Rotating superdense configurations: pulsars and their astrophysical manifestations

Sedrakian, D. M.; Чубарян, Э. В.

doi:10.1007/s10511-009-9093-1

Cited by 1 publication

(2 citation statements)

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“…The rotation of the star modifies the metric and thus the rotation frequency in the local inertial frame, which we denote by ω L . Slowly rotating stars admit perturbative approach, where the small parameter is the ratio of the rotational kinetic energy to the gravitational binding energy [154,155,156,157,158,159]. The angular velocity of a slowly rotating star obeys the following equation (r 4 jω…”

Section: Stellar Modelsmentioning

confidence: 99%

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The physics of dense hadronic matter and compact stars

Sedrakian

2007

Progress in Particle and Nuclear Physics

125

109

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This review describes the properties of hadronic phases of dense matter in compact stars. The theory is developed within the method of real-time Green's functions and is applied to study of baryonic matter at and above the saturation density. The non-relativistic and covariant theories based on continuum Green's functions and the T -matrix and related approximations to the selfenergies are reviewed. The effects of symmetry energy, onset of hyperons and meson condensation on the properties of stellar configurations are demonstrated on specific examples. Neutrino interactions with baryonic matter are introduced within a kinetic theory. We concentrate on the classification, analysis and first principle derivation of neutrino radiation processes from unpaired and superfluid hadronic phases. We then demonstrate how neutrino radiation rates from various microscopic processes affect the macroscopic cooling of neutron stars and how the observed X-ray fluxes from pulsars constrain the properties of dense hadronic matter. Contents IntroductionNeutron stars are born in a gravitational collapse of luminous stars whose core mass exceeds the Chandrasekhar limit for a self-gravitating body supported by degeneracy pressure of electron gas [1]. Being the densest observable bodies in our universe they open a window on the physics of matter under extreme conditions of high densities, pressures and strong electromagnetic and gravitational fields. Most of the known pulsars are isolated objects which emit radio-waves at frequencies 10 8 − 10 10 Hz, which are pulsed at the rotation frequency of the star. Young objects, like the pulsar in the Crab nebula, are also observed through X-rays that are emitted from their surface as the star radiates away its thermal energy. Relativistic magnetospheres of young pulsars emit detectable non-thermal optical and gamma radiation; they could be sources of high-energy elementary particles. Neutron stars in the binaries are powered by the energy of matter accreted from companion star.The radio observations of pulsars stretch back to 1967 when the first pulsar was discovered. Since then, the observational pulsar astronomy has been extremely important to the fundamental physics and 2 astrophysics, which is evidenced by two Nobel awards, one for the discovery of pulsars (Hewish 1974) [2], the other for the discovery of the first neutron star -neutron star binary pulsar (Hulse and Taylor, 1993) [3] whose orbital decay confirmed the gravitational radiation in full agreement with Einstein's General Theory of Relativity. The measurements of neutron star (NS) masses in binaries provide one of the most stringent constraint on properties of the superdense matter. The timing observations of the millisecond pulsars set an upper limit on the angular momentum that can be accommodated by a stable NS -a limit that can potentially constrains the properties of dense matter. Noise and rotational anomalies that are superimposed on the otherwise highly stable rotation of these objects provide a clue to the ...

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Section: Stellar Modelsmentioning

confidence: 99%

“…3.1) translates into expansion of the polarization tensor in particle-hole loops. The one-body processes (157) and (158) are described by the one-loop polarization tensor, the two-baryon processes, e.g. Eqs.…”

Section: Polarization Tensors Of Hadronic Mattermentioning

confidence: 99%