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I-Ching Yang

Publications and source records attributed to I-Ching Yang.

At least 19 recordsLinked to original sources
arXiv2022

On the energy of Schwarzschild spacetime with the post-Newtonian approximation

With the post-Newtonian approxination, the energy of Schwarzschild spacetime in the Weinberg prescription is obtained. The energy for the first post-Newtonian approximation $E^{(1)} = m$ gives the Newtonian treatment of Schwarzschild spacetime. However, for the second post-Newtonian approximation, the erergy is shown that $E^{(1)}$ adds extra terms $E^{(2)}$ which consist of the energy stored in the configuration $E_{\rm config}$, in the gravitational field $E_{\rm field}$. and a term of surface integral. These extra terms gives post-Newtonian corrections to the Newtonian treatment.

gr-qc↗
arXiv2021

The Einstein and M{\o}ller energy-momentum complexes in post-Newtonian approximation

In the first and second post-Newtonian approximation of the Schwarzschild metric, I obtain the energy component of the Einstein and M{\o}ller energy-momentum complex. Both energies involve the rest-mass energy $m$, the energy stored in the configuration and that in the gravitational field, but the energies of Schwarzschild spacetime in the Einstein and M{\o}ller prescriptions are the total mass-energy $M$. First, for general relativity, the rest-mass energy $m$ in the flat spacetime behaves like the bare mass, and the total mass-energy $M$ in the curved spacetime behaves like the experimentally observed mass. Second, the zero-potential surface is important condition for defining the energy of gravitational field, and plays an important role in the energy-momentum localization of general relativity.

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arXiv2021

On the energy density of linearly polarized, plane gravitational wave

In this article, the energy density of plane gravitational wave is studied by using Einstein and M{\o}ller's prescription of energy-momentum pseudotensors. The linearly polarized plan gravitational wave solution of Einstein field equation, which has been defined by Bondi et al., is represented by four kinds of different coodrinates. The energy distribution of gravitational wave solution in Einstein and M{\o}ller's prescription are obtained. Particularly the energy component is zero in null coordinates.

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arXiv2018

The energy of the universe in the Bianchi type-II cosmological model

To investigate the energy of Bianchi type-II cosmological model, I used the energy-momentum complexes of Einstein and M{\o}ller and obtained the zero total energy in these two prescriptions. This result reinforces the viewpoint of Albrow and Tryon that the universe must have a zero net value for all conserved quantities and be equivalent to the previous works of Nester et al. and Aydogdu et al.

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arXiv2016

The Relation Between the Quasi-localized Energy Complexes and the Thermodynamic Potential for the Schwarzschild-de Sitter Black Hole

The Schwarzschild-de Sitter (SdS) black hole solution, which has two event horizons, is considered to examine the relation between the quasi-localized energy complexes on ${\cal M}$ and the heat flows passing through its boundary $\partial {\cal M}$. Here ${\cal M}$ is the patch between cosmological event horizon and black hole event horizon of the SdS black hole solution. Conclusively, the relation, like the Legendre transformation, between the quasi-localized Einstein and M{\o}ller energy complex and the heat flows passing through the boundary is obeyed, and these two quasi-localized energy complexes could be corresponding to thermodynamic potentials.

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arXiv2011

Thermodynamical Properties and Quasi-localized Energy of the Stringy Dyonic Black Hole Solution

In this article, we calculate the heat flux passing through the horizon $. {\bf TS}|_{r_h}$ and the difference of energy between the Einstein and Møller prescription within the region ${\cal M}$, in which is the region between outer horizon ${\cal H}_+$ and inner horizon ${\cal H}_-$, for the modified GHS solution, KLOPP solution and CLH solution. The formula . E_{\rm Einstein}|_{\cal M} = . E_{\rm Møller}|_{\cal M} - \sum_{\partial {\cal M}} {\bf TS}$ is obeyed for the mGHS solution and the KLOPP solution, but not for the CLH solution. Also, we suggest a RN-like stringy dyonic black hole solution, which comes from the KLOPP solution under a dual transformation, and its thermodynamical properties are the same as the KLOPP solution.

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arXiv2011

The Quasi-localized Einstein and Møller Energy Complex as Thermodynamic Potentials

In this article, I obtain the Einstein and Møller energy complex in PG coordinates. According to the difference of energy within radius $r$ between Einstein and Møller prescription, I could present the difference of energy within radius $r$ like the fomula of Legendre transformation and propose that the Møller and Einstein energy complex play the role of internal energy and Helmholtz energy in thermodynamics.

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arXiv2009

The Energy of Regular Black Hole in General Relativity Coupled to Nonlinear Electrodynamics

According to the Einstein, Weinberg, and Møller energy-momentum complexes, we evaluate the energy distribution of the singularity-free solution of the Einstein field equations coupled to a suitable nonlinear electrodynamics suggested by Ayón-Beato and García. The results show that the energy associated with the definitions of Einstein and Weinberg are the same, but Møller not. Using the power series expansion, we find out that the first two terms in the expression are the same as the energy distributions of the Reissner-Nordström solution, and the third term could be used to survey the factualness between numerous solutions of the Einstein field eqautions coupled to a nonlinear electrodynamics.

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arXiv2009

Energy Distribution of a Regular Class of Exact Black Hole Solutions

In this paper we present the expressions for the energy of a regular class of exact black hole solutions of Einstein's equations coupled with a nonlinear electrodynamics source. We calculate the energy distribution using the Einstein, Weinberg and Møller prescriptions. We make a discussion of the results in function of two specific parameters, a sort of dipole and quadrupole moments of the nonlinear source $α$ and $β$, and in addition a study of some particular cases is performed.

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arXiv2009

On the Energy of Vaidya Space-time

In this paper we calculate the energy distribution of six cases of Vaidya-solutions in the Møller prescription. Except the energy complex of Møller for the monopole solution vanishes everywhere, for other solutions have non-zero energy component, only the energy distributions of the de Sitter and anti-de Sitter solution are independent on $v$. For the radiating dyon solution, the difference in energy complex between Møller's and Einstein's prescription is like the case of Reissner-Nordström solution.

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arXiv2007

Landau-Lifshitz and Weinberg Energy-Momentum Complexes for 2+1 Dimensional Black Hole Solutions

The aim of this paper is to evaluate the energy distribution of some 2+1 black hole solutions applying the Landau-Lifshitz and Weinberg definitions. The metrics under consideration describe the charged black hole, the solution coupling to a static scalar field and the static and circularly symmetric exact solution of the Einstein-massless scalar equation. Further, we compare the expressions for energy with those obtained using the Einstein and Moller prescriptions and give a discussion of the results.

gr-qc↗
arXiv2006

The Energy for 2+1 Dimensional Black Hole Solutions

The energy distributions of four 2+1 dimensional black hole solutions were obtained by using the Einstein and Møller energy-momentum complexes. while $r \to \infty$, the energy distributions of these four solutions become divergence.

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arXiv2005

The Evaluation of the Møller Energy Complex in Difference Coordinate Representations

The Møller energy complex of Schwarzschild black hole solution in several coodinates are evaluated. Our results show that the Møller energy complex is independent of not only the purely spatial transformation, but also the shift of time coordinate. So, we could conclude that a shift of time coordinates will not change the energy which is obtained by using the definition of Møller energy complex.

gr-qc↗
arXiv2004

On the Energy of Stringy Black Holes

It is well-known that one of the most interesting and challenging problems of General Relativity is the energy and momentum localization. There are many attempts to evaluate the energy distribution in a general relativistic system. One of the methods used for the energy and momentum localization is the one which used the energy-momentum complexes. After the Einstein work, a large number of definitions for the energy distribution was given. We mention the expressions proposed by Landau and Lifshitz, Papapetrou, Bergmann, Weinberg and Møller. The Einstein, Landau and Lifshitz, Papapetrou, Bergmann and Weinberg energy-momentum complexes are restricted to calculate the energy distribution in quasi-Cartesian coordinates. The energy-momentum complex of Møller gives the possibility to make the calculations in any coordinate system. In this paper we calculate the energy distribution of three stringy black hole solutions in the Møller prescription. The Møller energy-momentum complex gives us a consistent result for these three situations. Keywords: Møller energy-momentum complex, charged black hole solution in heterotic string theory PACS: 04. 20 Dw, 04. 70. Bw,

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arXiv2002

On the Difference of Energy between the Einstein and Møller Prescription

In some black hole solutions, these do not exist the same energy-momentum complexes associated with using definition of Einstein and Møller in given coordinates. Here, we consider the difference of energy between the Einstein and Møller prescription, and compare it with the energy density of those black hole solutions. We found out a special relation between the difference of energy between the Einstein and Møller prescription and the energy density for considered black hole solutions.

gr-qc↗
arXiv2001

Energy associated with a static spherically symmetric nonsingular black hole

We evaluate the energy distributions of the Dymnikova space-time using the Weinberg, Papapetrou, and Møller energy-momentum complexes. This result sustain the importance of the energy-momentum complexes in the evaluation of the energy distribution of a given space-time. To compare the energy distributions obtained by using several definitions, these results show that the Einstein, Tolman, and Weinberg energy complexes are the same in Schwarzschild Cartesian coordinates, but the Papapetrou and the Møller are not.

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