Search results for " stars: oscillations"

showing 2 items of 2 documents

QPO emission from moving hot spots on the surface of neutron stars: a model

2009

We present recent results of 3D magnetohydrodynamic simulations of neutron stars with small misalignment angles, as regards the features in lightcurves produced by regular movements of the hot spots during accretion onto the star. In particular, we show that the variation of position of the hot spot created by the infalling matter, as observed in 3D simulations, can produce high frequency Quasi Periodic Oscillations with frequencies associated with the inner zone of the disk. Previously reported simulations showed that the usual assumption of a fixed hot spot near the polar region is valid only for misalignment angles relatively large. Otherwise, two phenomena challenge the assumption: one …

High Energy Astrophysical Phenomena (astro-ph.HE)PhysicsAstrophysics::High Energy Astrophysical PhenomenaMonte Carlo methodEquatorFOS: Physical sciencesAstronomy and Astrophysicsaccretion accretion discs instabilities MHD stars: magnetic fields stars: neutron stars: oscillationsAstrophysics01 natural sciencesAccretion (astrophysics)Neutron starAccretion rateSettore FIS/05 - Astronomia E AstrofisicaSpace and Planetary Science0103 physical sciencesPolarAstrophysics::Solar and Stellar AstrophysicsMagnetohydrodynamic driveAstrophysics::Earth and Planetary AstrophysicsQuasi periodic010306 general physicsAstrophysics - High Energy Astrophysical Phenomena010303 astronomy & astrophysics
researchProduct

Rotational effects on the oscillation frequencies of newly born proto-neutron stars

2003

In this paper we study the effects of rotation on the frequencies of the quasi-normal modes of a proto-neutron star (PNS) born in a gravitational collapse during the first minute of life. Our analysis starts a few tenths of seconds after the PNS formation, when the stellar evolution can be described by a sequence of equilibrium configurations. We use the evolutionary models developed by Pons et al. (1999; 2001) that describe how a non rotating star cools down and contracts while neutrino diffusion and thermalization processes dominate the stellar dynamics. For assigned values of the evolution time, we set the star into slow rotation and integrate the equations of stellar perturbations in th…

relativityFOS: Physical sciencesmethods : numericalAstrophysicsAstrophysicsInstabilitystars : oscillationsmethods: numericalstars: neutronstars: rotationstars : rotationStellar dynamicsGravitational collapseAstrophysics::Solar and Stellar AstrophysicsTime domainStellar evolutionPhysicsgravitational waves; methods : numerical; methods: numerical; relativity; stars : neutron; stars : oscillations; stars : rotation; stars: neutron; stars: oscillations; stars: rotationAstrophysics (astro-ph)Astronomy and Astrophysicsstars : neutronNeutron stargravitational wavesSpace and Planetary ScienceFrequency domainstars: oscillationsAstrophysics::Earth and Planetary AstrophysicsNeutrinoMonthly Notices of the Royal Astronomical Society
researchProduct