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To explore the influence of the cosmological constant on black hole images, we have developed a comprehensive analytical method for simulating images of Kerr–de Sitter black holes illuminated by equatorial thin accretion disks. Through the application of explicit equations, we simulate images of Kerr–de Sitter black holes illuminated by both prograde and retrograde accretion disks, examining the impact of the cosmological constant on their characteristic curves, relative sizes, and observed intensities. Our findings reveal that, in comparison to Kerr black holes, the cosmological constant not only diminishes the relative size of a black hole but also amplifies its luminosity. Moreover, an observer’s relative position in the universe ( r 0 / r C ) can influence both the relative size and luminosity of a black hole, where r 0 is the distance from the observer to the black hole, r C is the cosmological horizon determined by the value of the cosmological constant Λ .

The Kiselev model describes a black hole surrounded by a fluid with equations of state p r / ρ = - 1 and p t / ρ = ( 3 w + 1 ) / 2 respectively in radial and tangential directions. It has been extensively studied in the parameter region - 1 < w < - 1 / 3 . If one rids off the black hole and turns to the region - 1 / 3 < w < 0 , i.e. p t > 0 , then a new horizon of black hole type will emerge. This case has been mentioned in Kiselev’s pioneer work but seldom investigated in the literature. Referring to it as reduced Kiselev black hole, we revisit this case with attention to its causal structure, thermodynamics, shadow cast and weak-field limit. An alternative interpretation and extensions of the black hole are also discussed.

We investigate the cosmological implications of a phantom dark energy model with bulk viscosity. We explore this model as a possible way to resolve the big rip singularity problem that plagues the phantom models. We use the latest type Ia supernova and Hubble parameter data to constrain the model parameters and find that the data favor a significant bulk viscosity over a non-constant potential term for the phantom field. We perform a dynamical analysis of the model and show that the only stable and physical attractor corresponds to a phantom-dominated era with a total equation of state that can be greater than - 1 due to the viscosity. We also study the general effect of viscosity on the phantom field and the late time evolution of the universe. We apply the statefinder diagnostic to the model and find that it approaches a nearby fixed point asymptotically, indicating that the universe can escape the big rip singularity with the presence of bulk viscosity. We conclude that bulk viscosity can play an important role in affecting the late-time behavior as well as alleviating the singularity problem of the phantom universe.

A bstract In this paper, we shall study the dynamical behavior of the universe accelerated by the so called Veneziano ghost dark energy component locally and globally by using the linearization and nullcline method developed in this paper. The energy density is generalized to be proportional to the Hawking temperature defined on the trapping horizon instead of Hubble horizon of the Friedmann-Robertson-Walker (FRW) universe. We also give a prediction of the fate of the universe and present the bifurcation phenomenon of the dynamical system of the universe. It seems that the universe could be dominated by dark energy at present in some region of the parameter space.

In this paper, we consider the fermionic Casimir effect under a new type of space-time topology using the concept of quotient topology. The relation between the new topology and that in Feng and Li (Phys. Lett. B 691:167, 2010 ), Zhai et al. (Mod. Phys. Lett. A 26:669, 2011 ) is something like that between a Möbius strip and a cylindric. We obtain the exact results of the Casimir energy and force for the massless and massive Dirac fields in the ( D +1)-dimensional space-time. For both massless and massive cases, there is a Z 2 symmetry for the Casimir energy. To see the effect of the mass, we compare the result with that of the massless one and we found that the Casimir force approaches the result of the force in the massless case when the mass tends to zero and vanishes when the mass tends to infinity.

Here we report on the interventions taken to treat a patient exposed to high-dose radiation and provide a protocol for treating such patients in the future. The patient, Mr. Wang, was a 58-year-old male janitor who was accidentally exposed to a 192Ir source with an activity of 966.4 GBq or 26.1 Ci. The dose estimated to the lower right limb was 4,100 Gy, whereas the whole-body effective dose was 1.51 Gy. The diagnosis was made according to the results of the patient dose estimation and clinical manifestations. Systemic treatment included stimulating bone marrow hematopoietic cells, enhancing immunity, anti-infection and vitamin supplements. The treatment of radiation-induced skin lesions consisted of several debridements, two skin-flap transplantations and application of mesenchymal stem cells (MSCs). Skin-flap transplantations and MSCs play important roles in the recovery of skin wound. A combination of antibiotics and antimycotic was useful in reducing inflammation. The application of vacuum sealing drainage was effective in removing necrotic tissue and bacteria, ameliorating ischemia and hypoxia of wound tissue, providing a fresh wound bed for wound healing and improving skin or flap graft survival rates. The victim survived the accident without amputation, and function of his highly exposed right leg was partially recovered. These results demonstrate the importance of collaboration among members of a multidisciplinary team in the treatment of this patient.

The power spectra of the scalar and tensor perturbations in the noncommutative k-inflation model are calculated in this paper. In this model, all the modes created when the stringy space–time uncertainty relation is satisfied, and they are generated inside the sound/Hubble horizon during inflation for the scalar/tensor perturbations. It turns out that a linear term describing the noncommutative space–time effect contributes to the power spectra of the scalar and tensor perturbations. Confronting the general noncommutative k-inflation model with latest results from Planck and BICEP2, and taking c S and λ as free parameters, we find that it is well consistent with observations. However, for the two specific models, i.e. the tachyon and DBI inflation models, it is found that the DBI model is not favored, while the tachyon model lies inside the 1 σ contour, when the e-folding number is assumed to be around 50 ∼ 60 .

In the plane wave spacetime, we find that there will be a precession angle deviation between two free-falling gyroscopes when gravitational waves passed through. This kind of angle deviation is closely related to the well-known standard velocity memory effect. Initial conditions such as the separation velocity or displacement between the two gyroscopes will affect this angle deviation. The evolutions of the angle deviation are calculated for different cases. We find that in some extreme circumstance, the angle deviation's order of magnitude produced by a rotating compact binary source could be \\(10^{-14}\\) rads. Therefore, this memory effect caused by the gravitational wave is likely to be detected in the future.

We investigate the cosmological implications of a phantom dark energy model with bulk viscosity. We explore this model as a possible way to resolve the big rip singularity problem that plagues the phantom models. We use the latest type Ia supernova and Hubble parameter data to constrain the model parameters and find that the data favor a significant bulk viscosity over a non-constant potential term for the phantom field. We perform a dynamical analysis of the model and show that the only stable and physical attractor corresponds to a phantom-dominated era with a total equation of state that can be greater than \\(-1\\) due to the viscosity. We also study the general effect of viscosity on the phantom field and the late time evolution of the universe. We apply the statefinder diagnostic to the model and find that it approaches a nearby fixed point asymptotically, indicating that the universe can escape the big rip singularity with the presence of bulk viscosity. We conclude that bulk viscosity can play an important role in affecting the late-time behavior as well as alleviating the singularity problem of the phantom universe.

When a gravitational wave or a graviton travels through an electric or magnetic background, it could convert into a photon with some probability. In this paper, a dipole magnetic field is considered as this kind of background in both the Minkowski spacetime and the curved spacetime in the near-zone of a neutron star. In the former case, we find that the graviton traveling vertically rather than parallel to the background magnetic field could be more effectively converted into an electromagnetic radiation field. In the latter case, we focus on the situation, in which the graviton travels along the radial direction near a neutron star. The radius of a neutron star is about ten kilometers, so the gravitational wave with long wavelength or low frequency may bypass neutron stars by diffraction. For high frequency gravitational wave, the conversion probability is proportional to the distance square as that in the static electric or magnetic background case. The smaller the inclination angle between the dipole field and the neutron star north pole is, the larger magnetic amplitude will be. The term that described curved spacetime will slightly enhance this kind of probability. We estimate that this value is about the order of \\(\\sim 10^{-14}- 10^{-10}\\). Therefore, it is expectable that this kind of conversion process may have a potential to open a window for observing high frequency gravitational waves.