arXiv subjects

Jiliang Jing

Publications and source records attributed to Jiliang Jing.

At least 289 records · Page 16Linked to original sources

arXiv2009

Dark energy model with higher derivative of Hubble parameter

In this letter we consider a dark energy model in which the energy density is a function of the Hubble parameter $H$ and its derivative with respect to time $ρ_{de}=3α\ddot{H}H^{-1}+3β\dot{H}+3γH^2$. The behavior of the dark energy and the expansion history of the Universe depend heavily on the parameters of the model $α$, $β$ and $γ$. It is very interesting that the age problem of the well-known three old objects can be alleviated in this models.

gr-qc↗

arXiv2009

Dark energy interacting with dark matter and unparticle

We study dynamical behaviors of the dark energy models interacting with dark matter and unparticle in the standard flat FRW cosmology. We considered four different interacting models and examined the stability of the critical points. We find that there exist late-time scaling attractors corresponding to an accelerating Universe and the alleviation of the coincidence problem depends on the choice of parameters in the models.

gr-qc↗

arXiv2009

Strong field gravitational lensing in the deformed Hǒrava-Lifshitz black hole

Adopting the strong field limit approach, we studied the properties of strong field gravitational lensing in the deformed Hǒrava-Lifshitz black hole and obtained the angular position and magnification of the relativistic images. Supposing that the gravitational field of the supermassive central object of the galaxy described by this metric, we estimated the numerical values of the coefficients and observables for gravitational lensing in the strong field limit. Comparing with the Reissner-Norstr\"{om} black hole, we find that with the increase of parameter $α$, the angular position $θ_{\infty}$ decreases more slowly and $r_m$ more quickly, but angular separation $s$ increases more rapidly. This may offer a way to detect the effects of to distinguish a deformed Hǒrava-Lifshitz black hole from a Reissner-Norstr\"{om} black hole by the astronomical instruments in the future.

gr-qc↗

arXiv2009

Entanglement of coupled massive scalar field in background of dilaton black hole

The entanglement of the coupled massive scalar field in the spacetime of a Garfinkle-Horowitz-Strominger(GHS) dilaton black hole has been investigated. It is found that the entanglement does not depend on the mass of the particle and the coupling between the scalar field and the gravitational field, but it decreases as the dilaton parameter $D$ increases. It is interesting to note that in the limit of $D\to M$, corresponding to the case of an extreme black hole, the state has no longer distillable entanglement for any state parameter $α$, but the mutual information equals to a nonvanishing minimum value, which indicates that the total correlations consist of classical correlations plus bound entanglement in this limit.

gr-qc↗

arXiv2009

Particle energy and Hawking temperature

Some authors have recently found that the tunneling approach gives a different Hawking temperature for a Schwarzschild black hole in a different coordinate system. In this paper, we find that to work out the Hawking temperature in a different coordinate system by the tunneling approach, we must use the correct definition of the energy of the radiating particles. By using a new definition of the particle energy, we obtain the correct Hawking temperature for a Schwarzschild black hole in two dynamic coordinate systems, the Kruskal-Szekers and dynamic Lemaitre coordinate systems.

gr-qc↗

arXiv2009

Dynamical evolution of phantom scalar perturbation in the background of Schwarzschild black String spacetime

Using Leaver's continue fraction and time domain method, we study the wave dynamics of phantom scalar perturbation in a Schwarzschild black string spacetime. We find that the quasinormal modes contain the imprint from the wavenumber $k$ of the fifth dimension. The late-time behaviors are dominated by the difference between the wavenumber $k$ and the mass $μ$ of the phantom scalar perturbation. For $k<μ$, the phantom scalar perturbation in the late-time evolution grows with an exponential rate as in the four-dimensional Schwarzschild black hole spacetime. While, for $k=μ$, the late-time behavior has the same form as that of the massless scalar field perturbation in the background of a black hole. Furthermore, for $k>μ$, the late-time evolution of phantom scalar perturbation is dominated by a decaying tail with an oscillation which is consistent with that of the usual massive scalar field. Thus, the Schwarzschild black string is unstable only against the phantom scalar perturbations which satisfy the wavelength $λ>2π/μ$. These information can help us know more about the wave dynamics of phantom scalar perturbation and the properties of black string.

gr-qc↗

arXiv2008

Wave dynamics of phantom scalar perturbation in the background of Schwarzschild black hole

Using Leaver's continue fraction and time domain method, we investigate the wave dynamics of phantom scalar perturbation in the background of Schwarzschild black hole. We find that the presence of the negative kinetic energy terms modifies the standard results in quasinormal spectrums and late-time behaviors of the scalar perturbations. The phantom scalar perturbation in the late-time evolution will grow with an exponential rate.

gr-qc↗

arXiv2008

Dynamics of interacting dark energy model in Einstein and Loop Quantum Cosmology

We investigate the background dynamics when dark energy is coupled to dark matter in the universe described by Einstein cosmology and Loop Quantum Cosmology. We introduce a new general form of dark sector coupling, which presents us a more complicated dynamical phase space. Differences in the phase space in obtaining the accelerated scaling attractor in Einstein cosmology and Loop Quantum Cosmology are disclosed.

gr-qc↗

arXiv2008

Hawking radiation, Entanglement and Teleportation in background of an asymptotically flat static black hole

The effect of the Hawking temperature on the entanglement and teleportation for the scalar field in a most general, static and asymptotically flat black hole with spherical symmetry has been investigated. It is shown that the same "initial entanglement" for the state parameter $α$ and its "normalized partners" $\sqrt{1-α^{2}}$ will be degraded by the Hawking effect with increasing Hawking temperature along two different trajectories except for the maximally entangled state. In the infinite Hawking temperature limit, corresponding to the case of the black hole evaporating completely, the state has no longer distillable entanglement for any $α$. It is interesting to note that the mutual information in this limit equals to just half of the "initially mutual information". It has also been demonstrated that the fidelity of teleportation decreases as the Hawking temperature increases, which just indicates the degradation of entanglement.

gr-qc↗

arXiv2008

Scalar emission in a rotating Gödel black hole

We study the absorption probability and Hawking radiation of the scalar field in the rotating Gödel black hole in minimal five-dimensional gauged supergravity. We find that Gödel parameter $j$ imprints in the greybody factor and Hawking radiation. It plays a different role from the angular momentum of the black hole in the Hawking radiation and super-radiance. These information can help us know more about rotating Gödel black holes in minimal five-dimensional gauged supergravity.

gr-qc↗

arXiv2008

What kinds of coordinate can keep the Hawking temperature invariant for the static spherically symmetric black hole?

By studying the Hawking radiation of the most general static spherically symmetric black hole arising from scalar and Dirac particles tunnelling, we find the Hawking temperature is invariant in the general coordinate representation (\ref{arbitrary1}), which satisfies two conditions: a) its radial coordinate transformation is regular at the event horizon; and b) there is a time-like Killing vector.

gr-qc↗

arXiv2008

Late-time tail of a coupled scalar field in the background of a black hole with a global monopole

Using the technique of spectral decomposition, we investigated the late-time tails of massless and massive coupled scalar fields in the background of a black hole with a global monopole. We found that due to existence of the coupling between the scalar and gravitational fields, the massless scalar field decay faster at timelike infinity $i_+$, and so does the massive one in the intermediate late time. But the asymptotically late-time tail for the massive scalar field is not affected and its decay rate still is $t^{-5/6}$.

gr-qc↗

arXiv2008

Degradation of non-maximal entanglement of scalar and Dirac fields in non-inertial frames

The entanglement between two modes of the free scalar and Dirac fields as seen by two relatively accelerated observers has been investigated. It is found that the same initial entanglement for an initial state parameter $α$ and its "normalized partner" $\sqrt{1-α^{2}}$ will be degraded by the Unruh effect along two different trajectories except for the maximally entangled state, which just shows the inequivalence of the quantization for a free field in the Minkowski and Rindler coordinates. In the infinite acceleration limit the state doesn't have the distillable entanglement for any $α$ for the scalar field but always remains entangled to a degree which is dependent of $α$ for the Dirac field. It is also interesting to note that in this limit the mutual information equals to just half of the initially mutual information, which is independent of $α$ and the type of field.

quant-ph↗

arXiv2008

Quasinormal modes and second order thermodynamic phase transition for Reissner-Nordström black hole

The relation between the quasinormal modes (QNMs) and the second order thermodynamic phase transition (SOTPT) for the Reissner-Nordström (RN) black hole is studied. It is shown that the quasinormal frequencies of the RN black hole start to get a spiral-like shape in the complex $ω$ plane and both the real and imaginary parts become the oscillatory functions of the charge if the real part of the quasinormal frequencies arrives at its maximum at the second order phase transition point of Davies for given overtone number and angular quantum number. That is to say, we can find out the SOTPT point from the QNMs of the RN black hole. The fact shows that the quasinormal frequencies carry the thermodynamical information of the RN black hole.

gr-qc↗

arXiv2008

Evolution of arbitrary spin fields in the Schwarzschild-monopole spacetime

The quasinormal modes (QNMs) and the late-time behavior of arbitrary spin fields are studied in the background of a Schwarzschild black hole with a global monopole (SBHGM). It has been shown that the real part of the QNMs for a SBHGM decreases as the symmetry breaking scale parameter $H$ increases but imaginary part increases instead. For large overtone number $n$, these QNMs become evenly spaced and the spacing for the imaginary part equals to $-i(1-H)^{3/2}/(4M)$ which is dependent of $H$ but independent of the quantum number $l$. It is surprisingly found that the late-time behavior is dominated by an inverse power-law tail $t^{-2[1+\sqrt{(s+1/2)^{2}+ (l-s)(l+s+1)/(1-H)}]}$ for each $l$, and as $H\to0$ it reduces to the Schwarzschild case $t^{-(2l+3)}$ which is independent of the spin number $s$.

gr-qc↗

arXiv2007

Entropy of the Schwarzschild-de Sitter Black Hole due to arbitrary spin fields in different Coordinates

By using the Newman-Penrose formalism and the improved thin-layer ``brick wall'' approach, the statistical-mechanical entropies of the Schwarzschild-de Sitter black hole arising from quantum massless arbitrary spin fields are studied in the Painlevé and Lemaitre coordinates. Although the metrics in both the Painlevé and the Lemaitre coordinates do not obviously possess the singularities as that in the Schwarzschild-like coordinate, we find that, for arbitrary spin fields, the entropies in the Painlevé and Lemaitre coordinates are exactly equivalent to that in the Schwarzschild-like coordinate.

gr-qc↗

arXiv2006

Late-time evolution of charged massive Dirac fields in the Kerr-Newman background

We investigate both the intermediate late-time tail and the asymptotic tail behavior of the charged massive Dirac fields in the background of the Kerr-Newman black hole. We find that the intermediate late-time behavior of charged massive Dirac fields is dominated by an inverse power-law decaying tail without any oscillation, which is different from the oscillatory decaying tails of the scalar field. We note that the dumping exponent depends not only on the angular quantum numbers $m$, the separation constant $λ$ and the rotating parameter $a$, but also on the product $seQ$ of the spin weight of the Dirac field and the charges of the black hole and the fields. We also find that the decay rate of the asymptotically late-time tail is $t^{-5/6}$, and the oscillation of the tail has the period of $2π/ μ$ which is modulated by two types of long-term phase shifts.

gr-qc↗

arXiv2006

Energy of general 4-dimensional stationary axisymmetric spacetime in the teleparallel geometry

The field equation with the cosmological constant term is derived and the energy of the general 4-dimensional stationary axisymmetric spacetime is studied in the context of the hamiltonian formulation of the teleparallel equivalent of general relativity (TEGR). We find that, by means of the integral form of the constraints equations of the formalism naturally without any restriction on the metric parameters, the energy for the asymptotically flat/de Sitter/Anti-de Sitter stationary spacetimes in the Boyer-Lindquist coordinate can be expressed as $E=\frac{1}{8π}\int_S dθdϕ(sinθ\sqrt{g_{θθ}}+\sqrt{g_{ϕϕ}}-(1/\sqrt{g_{rr}})(\partial{\sqrt{g_ {θθ} g_{ϕϕ}}}/\partial r))$. It is surprised to learn that the energy expression is relevant to the metric components $g_{rr}$, $g_{θθ}$ and $g_{ϕϕ}$ only. As examples, by using this formula we calculate the energies of the Kerr-Newman (KN), Kerr-Newman Anti-de Sitter (KN-AdS), Kaluza-Klein, and Cvetič-Youm spacetimes.

gr-qc↗