Cosmological γ-ray bursts from a neutron star collapse induced by a primordial black hole

A detailed analysis is presented for a novel scenario in which gamma-ray bursts are of intergalactic origin and arise from the induced collapse of an isolated neutron star triggered by a primordial black hole. The energy released from the phase transition of accreted nucleon matter into a quark-gluon plasma is transferred by degenerate neutrinos to the star’s surface, where neutrinos annihilate into an electron-positron plasma and produce an inverted temperature layer that preserves a fire-ball from undue baryonic pollution. Possible observational tests include the absence of apparent cosmological time dilation, the location of γ-ray bursts primarily outside of galaxies, a specific shape of the log N-log S curve, with a large peak near red shift z∼10, the emission of ∼10⁻³ of the total energy in the form of 100-GeV photons, a bimodal distribution of durations, a very weak accompanying pulse of gravitational radiation, etc. Pis’ma Zh. éksp. Teor. Fiz. 70, No. 10, 642–647 (25 November 1999) Published in English in the original Russian journal. Edited by Steve Torstveit.     

Analytical formulas for calculating the blocking probability of a dynamic star network

Routing and wavelength assignment (RWA) has becomeone of the key problems for today's complicated wave-length division multiplexing (WDM) networks. In gen-eral, RWA can be classified either into the dynamiccase and the static case according to the wavelengthallocation[1], or into the star, ring and mesh networksaccording to the topology. Although extensive researchworks[2,3] have been done on the RWA and many al-gorithms have been developed for the case of dynamicrings[4], little has been …     

Effects of σ* and Φ mesons on the surface redshift of a neutron star

The effects of σ and Φ mesons on the surface redshift of a neutron star have been investigated within the framework of relativistic mean field theory for the baryon octet {n,p,Λ,Σ,Σ 0,Σ +,Ξ,Ξ 0 } system.It is found that compared with those without considering the contributions of σ and Φ mesons,the surface redshift decreases and that corresponding to the maximum value of the mass also decreases from 0.2540 to 0.2236,about by 12%.Meanwhile,it is also found that including σ and Φ mesons,the M/R and that corresponding to the maximum mass decrease.     

Quantum communication in spin star configuration

This paper considers a generalized spin star system which can be solved exactly, with the central spin-1/2 system embedded in an outer ring of N spin-1/2 particles（denoted as spin bath）. In this model, in addition to the central-outer interaction, each pair of nearest neighbour of the bath interacts within themselves. The general expressions of the eigenstates as well as the eigenvalues of the model are derived with the use of the symmetries of system. It analyses the quantum state transfer and the dynamical behaviour of entanglement created during quantum communication. It also analyses the efficiency of the configuration regarded as quantum phase covariant clone or decoherence model. Some interesting results are discovered concerning the properties of quantum communication in this model.     

A charged star with geometric Karmarkar condition

In this paper, we analyse an analytical solution of the Einstein–Maxwell field equations that considers matter with anisotropic pressures in a static and spherically symmetric geometry. We report the manner in which we obtained the solution, which is by means of the Karmarkar condition. For the model, we assume a state equation that describes the interaction of matter from quarks P =(c²ρ-4B_g)/3 and we consider the presence of electric charge, which can generate that the rad...     

Equivalence of star products on a symplectic manifold; an introduction to Deligne's Čech cohomology classes

These notes grew out of the Quantisation Seminar 1997–1998 on Deligne's paper [P. Deligne, Déformations de l'algèbre des fonctions d'une variété symplectique: Comparison entre Fedosov et De Wilde, Lecomte, Selecta Math. (New Series) 1 (1995) 667–697] and the lecture of the first author in the Workshop on Quantisation and Momentum Maps at the University of Warwich in December 1997.We recall the definitions of the cohomology classes introduced by Deligne for equivalence classes of differential star products on a symplectic manfold and show the properties of the relations between these classes by elementary methods based on Čech cohomology.     

Three-α-particle reactions in kinematical star conditions

The¹⁰B(d, )⁴He reaction was studied at energies between 4.2 and 6.6 MeV in kinematical plane-star conditions with special emphasis on sequential processes through the⁸Be state of 11.4 MeV. The results are compared with predictions of the Quebert model.Dedicated to Profs. Erich Schmid and Ivo laus on the occasion of their 60th birthdays     

Absorption of gamma-ray photons in a vacuum neutron star magnetosphere: II. The formation of “lightnings”

The absorption of a high-energy photon from the external cosmic gamma-ray background in the inner neutron star magnetosphere triggers the generation of a secondary electron-positron plasma and gives rise to a lightning—a lengthening and simultaneously expanding plasma tube. It propagates along magnetic fields lines with a velocity close to the speed of light. The high electron-positron plasma generation rate leads to dynamical screening of the longitudinal electric field that is provided not by charge separation but by electric current growth in the lightning. The lightning radius is comparable to the polar cap radius of a radio pulsar. The number of electron-positron pairs produced in the lightning in its lifetime reaches 10²⁸. The density of the forming plasma is comparable to or even higher than that in the polar cap regions of ordinary pulsars. This suggests that the radio emission from individual lightnings can be observed. Since the formation time of the radio emission is limited by the lightning lifetime, the possible single short radio bursts may be associated with rotating radio transients (RRATs).     

Re-research on the size of proto-neutron star in core-collapse supernova

The electron capture timescale may be shorter than hydrodynamic timescale in inner iron core of core-collapse supernova according to a recent new idea. Based on the new idea, this paper carries out a numerical simulation on supernova explosion for the progenitor model Ws15M. The numerical result shows that the size of proto-neutron star has a significant change （decrease about 20%）, which may affects the propagation of the shock wave and the final explosion energy.     

Antikaon condensation in neutron star matter with strong magnetic fields

We study the influence of strong magnetic fields on antikaon condensation in neutron star matter using the quark-meson coupling (QMC) model. The QMC model describes a nuclear many-body system as nonoverlapping MIT bags interacting through the self-consistent exchange of scalar and vector meson mean fields. It is found that the presence of strong magnetic fields alters the threshold density of antikaon condensation significantly. The results of the QMC model are compared with those obtained in a relativistic mean-field (RMF) model.     

Landau–Ginzburg theory for ‘star’-shaped droplets

ABSTRACT

Molecular simulations have shown that when a nano-drop comprising a single spherical central ion and a dielectric solvent is charged above a well-defined threshold, it acquires a stable star morphology. A linear continuum model of the ‘star’-shapes comprised electrostatic and surface energy is not sufficient to describe these shapes. We employ combined molecular dynamics, continuum electrostatics and macroscopic modelling in order to construct a unified free energy functional that describes the observed star-shaped droplets. We demonstrate that the Landau free energy coupled to the third-order Steinhardt invariant mimics the shapes of droplets detected in molecular simulations. Using the maximum likelihood technique we build a universal free energy functional that describes droplets for a range of Rayleigh fissility parameter. The analysis of the macroscopic free energy demonstrates the origin of the finite amplitude perturbations just above the Rayleigh limit. We argue that the presence of the finite amplitude perturbations precludes the use of the small parameter perturbation method for the analysis of the shapes above the Rayleigh limit of the corresponding spherical shape.     

Restoration of solar and star images with phase diversity-based blind deconvolution

The images recorded by a ground-based telescope are often degraded by atmospheric turbulence and the aberration of the optical system.Phase diversity-based blind deconvolution is an effective post-processing method that can be used to overcome the turbulence-induced degradation.The method uses an ensemble of short-exposure images obtained simultaneously from multiple cameras to jointly estimate the object and the wavefront distribution on pupil.Based on signal estimation theory and optimization theory,we derive the cost function and solve the large-scale optimization problem using a limited memory Broyden- Fletcher-Goldfarb-Shanno (L-BFGS) method.We apply the method to the turbulence-degraded images generated with computer,the solar images acquired with the swedish vacuum solar telescope (SVST,0.475 m) in La Palma and the star images collected with 1.2-m telescope in Yunnan Observatory.In order to avoid edge effect in the restoration of the solar images,a modified Hanning apodized window is adopted. The star image still can be restored when the defocus distance is measured inaccurately.The restored results demonstrate that the method is efficient for removing the effect of turbulence and reconstructing the point-like or extended objects.     

On Bose–Einstein condensation in Josephson junctions star graph arrays

We report on the evidence of anomalous currents in graph-shaped arrays of Josephson junctions along peculiar branches of the networks. The specific case of a star-shaped array is considered and the evidence of the anomalies is achieved by comparing the current-voltage characteristics of the arrays embedded in the star structure with those of “reference” arrays which are fabricated by-side the network structure and are dc-isolated from these. The experimental data are consistent with the results of a theoretical model predicting gradients of the populations of Cooper pairs on the islands situated in proximity of the central superconductive island as a result of a Bose–Einstein condensation process.     

Design and fabrication of the star coupler based on SOI material

A 1×25 star coupler is designed through calculation and beam propagation method (BPM) simulation. Improvement methods are focused on the design of the tapered waveguides in the device, improving the uniformity of the output light power of the star coupler. Utilizing the conventional Si process technology, the device is fabricated based on silicon-on-insulator (SOI) material. The test result shows that the star coupler has a perfect function of power splitting.     

Characteristic classes of star products on Marsden–Weinstein reduced symplectic manifolds

In this note we consider a quantum reduction scheme in deformation quantization on symplectic manifolds proposed by Bordemann, Herbig and Waldmann based on BRST cohomology. We explicitly construct the induced map on equivalence classes of star products which will turn out to be an analogue to the Kirwan map in the Cartan model of equivariant cohomology. As a byproduct, we shall see that every star product on a (suitable) reduced manifold is equivalent to a reduced star product.