Academic literature on the topic 'Vaidya’s black hole'
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Journal articles on the topic "Vaidya’s black hole"
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IBOHAL, NG, and L. KAPIL. "CHARGED BLACK HOLES IN VAIDYA BACKGROUNDS: HAWKING'S RADIATION." International Journal of Modern Physics D 19, no. 04 (April 2010): 437–64. http://dx.doi.org/10.1142/s0218271810016518.
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In this paper we propose a class of embedded solutions of Einstein's field equations describing nonrotating Reissner–Nordstrom–Vaidya and rotating Kerr–Newman–Vaidya black holes. The Reissner–Nordstrom–Vaidya is obtained by embedding Reissner–Nordstrom solution into the nonrotating Vaidya. Similarly, we also find the Kerr–Newman–Vaidya black hole, when Kerr–Newman embeds into the rotating Vaidya solution. The Reissner–Nordstrom–Vaidya solution is type D whereas the Kerr–Newman–Vaidya metric is algebraically special of type II by the Petrov classification of space–time. These embedded solutions can be expressed in the Kerr–Schild ansatze on different backgrounds. The energy–momentum tensors for both nonrotating as well as rotating embedded solutions satisfy the energy conservation equations which show that they are solutions of Einstein's field equations. The surface gravity, area, temperature and entropy are also presented for each embedded black hole. It is observed that the area of the embedded black holes is greater than the sum of the areas of the individual ones. By considering the charge to be a function of radial coordinates it is shown that there is a change in the masses of the variably charged black holes. If such radiation continues, the mass of the black hole will evaporate completely thereby forming "instantaneous" charged black holes and creating embedded negative mass naked singularities describing the possible the life of radiation embedded black holes during their continuous radiation processes.
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IBOHAL, NG, and L. DORENDRO. "NON-STATIONARY ROTATING BLACK HOLES: ENTROPY AND HAWKING'S RADIATION." International Journal of Modern Physics D 14, no. 08 (August 2005): 1373–412. http://dx.doi.org/10.1142/s0218271805007127.
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In this paper we derive a class of non-stationary rotating solutions including Vaidya–Bonnor–de Sitter, Vaidya–Bonnor-monopole and Vaidya–Bonnor–Kerr. The rotating Viadya–Bonnor–de Sitter solution describes an embedded black hole that the rotating Vaidya–Bonnor black hole is embedded into the rotating de Sitter cosmological universe. In the case of the Vaidya–Bonnor–Kerr, the rotating Vaidya–Bonnor solution is embedded into the vacuum Kerr solution, and similarly, Vaidya–Bonnor-monopole. By considering the charge to be function of u and r, we discuss the Hawking's evaporation of the masses of variable-charged non-embedded, non-rotating and rotating Vaidya–Bonnor, and embedded rotating, Vaidya–Bonnor–de Sitter, Vaidya–Bonnor-monopole and Vaidya–Bonnor–Kerr, black holes. It is found that every electrical radiation of variable-charged black holes will produce a change in the mass of the body without affecting the Maxwell scalar in non-embedded cases; whereas in embedded cases, the Maxwell scalar, the cosmological constant, monopole charge and the Kerr mass are not affected by the radiation process. It was also found that during the Hawking's radiation process, after the complete evaporation of masses of these variable-charged black holes, the electrical radiation will continue creating (i) negative mass naked singularities in non-embedded ones, and (ii) embedded negative mass naked singularities in embedded black holes. The surface gravity, entropy and angular velocity of the horizon are presented for each of these non-stationary black holes.
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Mustari, Mustari, and Yuant Tiandho. "Thermodynamics of a Non-Stationary Black Hole Based on Generalized Uncertainty Principle." Journal of Physics: Theories and Applications 1, no. 2 (October 29, 2017): 127. http://dx.doi.org/10.20961/jphystheor-appl.v1i2.19308.
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In the general theory of relativity (GTR), black holes are defined as objects with very strong gravitational fields even light can not escape. Therefore, according to GTR black hole can be viewed as a non-thermodynamic object. The worldview of a black hole began to change since Hawking involves quantum field theory to study black holes and found that black holes have temperatures that analogous to black body radiation. In the theory of quantum gravity there is a term of the minimum length of an object known as the Planck length that demands a revision of Heisenberg's uncertainty principle into a Generalized Uncertainty Principle (GUP). Based on the relationship between the momentum uncertainty and the characteristic energy of the photons emitted by a black hole, the temperature and entropy of the non-stationary black hole (Vaidya-Bonner black hole) were calculated. The non-stationary black hole was chosen because it more realistic than static black holes to describe radiation phenomena. Because the black hole is dynamic then thermodynamics studies are conducted on both black hole horizons: the apparent horizon and its event horizon. The results showed that the dominant correction term of the temperature and entropy of the Vaidya-Bonner black hole are logarithmic.
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LIU, BAI SHENG, and JING YI ZHANG. "DISCUSSION ON EVENT HORIZON AND QUANTUM ERGOSPHERE OF DYNAMIC DE SITTER BLACK HOLES." Modern Physics Letters A 27, no. 04 (February 10, 2012): 1250010. http://dx.doi.org/10.1142/s0217732312500101.
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In the paper, the tunneling framework is applied to calculate the local horizons of Vaidya–de Sitter black holes and Vaidya–Bonner–de Sitter black holes. The researches show that the quantum ergosphere of a spherically symmetric black hole is identical with the potential barrier set by the tunneling process. The calculations also indicate that both the apparent horizons of the dynamic de Sitter black hole produce Hawking radiation. The conclusions can be applicable to either the charged or uncharged particles' Hawking radiation.
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CASTRO, C., J. A. NIETO, L. RUIZ, and J. SILVAS. "ON TIME-DEPENDENT BLACK HOLES AND COSMOLOGICAL MODELS FROM A KALUZA–KLEIN MECHANISM." International Journal of Modern Physics A 24, no. 07 (March 20, 2009): 1383–415. http://dx.doi.org/10.1142/s0217751x09042931.
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Novel static, time-dependent and spatial–temporal solutions to Einstein field equations, displaying singularities, with and without horizons, and in several dimensions, are found based on a dimensional reduction procedure widely used in Kaluza–Klein-type theories. The Kerr–Newman black hole entropy as well as the Reissner–Nordstrom, Kerr and Schwarzschild black hole entropy are derived from the corresponding Euclideanized actions. A very special cosmological model based on the dynamical interior geometry of a black hole is found that has no singularities at t = 0 due to the smoothing of the mass distribution. We conclude with another cosmological model equipped also with a dynamical horizon and which is related to Vaidya's metric (associated with the Hawking radiation of black holes) by interchanging t ↔ r, which might render our universe a dynamical black hole.
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Ishwarchandray, Ngangbam, and Ng Ibohal. "Black Holes in Non-stationary de Sitter Space with Variable Λ(u)." Journal of the Tensor Society 11, no. 01 (June 30, 2007): 25–48. http://dx.doi.org/10.56424/jts.v11i01.10586.
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In this paper we discuss a class of non-stationary solutions of Einstein’s field equations based on the non-stationary de Sitter space-time. These solutions include Schwarz-schild-de Sitter and Vaidya-de Sitter black holes with a cosmological variable Λ(u). Schwarzschild-de Sitter solution with variable Λ(u) is regarded as a generalization of Schwarzschild-de Sitter solution with constant Λ. Vaidya-de Sitter black hole with variable Λ(u) is also a generalization of the radiating Vaidya black hole embedded into the stationary de Sitter space with constant Λ. It is shown the interaction of the Vaidya null fluid with the non-stationary de Sitter field expressing in an energy-momentum tensor. The energy-momentum tensor of the embedded de Sitter black holes satisfies the energy conservation law. The energy conditions (like weak, strong and dominant conditions) for the energy-momentum tensor are also studied. The physical properties of the time-like vector fields for both the embedded solutions are discussed. It is also found that the space-time geometry of Schwarzschild-de Sitter and Vaidya-de Sitter solution with variable Λ(u) are type D in the Petrov classifications of space-times. We also discuss the surface gravity, temperature and entropy of the space-time on the cosmological black hole horizons. It is also suggested that the modified Einstein’s field equations associated with a variable cosmological Λ(u) will take the form R_{ab}−(1/2) R g_{ab}+ Λ(u) g_{ab} = −K{T_{ab}+T^(NS)_{ab} } for any type of matter field distribution T_{ab}.
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WU, S. Q., and X. CAI. "NON-EXISTENCE OF NEW QUANTUM ERGOSPHERE EFFECT OF A VAIDYA-TYPE BLACK HOLE." Modern Physics Letters A 16, no. 24 (August 10, 2001): 1549–57. http://dx.doi.org/10.1142/s0217732301004789.
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Hawking evaporation of Dirac particles and scalar fields in a Vaidya-type black hole is investigated by the method of generalized tortoise coordinate transformation. It is shown that Hawking radiation of Dirac particles does not exist for P1, Q2 components but for P2, Q1 components in any Vaidya-type black holes. Both the location and the temperature of the event horizon change with time. The thermal radiation spectrum of Dirac particles is the same as that of Klein–Gordon particles. We demonstrate that there is no new quantum ergosphere effect in the thermal radiation of Dirac particles in any spherically symmetry black holes.
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Kumah, Mohammed, and Francis T. Oduro. "On the Trapped Surface Characterization of Black Hole Region in Vaidya Spacetime." Journal of Mathematics Research 10, no. 1 (January 8, 2018): 59. http://dx.doi.org/10.5539/jmr.v10n1p59.
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Characterizing black holes by means of classical event horizon is a global concept because it depends on future null infinity. This means, to find black hole region and event horizon requires the notion of the entire spacetime which is a teleological concept. With this as a motivation, we use local approach as a complementary means of characterizing black holes. In this paper we apply Gauss divergence and covariant divergence theorems to compute the fluxes and the divergences of the appropriate null vectors in Vaidya spacetime and thus explicitly determine the existence of trapped and marginally trapped surfaces in its black hole region.
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Chen, Ge-Rui, and Yong-Chang Huang. "Entropy spectrum of the apparent horizon of Vaidya black holes via adiabatic invariance." Modern Physics Letters A 31, no. 06 (February 21, 2016): 1650011. http://dx.doi.org/10.1142/s0217732316500115.
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The spectroscopy of the apparent horizon of Vaidya black holes is investigated via adiabatic invariance. We obtain an equally spaced entropy spectrum with its quantum equal to the one given by Bekenstein [J. D. Bekenstein, Phys. Rev. D 7, 2333 (1973)]. We demonstrate that the quantization of entropy and area is a generic property of horizon, not only for stationary black holes, and the results also exit in a dynamical black hole. Our work also shows that the quantization of black hole is closely related to the tunneling formalism for deriving the Hawking effect, which is interesting.
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Sadeghian, S., and A. Shafiekhani. "Extremal charged Vaidya and its near horizon geometry." International Journal of Modern Physics D 26, no. 04 (February 17, 2017): 1750036. http://dx.doi.org/10.1142/s0218271817500365.
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Recently [Formula: see text]-dimensional spherically symmetric charged Vaidya black hole solution has been constructed. We observe that this nonstationary solution admits extremal limit and study its near horizon geometry. We show that the symmetry of the near horizon geometry is [Formula: see text]. Our analysis shows that the theorems for the near horizon geometry of stationary extremal black holes, may be extended to nonstationary cases.
Dissertations / Theses on the topic "Vaidya’s black hole"
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Coudray, Armand. "Asymptotic behaviour of zero rest-mass fields on radiative space-times." Electronic Thesis or Diss., Brest, 2024. http://www.theses.fr/2024BRES0026.
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Cette thèse explore deux sujets distincts. La première partie examine le comportement asymptotique des ondes scalaires dans l’espace-temps de Vaidya, décrivant un trou blanc sphérique en évaporation via émission de poussières isotropes. L’analyse se focalise sur la régularité des ondes scalaires conformes au bord (passé et futur) isotrope du compactifié, en fonction des données initiales du champ conforme. Nous construisons également l’opérateur de scattering conforme, montrant qu’il encode toute l’évolution du champ dans l’espace-temps compactifié. Ces résultats reposent sur des méthodes d’inégalités d’énergie et de champs de vecteurs. La seconde partie se concentre sur l’analyse des courbes isotropes entrantes dans les espaces-temps purement radiatifs de Robinson-Trautman de type D. Contrairement à une étude précédente sur la métrique de Vaidya, ces courbes ne forment pas l’horizon passé en raison de la géométrie de la solution. Le dernier chapitre classe ces courbes, montrant qu’elles présentent un comportement similaire à celui observé dans l’espace-temps de VaidyaThis thesis adresses two distinct subjects. The first part examines the asymptotic behavior of scalar waves in the Vaidya spacetime, describing a spherical white hole evaporating via emission of isotropic dust. The analysis focuses on the regularity of conformal scalar waves at the isotropic boundary (past and future) of the compactified spacetime, depending on the initial data of the conformal field. Additionally, we construct the conformal scattering operator, demonstrating its ability to encode the entire field evolution in the compactified spacetime.These findings rely on energy inequalities and vector field methods.The second part centers on analyzing incoming isotropic curves in the purely radiative Robinson-Trautman spacetimes of type D. In contrast to a previous study on Vaidya’s metric, these curves do not form the past horizon due to the solution’s geometry. The final chapter categorizes these curves, revealing a behavior akin to that observed in Vaidya’s spacetime
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Rossi, Dario. "Reissner-Nordström black holes and mass inflation." Bachelor's thesis, Alma Mater Studiorum - Università di Bologna, 2019. http://amslaurea.unibo.it/18370/.
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The existence and structure of black holes are derived from Einstein’s general theory of
relativity. Mass inflation (an increase in mass) is found when the internal structure of
black holes is studied. The objective of the present study is two-fold: (i) to obtain an
understanding of the nature of Reissner-Nordström black holes and (ii) examine the mass
inflation phenomenon. To do so, spherical symmetric solutions to Einstein’s field equations are analyzed.The Schwarzschild solution is analyzed to show the most basic result
of general relativity. The analytical (Kruskal) continuation of the Schwarzschild solution
and the mechanism of gravitational collapse are also discussed. The Reissner-Nordström
metric is then examined in detail analyzing both the general characteristics and the most
generic field equations for a body with spherical symmetry. Moreover two important applications are considered: the Vaidya solutions and the Dray-’t Hooft-Redmount (DTR)
relation. The mass inflation phenomenon is then formulated by formally integrating
Einstein’s field equations considering continuous infalling and outgoing radial fluxes of
gravitational radiation. To evaluate the growth rate of the gravitational mass, a formal
perturbation expansion in terms of the product of the flux luminosities is developed.
Finally, the possibility that the asymmetries occurring during a realistic collapse could
change the conclusions obtained for spherical symmetry is considered. The most striking
features of the physics behind black holes and the mass inflation phenomenon are shown.
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Chirenti, Cecilia Bertoni Martha Hadler. "Perturbações de sistemas gravitacionais: a métrica de vaidya, mini buracos negros e gravastares." Universidade de São Paulo, 2007. http://www.teses.usp.br/teses/disponiveis/43/43134/tde-12092007-152702/.
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Estudos de perturbações em sistemas gravitacionais no âmbito da Relatividade Geral vêm sofrendo grandes desenvolvimentos nos últimos anos, especialmente em face da evolução dos modernos detectores de ondas gravitacionais. Abordamos neste trabalho as perturbações de diferentes cenários. Principiamos com a métrica de Vaidya, utilizada para descrever espaços-tempos esfericamente simétricos e dependentes do tempo. Nossas simulações mostraram que as freqüências dos modos quasi-normais (MQN\'s) apresentam um novo efeito inercial para variações rápidas da função de massa, retornando depois ao comportamento adiabático. Em seguida, apresentamos um modelo para a evaporação de mini buracos negros por radiação de Hawking inspirado no cenário de criação destes objetos em aceleradores de partículas, previsto pelas novas teorias com dimensões extras. Nosso modelo, baseado na métrica de Vaidya n-dimensional, tornou possível a análise de MQN\'s resultando na possibilidade de se obter os parâmetros relevantes do buraco negro, como a sua massa inicial e o número de dimensões extras, a partir de medições experimentais. Finalmente, realizamos um estudo sobre uma nova solução denominada gravastar, proposta como um modelo alternativo para o estágio final de estrelas com grande massa. Obtivemos limites para os parâmetros da solução e verificamos a sua estabilidade frente a perturbações axiais, concluindo positivamente a respeito da possibilidade de se distinguir entre buracos negros e gravastares com base no seu espectro de MQN\'s.Perturbative studies of gravitational systems in General Relativity have gone through big developments in the last years, especially due to the evolution of the modern gravitational wave detectors. We consider in this work different perturbations in different scenarios. Firstly we consider the Vaidya metric, mainly used to describe time-dependent spherically symmetric spacetimes. Our simulations show that the frequencies of the quasinormal modes (QNM\'s) present a new inertial effect for rapidly varying mass functions, returning afterwards to the adiabatic behavior. Next we present a model for evaporating mini black holes in particle accelerators, in the context of the new gravity models with extra dimensions. With our model, based on the n-dimensional Vaidya metric, we are able to perform a QNM analysis which results in the possibility of obtaining the parameters of the black hole, such as its initial mass and the number of extra dimensions, from the experimental measurements. Finally, we present a study of a new solution, the gravastar, proposed as an alternative model for the end state of massive stars. We obtain bounds for the parameters of the solution and verify its stability against axial perturbations. Our results indicate that the gravastar\'s QNM spectrum can indeed be used to distinguish a black hole from a gravastar.
Conference papers on the topic "Vaidya’s black hole"
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Triyanta, H. M. Siahaan, and A. N. Bowaire. "Hawking temperatures for the Vaidya and the Reissner-Nordstrom-Vaidya black holes." In THE 4TH INTERNATIONAL CONFERENCE ON THEORETICAL AND APPLIED PHYSICS (ICTAP) 2014. AIP Publishing LLC, 2016. http://dx.doi.org/10.1063/1.4943704.
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