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Статті в журналах з теми "Perfect Fluids"

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Автор: Grafiati

Опубліковано: 10 грудня 2022

Оновлено: 28 січня 2023

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1

Bastiaensen, B., H. R. Karimian, N. Van den Bergh, and L. Wylleman. "Purely radiative perfect fluids." Classical and Quantum Gravity 24, no. 13 (June 12, 2007): 3211–20. http://dx.doi.org/10.1088/0264-9381/24/13/005.

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2

Kramer, D. "Rigidly rotationg perfect fluids." Astronomische Nachrichten: A Journal on all Fields of Astronomy 307, no. 5 (1986): 309–12. http://dx.doi.org/10.1002/asna.2113070519.

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3

Stastna, J. "Hamilton's principle for perfect fluids." International Journal of Mathematical Education in Science and Technology 17, no. 3 (May 1986): 311–14. http://dx.doi.org/10.1080/0020739860170306.

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4

Garfinkle, David, E. N. Glass, and J. P. Krisch. "Solution Generating with Perfect Fluids." General Relativity and Gravitation 29, no. 4 (April 1997): 467–80. http://dx.doi.org/10.1023/a:1018882615955.

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5

Neilsen, David W., and Matthew W. Choptuik. "Critical phenomena in perfect fluids." Classical and Quantum Gravity 17, no. 4 (January 25, 2000): 761–82. http://dx.doi.org/10.1088/0264-9381/17/4/303.

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6

Pomeau, Yves. "Vortex dynamics in perfect fluids." Journal of Plasma Physics 56, no. 3 (December 1996): 407–18. http://dx.doi.org/10.1017/s0022377800019371.

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Анотація:

I review the current status of a problem, relevant to both plasma physics and ordinary fluid mechanics, namely the long-time behaviour of solutions of the perfect fluid equations. In two space dimensions, thanks in particular to the work of D. Montgomery, the situation is now quite clear, since one expects the formation at long times of large vortices in a background of potential flow. In three dimensions, the situation is blurred, although its understanding is a central issue for fully developped turbulence. I present some new estimates for a possible scenario of self-similar blow up of solutions of 3D Euler. That turns out to be a rather subtle question, if one tries to stay consistent with the conservation of circulation and of energy.

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7

Tarachand, R. K., and N. Ibotombi Singh. "Slowly-rotating cosmological perfect fluids." Astrophysics and Space Science 137, no. 1 (1987): 85–91. http://dx.doi.org/10.1007/bf00641622.

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8

Van den Bergh, N. "Nonrotating and nonexpanding perfect fluids." General Relativity and Gravitation 20, no. 2 (February 1988): 131–38. http://dx.doi.org/10.1007/bf00759323.

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9

Kramer, Dietrich. "Perfect fluids with conformal motion." General Relativity and Gravitation 22, no. 10 (October 1990): 1157–62. http://dx.doi.org/10.1007/bf00759016.

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10

Van den Bergh, N. "Conformally Ricci‐flat perfect fluids." Journal of Mathematical Physics 27, no. 4 (April 1986): 1076–81. http://dx.doi.org/10.1063/1.527151.

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11

Kramer, D. "Cylindrically symmetric static perfect fluids." Classical and Quantum Gravity 5, no. 2 (February 1, 1988): 393–98. http://dx.doi.org/10.1088/0264-9381/5/2/018.

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12

Ballesteros, Guillermo, and Brando Bellazzini. "Effective perfect fluids in cosmology." Journal of Cosmology and Astroparticle Physics 2013, no. 04 (April 2, 2013): 001. http://dx.doi.org/10.1088/1475-7516/2013/04/001.

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13

Kramer, D. "Perfect fluids as minimal surfaces." Astronomische Nachrichten: A Journal on all Fields of Astronomy 309, no. 4 (1988): 267–72. http://dx.doi.org/10.1002/asna.2113090419.

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14

Gutiérrez-Piñeres, A. C., and C. S. Lopez-Monsalvo. "Relativistic disks with two charged perfect fluids components." Revista de la Escuela de Física 6, no. 1 (January 16, 2019): 1–8. http://dx.doi.org/10.5377/ref.v6i1.7014.

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Анотація:

A method to describe exact solutions of the Einstein-Maxwell field equations in terms of relativistic thin disks constituted by two perfect charged fluids is presented. Describing the surface of the disk as a single charged fluid we find explicit expressions for the rest energies, the pressures and the electric charge densities of the two fluids. An explicit example is given. The particular case of the thin disks composed by two charged perfect fluids with barotropic equation of state is also presented.

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15

Capozziello, Salvatore, Carlo Alberto Mantica, and Luca Guido Molinari. "Geometric perfect fluids from Extended Gravity." Europhysics Letters 137, no. 1 (January 1, 2022): 19001. http://dx.doi.org/10.1209/0295-5075/ac525d.

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Abstract A main issue in cosmology and astrophysics is whether the dark sector phenomenology originates from particle physics, then requiring the detection of new fundamental components, or it can be addressed by modifying General Relativity. Extended Theories of Gravity are possible candidates aimed at framing dark energy and dark matter in a comprehensive geometric view. Considering the concept of perfect scalars, we show that the field equations of such theories naturally contain perfect fluid terms. Specific examples are developed for the Friedman-Lemaître-Roberson-Walker metric.

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16

Sandin, Patrik, and Claes Uggla. "Perfect fluids and generic spacelike singularities." Classical and Quantum Gravity 27, no. 2 (January 4, 2010): 025013. http://dx.doi.org/10.1088/0264-9381/27/2/025013.

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17

Fodor, Gyula, Mattias Marklund, and Zoltán Perjés. "Axistationary perfect fluids - a tetrad approach." Classical and Quantum Gravity 16, no. 2 (January 1, 1999): 453–63. http://dx.doi.org/10.1088/0264-9381/16/2/010.

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18

Kramer, D. "Perfect fluids with vanishing Simon tensor." Classical and Quantum Gravity 2, no. 6 (November 1, 1985): L135—L139. http://dx.doi.org/10.1088/0264-9381/2/6/005.

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19

Karkowski, Janusz, and Edward Malec. "Binding energy of static perfect fluids." Classical and Quantum Gravity 21, no. 16 (August 3, 2004): 3923–32. http://dx.doi.org/10.1088/0264-9381/21/16/007.

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20

Ibohal, Ng. "Rotating metrics admitting non-perfect fluids." General Relativity and Gravitation 37, no. 1 (January 2005): 19–51. http://dx.doi.org/10.1007/s10714-005-0002-6.

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21

Oliynyk, Todd A. "The Newtonian Limit for Perfect Fluids." Communications in Mathematical Physics 276, no. 1 (September 13, 2007): 131–88. http://dx.doi.org/10.1007/s00220-007-0334-z.

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22

Lang, J. M., and C. B. Collins. "Observationally homogeneous shear-free perfect fluids." General Relativity and Gravitation 20, no. 7 (July 1988): 683–710. http://dx.doi.org/10.1007/bf00758973.

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23

Oliynyk, Todd A. "Post-Newtonian Expansions for Perfect Fluids." Communications in Mathematical Physics 288, no. 3 (February 18, 2009): 847–86. http://dx.doi.org/10.1007/s00220-009-0738-z.

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24

Khater, A. H., and M. F. Mourad. "Rotating perfect fluids in general relativity." Astrophysics and Space Science 163, no. 2 (1990): 247–53. http://dx.doi.org/10.1007/bf00655746.

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25

Danchin, Raphaël. "On perfect fluids with bounded vorticity." Comptes Rendus Mathematique 345, no. 7 (October 2007): 391–94. http://dx.doi.org/10.1016/j.crma.2007.09.002.

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26

Brown, J. D. "Action functionals for relativistic perfect fluids." Classical and Quantum Gravity 10, no. 8 (August 1, 1993): 1579–606. http://dx.doi.org/10.1088/0264-9381/10/8/017.

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27

Van den Bergh, N. "Conformally Ricci‐flat perfect fluids. II." Journal of Mathematical Physics 29, no. 6 (June 1988): 1451–54. http://dx.doi.org/10.1063/1.528198.

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28

Koch, Herbert. "Transport and instability for perfect fluids." Mathematische Annalen 323, no. 3 (July 1, 2002): 491–523. http://dx.doi.org/10.1007/s002080200312.

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29

Naicker, Shavani, Sunil D. Maharaj, and Byron P. Brassel. "Isotropic Perfect Fluids in Modified Gravity." Universe 9, no. 1 (January 11, 2023): 47. http://dx.doi.org/10.3390/universe9010047.

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Анотація:

We generate the Einstein–Gauss–Bonnet field equations in higher dimensions for a spherically symmetric static spacetime. The matter distribution is a neutral fluid with isotropic pressure. The condition of isotropic pressure, an Abel differential equation of the second kind, is transformed to a first order nonlinear canonical differential equation. This provides a mechanism to generate exact solutions systematically in higher dimensions. Our solution generating algorithm is a different approach from those considered earlier. We show that a specific choice of one potential leads to a new solution for the second potential for all spacetime dimensions. Several other families of exact solutions to the condition of pressure isotropy are found for all spacetime dimensions. Earlier results are regained from our treatments. The difference with general relativity is highlighted in our study.

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30

KUMAR, SACHIN, PRATIBHA, and Y. K. GUPTA. "INVARIANT SOLUTIONS OF EINSTEIN FIELD EQUATION FOR NONCONFORMALLY FLAT FLUID SPHERES OF EMBEDDING CLASS ONE." International Journal of Modern Physics A 25, no. 20 (August 10, 2010): 3993–4000. http://dx.doi.org/10.1142/s0217751x10050184.

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Анотація:

In the present paper, nonconformal spherical symmetric perfect fluid solutions to Einstein field equations are obtained by using the invariance of the equations under the Lie group of transformations and some new solutions of this category are obtained satisfying the reality conditions like ρ ≥ p ≥ 0, ρr < 0, pr < 0 (p and ρ being pressure and energy-density respectively) in the region 0 < r < a. Such fluids do not represent isolated fluid spheres as pressure free interface is not possible for nonconformally perfect fluids of class one.

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31

KIESS, THOMAS E. "A NONSINGULAR PERFECT FLUID CLASSICAL LEPTON MODEL OF ARBITRARILY SMALL RADIUS." International Journal of Modern Physics D 22, no. 14 (December 2013): 1350088. http://dx.doi.org/10.1142/s0218271813500880.

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We exhibit a classical lepton model based on a perfect fluid that reproduces leptonic charges and masses in arbitrarily small volumes without metric singularities or pressure discontinuities. This solution is the first of this kind to our knowledge, because to date the only classical general relativistic models that have reproduced leptonic charges and masses in arbitrarily small volumes are based on imperfect (anisotopic) fluids or perfect fluids with electric field discontinuities. We use a Maxwell–Einstein exact metric for a spherically symmetric static perfect fluid in a region in which the pressure vanishes at a boundary, beyond which the metric is of the Reissner–Nordström form. This construction models lepton mass and charge in the limit as the boundary → 0.

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32

Capozziello, Salvatore, Carlo Alberto Mantica, and Luca Guido Molinari. "Cosmological perfect-fluids in f(R) gravity." International Journal of Geometric Methods in Modern Physics 16, no. 01 (January 2019): 1950008. http://dx.doi.org/10.1142/s0219887819500087.

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We show that an [Formula: see text]-dimensional generalized Robertson–Walker (GRW) space-time with divergence-free conformal curvature tensor exhibits a perfect fluid stress–energy tensor for any [Formula: see text] gravity model. Furthermore, we prove that a conformally flat GRW space-time is still a perfect fluid in both [Formula: see text] and quadratic gravity where other curvature invariants are considered.

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33

Capozziello, Salvatore, Carlo Alberto Mantica, and Luca Guido Molinari. "Cosmological perfect fluids in Gauss–Bonnet gravity." International Journal of Geometric Methods in Modern Physics 16, no. 09 (September 2019): 1950133. http://dx.doi.org/10.1142/s0219887819501330.

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In a [Formula: see text]-dimensional Friedmann–Robertson–Walker metric, it is rigorously shown that any analytical theory of gravity [Formula: see text], where [Formula: see text] is the curvature scalar and [Formula: see text] is the Gauss–Bonnet topological invariant, can be associated to a perfect-fluid stress–energy tensor. In this perspective, dark components of the cosmological Hubble flow can be geometrically interpreted.

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34

Bettoni, Dario, and Stefano Liberati. "Dynamics of non-minimally coupled perfect fluids." Journal of Cosmology and Astroparticle Physics 2015, no. 08 (August 13, 2015): 023. http://dx.doi.org/10.1088/1475-7516/2015/08/023.

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35

Guilfoyle, Brendan. "A structure theorem for stationary perfect fluids." Classical and Quantum Gravity 22, no. 9 (April 6, 2005): 1599–606. http://dx.doi.org/10.1088/0264-9381/22/9/008.

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36

Haggag, S. "Comment on 'cylindrically symmetric static perfect fluids'." Classical and Quantum Gravity 6, no. 6 (June 1, 1989): 945–47. http://dx.doi.org/10.1088/0264-9381/6/6/018.

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37

Giambò, Roberto, Fabio Giannoni, Giulio Magli, and Paolo Piccione. "Naked singularities formation in perfect fluids collapse." Classical and Quantum Gravity 20, no. 22 (October 13, 2003): 4943–48. http://dx.doi.org/10.1088/0264-9381/20/22/017.

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38

Iyer, Vivek. "Lagrangian perfect fluids and black hole mechanics." Physical Review D 55, no. 6 (March 15, 1997): 3411–26. http://dx.doi.org/10.1103/physrevd.55.3411.

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39

Van den Bergh, N. "Irrotational and conformally Ricci-flat perfect fluids." General Relativity and Gravitation 18, no. 6 (June 1986): 649–68. http://dx.doi.org/10.1007/bf00769933.

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40

Deng, Yaobing, and Philip D. Mannheim. "Perfect maxwell fluids in the standard cosmology." General Relativity and Gravitation 20, no. 10 (October 1988): 969–87. http://dx.doi.org/10.1007/bf00759020.

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41

Alonso-Blanco, R. J., and J. Muñoz-Díaz. "Flux-variational formulation of relativistic perfect fluids." Journal of Geometry and Physics 147 (January 2020): 103525. http://dx.doi.org/10.1016/j.geomphys.2019.103525.

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42

Penna, Vittorio, and Mauro Spera. "On coadjoint orbits of rotational perfect fluids." Journal of Mathematical Physics 33, no. 3 (March 1992): 901–9. http://dx.doi.org/10.1063/1.529741.

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43

Oliynyk, Todd A. "The fast Newtonian limit for perfect fluids." Advances in Theoretical and Mathematical Physics 16, no. 2 (2012): 359–91. http://dx.doi.org/10.4310/atmp.2012.v16.n2.a1.

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44

SLOBODEANU, RADU. "PERFECT FLUIDS FROM HIGH POWER SIGMA-MODELS." International Journal of Geometric Methods in Modern Physics 08, no. 08 (December 2011): 1763–82. http://dx.doi.org/10.1142/s0219887811005919.

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Анотація:

Certain critical points of a sextic sigma-model Lagrangian reminiscent of Skyrme model correspond to perfect fluids with stiff matter equation of state. We analyze from a differential geometric perspective this correspondence extended to general barotropic fluids.

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45

Brown, David J. "On Variational Principles for Gravitating Perfect Fluids." Annals of Physics 248, no. 1 (May 1996): 1–33. http://dx.doi.org/10.1006/aphy.1996.0049.

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46

Van den Bergh, N. "Shearfree and conformally Ricci-flat perfect fluids." Letters in Mathematical Physics 11, no. 2 (February 1986): 141–46. http://dx.doi.org/10.1007/bf00398425.

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47

De, Uday Chand, Sameh Shenawy, Abdallah Abdelhameed Syied, and Nasser Bin Turki. "Conformally Flat Pseudoprojective Symmetric Spacetimes in f R , G Gravity." Advances in Mathematical Physics 2022 (March 25, 2022): 1–7. http://dx.doi.org/10.1155/2022/3096782.

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Анотація:

Sufficient conditions on a pseudoprojective symmetric spacetime PPS n whose Ricci tensor is of Codazzi type to be either a perfect fluid or Einstein spacetime are given. Also, it is shown that a PPS n is Einstein if its Ricci tensor is cyclic parallel. Next, we illustrate that a conformally flat PPS n spacetime is of constant curvature. Finally, we investigate conformally flat PPS 4 spacetimes and conformally flat PPS 4 perfect fluids in f R , G theory of gravity, and amongst many results, it is proved that the isotropic pressure and the energy density of conformally flat perfect fluid PPS 4 spacetimes are constants and such perfect fluid behaves like a cosmological constant. Further, in this setting, we consider some energy conditions.

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48

Fermi, Davide, Massimo Gengo, and Livio Pizzocchero. "On the Necessity of Phantom Fields for Solving the Horizon Problem in Scalar Cosmologies." Universe 5, no. 3 (March 11, 2019): 76. http://dx.doi.org/10.3390/universe5030076.

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We discuss the particle horizon problem in the framework of spatially homogeneous and isotropic scalar cosmologies. To this purpose we consider a Friedmann–Lemaître–Robertson–Walker (FLRW) spacetime with possibly non-zero spatial sectional curvature (and arbitrary dimension), and assume that the content of the universe is a family of perfect fluids, plus a scalar field that can be a quintessence or a phantom (depending on the sign of the kinetic part in its action functional). We show that the occurrence of a particle horizon is unavoidable if the field is a quintessence, the spatial curvature is non-positive and the usual energy conditions are fulfilled by the perfect fluids. As a partial converse, we present three solvable models where a phantom is present in addition to a perfect fluid, and no particle horizon appears.

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49

KINASIEWICZ, BOGUSZ, PATRYK MACH, and EDWARD MALEC. "SELFGRAVITATION IN A GENERAL-RELATIVISTIC ACCRETION OF STEADY FLUIDS." International Journal of Geometric Methods in Modern Physics 04, no. 01 (February 2007): 197–208. http://dx.doi.org/10.1142/s0219887807001953.

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Анотація:

The selfgravity of an infalling gas can alter significantly the accretion of gases. In the case of spherically symmetric steady flows of polytropic perfect fluids the mass accretion rate achieves maximal value when the mass of the fluid is 1/3 of the total mass. There are two weakly accreting regimes, one over-abundant and the other poor in fluid content. The analysis within the newtonian gravity suggests that selfgravitating fluids can be unstable, in contrast to the accretion of test fluids.

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50

Krechet, V. G., M. L. Fil’chenkov, and G. N. Shikin. "Nonlinear scalar and spinor fields simulating perfect fluids." Gravitation and Cosmology 15, no. 1 (January 2009): 37–39. http://dx.doi.org/10.1134/s0202289309010101.

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