 2022
PY - 2022
VL - 21
IS - 4
SP - 765
EP - 774
KW - rotating neutron stars
KW - Mean Field Approximation
KW - equation of state
KW - density-dependent interaction
KW - Einstein field equations
DO - 10.47176/ijpr.21.4.21011
N2 - Using the density-dependent equation of states to describe the matter of rotating neutron stars, we construct equilibrium configurations of rotating neutron stars. The interaction between baryons is described by exchanging the scalar and vector mesons in the relativistic mean-field theory. The mesons coupling coefficients are functions of the environmental density. The sequence of equilibrium states is calculated for the four frequencies observed for rotating neutron stars namely, 25, 317, 716, and 1122 Hz. These sequences are constrained by static, Keplerian (mass-shedding sequence), and secular axisymmetric instability sequences. This allows the radius and mass range of the stars will be obtained in each of the models. We can also calculate the parameters of the fastest rotating star described by each model.
UR - https://ijpr.iut.ac.ir/article_1752.html
L1 - https://ijpr.iut.ac.ir/article_1752_058f6b585235b58050d529a4aa58501d.pdf
ER -