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1.
We study the thermodynamic phase transition of a quantum-corrected Schwarzschild black hole. The modified metric affects the critical temperature which is slightly less than the conventional one. The space without black holes is not the hot flat space but the hot curved space due to vacuum fluctuations so that there appears a type of Gross–Perry–Yaffe phase transition even for the very small size of black hole, which is impossible for the thermodynamics of the conventional Schwarzschild black hole. We discuss physical consequences of the new phase transition in this framework. 相似文献
2.
Bernd Brügmann 《General Relativity and Gravitation》2009,41(9):2131-2151
The success of the moving puncture method for the numerical simulation of black hole systems can be partially explained by
the properties of stationary solutions of the 1 + log coordinate condition. We compute stationary 1 + log slices of the Schwarzschild
spacetime in isotropic coordinates in order to investigate the coordinate singularity that the numerical methods have to handle
at the puncture. We present an alternative integration method to obtain isotropic coordinates that simplifies numerical integration
and that gives direct access to a local expansion in the isotropic radius near the puncture. Numerical results have shown
that certain quantities are well approximated by a function linear in the isotropic radius near the puncture, while here we
show that in some cases the isotropic radius appears with an exponent that is close to but unequal to one.
This paper is dedicated to the memory of Jürgen Ehlers. I have known JE for a number of years, in particular during his time
as founding director of the Albert Einstein Institute in Potsdam. JE was the mentor of my habilitation thesis in 1996, and
I am deeply thankful for many insightful discussions. JE combined great breadth and physical intuition with sharp analytical
thought. His example inspired me to look beyond the numerical methods and results of numerical relativity to the analytic
foundations. For example, while at the AEI, S. Brandt and I introduced “puncture initial data” for the numerical construction
of general multiple black hole spacetimes [3]. While the puncture construction starts with an analytic trick of the sort that
numerical relativists may devise, it is fair to say that the keen interest in analytical relativity created by JE at the AEI
induced us to push our analysis one step further. As a result [3] connects to [26] for an existence and uniqueness proof for
such black hole initial data, using weighted Sobolev spaces (see also [4–6]). The present work and its predecessors [9–12]
represent an example where numerical experiments led to the discovery of an analytic solution for the 1 + log gauge for the
Schwarzschild solution, and the present result, although modest, is of the type which I believe JE would have appreciated. 相似文献
3.
We derive the metric for a Schwarzschild black hole with global monopole charge by relaxing asymptotic flatness of the Schwarzschild
field. We then study the effect of global monopole charge on particle orbits and the Hawking radiation. It turns out that
existence, boundedness and stability of circular orbits scale up by (1−8πη
2)−1, and the perihelion shift and the light bending by (1−8πη
2)−3/2, while the Hawking temperature scales down by (1−8πη
2)2 the Schwarzschild values. Hereη is the global charge. 相似文献
4.
We introduce an effective action smoothly extending the standard Einstein–Hilbert action to include un-gravity effects. The improved field equations are solved for the un-graviton corrected Schwarzschild geometry reproducing the Mureika result. This is an important test to confirm the original “guess” of the form of the un-Schwarzschild metric. Instead of working in the weak field approximation and “dressing” the Newtonian potential with un-gravitons, we solve the “effective Einstein equations” including all order un-gravity effects. An unexpected “bonus” of accounting un-gravity effects is the fractalisation of the event horizon. In the un-gravity dominated regime the event horizon thermodynamically behaves as fractal surface of dimensionality twice the scale dimension dU. 相似文献
5.
Thomas Müller 《General Relativity and Gravitation》2008,40(10):2185-2199
Consider a radially freely falling observer who plunges into a Schwarzschild black hole. In contrast to a static observer,
he will have a different view of the black hole and of the outer sky. Furthermore, the relationship between the proper time
of the falling observer and the proper time of a distant static observer differs from the relationship between the proper
times of two static observers or two freely falling observers. 相似文献
6.
Schwarzschild black holes with quantum corrections are studied under scalar field perturbations and electromagnetic field perturbations to analyze the effect of the correction term on the potential function and quasinormal mode (QNM). In classical general relativity, spacetime is continuous and there is no existence of the so-called minimal length. The introduction of the correction items of the generalized uncertainty principle, the parameter β, can change the singularity structure of the black hole gauge and may lead to discretization in time and space. We apply the sixth-order WKB method to approximate the QNM of Schwarzschild black holes with quantum corrections and perform numerical analysis to derive the results of the method. Also, we find that the effective potential and QNM in scalar fields are larger than those in electromagnetic fields. 相似文献
7.
V.A. Belinski 《Physics letters. A》2012,376(3):207-215
It is shown here that there is no way for particle creation to occur by quantum tunneling through an infinitesimal neighborhood of the black hole horizon. This result is a trivial consequence of the regularity of the horizon, the equivalence principle and the general covariance of the relativistic theory of gravity. Moreover, we also confirm the less trivial statement that no particle creation by quantum tunneling through the black hole horizon is possible independent of the size of the presupposed tunneling domain. 相似文献
8.
9.
The stability of the Schwarzschild black hole is restudied in the Painlevé
coordinates. Using the Painlevé time coordinate to define the initial time, we
reconsider the odd perturbation and find that the Schwarzschild black hole in the
Painlevé coordinates is unstable. The Painlevé metric in this paper
corresponds to the white-hole-connected region of the Schwarzschild black hole
(r>2m) and the odd perturbation may be regarded as the angular perturbation.
Therefore, the white-hole-connected region of the Schwarzschild black hole is
unstable with respect to the rotating perturbation. 相似文献
10.
《Fortschritte der Physik》2017,65(1)
By analyzing the key properties of black holes from the point of view of quantum information, we derive a model‐independent picture of black hole quantum computing. It has been noticed that this picture exhibits striking similarities with quantum critical condensates, allowing the use of a common language to describe quantum computing in both systems. We analyze such quantum computing by allowing coupling to external modes, under the condition that the external influence must be soft‐enough in order not to offset the basic properties of the system. We derive model‐independent bounds on some crucial time‐scales, such as the times of gate operation, decoherence, maximal entanglement and total scrambling. We show that for black hole type quantum computers all these time‐scales are of the order of the black hole half‐life time. Furthermore, we construct explicitly a set of Hamiltonians that generates a universal set of quantum gates for the black hole type computer. We find that the gates work at maximal energy efficiency. Furthermore, we establish a fundamental bound on the complexity of quantum circuits encoded on these systems, and characterize the unitary operations that are implementable. It becomes apparent that the computational power is very limited due to the fact that the black hole life‐time is of the same order of the gate operation time. As a consequence, it is impossible to retrieve its information, within the life‐time of a black hole, by externally coupling to the black hole qubits. However, we show that, in principle, coupling to some of the internal degrees of freedom allows acquiring knowledge about the micro‐state. Still, due to the trivial complexity of operations that can be performed, there is no time advantage over the collection of Hawking radiation and subsequent decoding. 相似文献
11.
Ayan Chatterjee 《Annals of Physics》2011,(2):307-322
The paper deals with the extension of the Weak Isolated Horizon (WIH) formulation of black hole horizons to the non-minimally coupled scalar fields. In the early part of the paper, we introduce an appropriate Holst type action to incorporate scalar fields non-minimally coupled to gravity and construct the covariant phase space of the theory. Using this phase space, we proceed to prove the laws of black hole mechanics. Further, we show that with a gauge fixing, the symplectic structure on the horizon reduces to that of a U(1) Chern–Simons theory. The level of the Chern–Simons theory is shown to depend on the non-minimally coupled scalar field. 相似文献
12.
A modified de Broglie-Bohm approach is generalized to the Schwarzschild black hole. By using this method, the quantum potential and the quantum trajectories of the black hole are investigated. And we find that the linear combination of two particular solutions of the black hole wavefunction is not physical although each of them is physical, if we think that the quantum gravity should reduce into its corresponding classical counterpart in which the gravity vanishes. It seems to confirm the argument, given by Alwis and MacIntire, that a possible resolution on the quantum gravity is to give up the superposition principle. 相似文献
13.
Thomas Müller 《General Relativity and Gravitation》2009,41(3):541-558
A star orbiting a Schwarzschild black hole can be used as a toy model for an educational study of the relativistic effects
like bending of light, geodesic precession, and frequency shift. Additionally, the finiteness of the speed of light plays
a crucial role for the visual appearance of the star. We will develop an analytic method to show the difference between the
actual and the apparent position of the star depending on the observation time and the observer’s inclination to the orbital
plane. 相似文献
14.
Hawking radiation from the with a global monopole via Schwarzschild black hole gravitational anomaly 下载免费PDF全文
This paper derives the Hawking flux from the Schwarzschild black hole with a global monopole by using Robinson and Wilczek's method. Adopting a dimensional reduction technique, it can describe the effective quantum field in the (3 + 1)-dimensional global monopole background by an infinite collection of the (1 + 1)-dimensional massless fields if neglecting the ingoing modes near the horizon, where the gravitational anomaly can be cancelled by the (1 + 1)- dimensional black body radiation at the Hawking temperature. 相似文献
15.
The mass of the Schwarzschild black hole, an observable quantity, is defined as a dynamical variable, while the corresponding
conjugate is considered as a generalized momentum. Then a two-dimensional phase space is composed of the two variables. In
the two-dimensional phase space, a harmonic oscillator model of the Schwarzschild black hole is obtained by a canonical transformation.
By this model, the mass spectrum of the Schwarzschild black hole is firstly obtained. Further the horizon area operator, quantum
area spectrum and entropy are obtained in the Fock representation. Lastly, the wave function of the horizon area is derived
also.
Supported by the National Natural Science Foundation of China (Grant No. 10773002) and the Natural Research Foundation of
Heze University (Grant No. XY05WL02) 相似文献
16.
Robert Oeckl 《Physics letters. A》2018,382(37):2622-2625
The apparent incompatibility between quantum theory and general relativity has long hampered efforts to find a quantum theory of gravity. The recently proposed positive formalism for quantum theory purports to remove this incompatibility. We showcase the power of the positive formalism by applying it to the black hole to white hole transition scenario that has been proposed as a possible effect of quantum gravity. We show how the characteristic observable of this scenario, the bounce time, can be predicted within the positive formalism, while a traditional S-matrix approach fails at this task. Our result also involves a conceptually novel use of positive operator valued measures. 相似文献
17.
This paper studies the finite statistical-mechanical entropy of the
Schwarzschild anti-de Sitter (AdS) spacetime arising from quantum
massless scalar field by using the `brick wall' approach in the
Painlev\'e and Lemaitre coordinates. At first glance, it seems that
the results would be different from that in the Schwarzschild-like
coordinate since both the Painlev\'e and the Lemaitre spacetimes do
not possess the event horizon obviously. However, this paper proves
that the entropies in these coordinates are exactly equivalent to
that in the Schwarzschild-like coordinate. 相似文献
18.
19.
Alex B. Nielsen 《General Relativity and Gravitation》2009,41(7):1539-1584
We investigate whether black holes can be defined without using event horizons. In particular we focus on the thermodynamic
properties of event horizons and the alternative, locally defined horizons. We discuss the assumptions and limitations of
the proofs of the zeroth, first and second laws of black hole mechanics for both event horizons and trapping horizons. This
leads to the possibility that black holes may be more usefully defined in terms of trapping horizons. We also review how Hawking
radiation may be seen to arise from trapping horizons and discuss which horizon area should be associated with the gravitational
entropy. 相似文献
20.
We present the quasinormal frequencies of the massive scalar field in the background of a Schwarzchild black hole surrounded
by quintessence with the third-order WKB method. The mass of the scalar field u plays an important role in studying the quasinormal frequencies, the real part of the frequencies increases linearly as mass
of the field u increases, while the imaginary part in absolute value decreases linearly which leads to damping more slowly than the massless
scalar field. The frequencies have a limited value, so it is easier to detect the quasinormal modes. Moreover, owing to the
presence of the quintessence, the massive scalar field damps more slowly.
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