Abstract:Employing the Quark Mass Denisity-and temperature-dependent model and the Hartle's method, We have studied the slowly rotating strange star with uniform angular velocity. The mass-radius relation, the moment of inertia and the frame dragging for different frequencies are given. We found that we cannot use the strange star to solve the challenges of Stella and Vietri for the horizontal branch oscillations and the moment of inertia I 45 /(M/M s ) > 2.3. Furthermore, we extended the Hartle's method to study the d… Show more
“…The reason is that the crust is not considered in Ref. [16], so similar behavior is observed in our Fig.2. When the star is very small, the crust thickness becomes important, which will change the shape of the M -R curve significantly.…”
Section: Comparison Between Different Starssupporting
confidence: 73%
“…One significant distinctness of the strange quark star is that its M -R curve has different direction from the other three types at small M , as was shown in Fig.2 of Ref. [16]. The reason is that the crust is not considered in Ref.…”
Section: Comparison Between Different Starsmentioning
The equations of state for neutron matter, strange and non-strange hadronic matter in a chiral SU (3) quark mean field model are applied in the study of slowly rotating neutron stars and hadronic stars. The radius, mass, moment of inertia, and other physical quantities are carefully examined. The effect of nucleon crust for the strange hadronic star is exhibited. Our results show the rotation can increase the maximum mass of compact stars significantly. For big enough mass of pulsar which can not be explained as strange hadronic star, the theoretical approaches to increase the maximum mass are addressed.
“…The reason is that the crust is not considered in Ref. [16], so similar behavior is observed in our Fig.2. When the star is very small, the crust thickness becomes important, which will change the shape of the M -R curve significantly.…”
Section: Comparison Between Different Starssupporting
confidence: 73%
“…One significant distinctness of the strange quark star is that its M -R curve has different direction from the other three types at small M , as was shown in Fig.2 of Ref. [16]. The reason is that the crust is not considered in Ref.…”
Section: Comparison Between Different Starsmentioning
The equations of state for neutron matter, strange and non-strange hadronic matter in a chiral SU (3) quark mean field model are applied in the study of slowly rotating neutron stars and hadronic stars. The radius, mass, moment of inertia, and other physical quantities are carefully examined. The effect of nucleon crust for the strange hadronic star is exhibited. Our results show the rotation can increase the maximum mass of compact stars significantly. For big enough mass of pulsar which can not be explained as strange hadronic star, the theoretical approaches to increase the maximum mass are addressed.
“…and when T T C , m q = 0, m s,s = m s0 , This quark mass density-and temperature-dependent model (QMDTD) has been employed to discuss the properties of strange quark matter [14,16], the dibaryon system [19], and the strange quark star [20,21]. Instead of the correspondence of MIT bag to the QMDD model, we have proved that QMDTD model mimicks the Freidberg-Lee (FL) soliton bag model [22,23].…”
We present an improved quark mass density-dependent model with the nonlinear scalar sigma field and the ω-meson field. By comparing with the quark-meson coupling model, we show that our model can successfully describe saturation properties, the equation of state, the compressibility and the effective nuclear mass of nuclear matter under the mean field approximation.
“…many physical properties of strange quark matter [12,13,14,15,16,17,18,19,20,21,22,23,24,25] and strange quark star [26,27] have been studied, and the results are in good agreement with those given by MIT bag model [28].…”
Section: Introductionmentioning
confidence: 57%
“…(31) also conflicts with the requirement in Eq. (27), then the inconsistency of the traditional treatment with partial derivative is transparent.…”
Section: Inconsistency Of Traditional Thermodynamic Treatments Wimentioning
The ambiguities and inconsistencies in previous thermodynamic treatments for the quark mass density-dependent model are addressed. A new treatment is suggested to obtain the self-consistent results. A new independent variable of effective mass is introduced to make the traditional thermodynamic calculation with partial derivative still practicable. The contribution from physical vacuum has been discussed. We find that the properties of strange quark matter given by quark mass density-dependent model are nearly the same as those obtained by MIT bag model after considering the contribution of the physical vacuum.
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