Radial Oscillations of Quark Stars in Strong Magnetic Fields

Anand, J. D.; Devi, Nirmala; Gupta, V. K.; Singh, S. Somorendro

doi:10.1086/309144

Cited by 14 publications

(23 citation statements)

References 23 publications

(20 reference statements)

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“…Many aspects of SQM, such as radial oscillations of both rotating/nonrotating quark stars and bulk viscosity have been studied by various authors in this model. 7,20 At zero and very low temperatures the model works reasonably well and gives results for various quantities like the M -R relation and viscosity which are qualitatively similar to those obtained with bag model. Very recently Zhang and Su 21 have pointed out that the DDQM model suffers from a basic drawback, viz that it cannot be used to explain the process of quark deconfinement phase transition as quark confinement is permanent in this model.…”

Section: Introductionsupporting

confidence: 68%

Study of Proto Strange Stars in Temperature and Density Dependent Quark Mass Model

Gupta

Singh

et al. 2003

Int. J. Mod. Phys. D

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We report on the study of the mass-radius (M -R) relation and the radial oscillations of proto strange stars. For the quark matter we have employed the very recent modification, the temperature and density dependent quark mass model of the well known density dependent quark mass model. We find that the maximum mass the star can support increases significantly with the temperature of the star in this model which implies that transition to a black hole at the early stage of formation of the star is inhibited. As for the effect of the neutrinos, we find, contrary to expectation, that the values of mass, radius and oscillation frequencies are almost independent of the neutrino chemical potentials.

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Section: Introductionsupporting

confidence: 68%

Study of Proto Strange Stars in Temperature and Density Dependent Quark Mass Model

Gupta

Singh

et al. 2003

Int. J. Mod. Phys. D

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“…This confinement mechanism is almost the same as that of the MIT bag model. It has been shown by many authors that the thermodynamical properties given by QMDD model are similar to that of MIT bag model [14], and the M-R relation, viscosity radial oscillation of both rotating and non-rotating strange quark star described by QMDD model are qualitatively similar to those obtained with MIT bag model [10].…”

Section: Introductionsupporting

confidence: 64%

Slowly Rotating Proto Strange Stars in Quark Mass Density- And Temperature-Dependent Model

Shen

Zhang

Wang

et al. 2005

Int. J. Mod. Phys. A

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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 differential rotating strange star and found that the differential rotation is an effective way to get massive strange star.

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“…Several works have dealt with the problem of radial oscillations of strange and hybrid stars [3,11,12,13,14,16,15]. Väth & Chanmugan [3] showed that the oscillation frequencies of strange stars have qualitatively a different dependence on the central density compared with the case of neutron stars, as the periods of all modes go to zero when the central density of the strange star approaches its smallest possible value.…”

Section: Introductionmentioning

confidence: 99%

“…Their results showed that oscillation periods are similar to those obtained within the MIT bag model. Recently, Anand et al [13] studied the radial oscillations of magnetized…”

Section: Introductionmentioning

confidence: 99%

Radial Oscillations of Color Superconducting Quark Stars

Flores¹

2011

Proceedings of 4th School on Cosmic Rays and Astrophysics — PoS(CRA School)

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We investigate the effect of the color-flavor locking pairing pattern on the adiabatic radial oscillations of pure self-bound quark stars using an equation of state in the framework of the MIT Bag model. We integrate the equations of relativistic radial oscillations to determine the fundamental and the first excited oscillation modes for several parameterizations of the equation of state. For low mass stars we find that the period of the fundamental mode is typically ∼ 0.1 ms and has a small dependence on the parameters of the equation of state. For large mass stars the effect of color-flavor locking is related to the rise of the maximum mass with increasing ∆. As for unpaired quark stars, the period of the fundamental mode becomes divergent at the maximum mass but now the divergence is shifted to large masses for large values of the pairing gap ∆. As a consequence, the oscillation period is strongly affected by color superconductivity for stars with M 1.5 M . We further discuss the excitation and damping of the modes and their potential detectability during violent transient phenomena.4th School on Cosmic Rays and Astrophysics

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Radial Oscillations of Quark Stars in Strong Magnetic Fields

Cited by 14 publications

References 23 publications

Study of Proto Strange Stars in Temperature and Density Dependent Quark Mass Model

Study of Proto Strange Stars in Temperature and Density Dependent Quark Mass Model

Slowly Rotating Proto Strange Stars in Quark Mass Density- And Temperature-Dependent Model

Radial Oscillations of Color Superconducting Quark Stars

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