Chaos in classical cosmology (II)
Abstract We present a new dynamical calculation about the Friedman-Robertson-Walker universe considered as an autonomous Hamiltonian. The time evolution of this Hamiltonian presents numerical instabilities so we apply a symplectic integration via infinitesimal canonical transformations of the phase...
Ausführliche Beschreibung
Autor*in: |
Blanco, S. [verfasserIn] |
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Format: |
Artikel |
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Sprache: |
Englisch |
Erschienen: |
1995 |
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Schlagwörter: |
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Anmerkung: |
© Plenum Publishing Corporation 1995 |
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Übergeordnetes Werk: |
Enthalten in: General relativity and gravitation - Kluwer Academic Publishers-Plenum Publishers, 1970, 27(1995), 12 vom: Dez., Seite 1295-1307 |
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Übergeordnetes Werk: |
volume:27 ; year:1995 ; number:12 ; month:12 ; pages:1295-1307 |
Links: |
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DOI / URN: |
10.1007/BF02153318 |
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Katalog-ID: |
OLC2113759497 |
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520 | |a Abstract We present a new dynamical calculation about the Friedman-Robertson-Walker universe considered as an autonomous Hamiltonian. The time evolution of this Hamiltonian presents numerical instabilities so we apply a symplectic integration via infinitesimal canonical transformations of the phase space time evolution that preserves the Poincaré invariant. In this way, we have also obtained a sensitive improvement in the accuracy of the Hamiltonian constraint, as well as in the computing time. We confirm our previous results; in a spatially closed universe, the route to chaos is reached by sucessive breakage of the resonant tori due to the action of 1∶1 resonances. | ||
650 | 4 | |a Phase Space | |
650 | 4 | |a Time Evolution | |
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700 | 1 | |a Costa, A. |4 aut | |
700 | 1 | |a Rosso, O. A. |4 aut | |
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10.1007/BF02153318 doi (DE-627)OLC2113759497 (DE-He213)BF02153318-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Blanco, S. verfasserin aut Chaos in classical cosmology (II) 1995 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Plenum Publishing Corporation 1995 Abstract We present a new dynamical calculation about the Friedman-Robertson-Walker universe considered as an autonomous Hamiltonian. The time evolution of this Hamiltonian presents numerical instabilities so we apply a symplectic integration via infinitesimal canonical transformations of the phase space time evolution that preserves the Poincaré invariant. In this way, we have also obtained a sensitive improvement in the accuracy of the Hamiltonian constraint, as well as in the computing time. We confirm our previous results; in a spatially closed universe, the route to chaos is reached by sucessive breakage of the resonant tori due to the action of 1∶1 resonances. Phase Space Time Evolution Computing Time Differential Geometry Space Time Costa, A. aut Rosso, O. A. aut Enthalten in General relativity and gravitation Kluwer Academic Publishers-Plenum Publishers, 1970 27(1995), 12 vom: Dez., Seite 1295-1307 (DE-627)129605735 (DE-600)242130-6 (DE-576)015100022 0001-7701 nnns volume:27 year:1995 number:12 month:12 pages:1295-1307 https://doi.org/10.1007/BF02153318 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_30 GBV_ILN_31 GBV_ILN_40 GBV_ILN_60 GBV_ILN_70 GBV_ILN_2009 GBV_ILN_2409 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4306 AR 27 1995 12 12 1295-1307 |
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10.1007/BF02153318 doi (DE-627)OLC2113759497 (DE-He213)BF02153318-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Blanco, S. verfasserin aut Chaos in classical cosmology (II) 1995 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Plenum Publishing Corporation 1995 Abstract We present a new dynamical calculation about the Friedman-Robertson-Walker universe considered as an autonomous Hamiltonian. The time evolution of this Hamiltonian presents numerical instabilities so we apply a symplectic integration via infinitesimal canonical transformations of the phase space time evolution that preserves the Poincaré invariant. In this way, we have also obtained a sensitive improvement in the accuracy of the Hamiltonian constraint, as well as in the computing time. We confirm our previous results; in a spatially closed universe, the route to chaos is reached by sucessive breakage of the resonant tori due to the action of 1∶1 resonances. Phase Space Time Evolution Computing Time Differential Geometry Space Time Costa, A. aut Rosso, O. A. aut Enthalten in General relativity and gravitation Kluwer Academic Publishers-Plenum Publishers, 1970 27(1995), 12 vom: Dez., Seite 1295-1307 (DE-627)129605735 (DE-600)242130-6 (DE-576)015100022 0001-7701 nnns volume:27 year:1995 number:12 month:12 pages:1295-1307 https://doi.org/10.1007/BF02153318 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_30 GBV_ILN_31 GBV_ILN_40 GBV_ILN_60 GBV_ILN_70 GBV_ILN_2009 GBV_ILN_2409 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4306 AR 27 1995 12 12 1295-1307 |
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10.1007/BF02153318 doi (DE-627)OLC2113759497 (DE-He213)BF02153318-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Blanco, S. verfasserin aut Chaos in classical cosmology (II) 1995 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Plenum Publishing Corporation 1995 Abstract We present a new dynamical calculation about the Friedman-Robertson-Walker universe considered as an autonomous Hamiltonian. The time evolution of this Hamiltonian presents numerical instabilities so we apply a symplectic integration via infinitesimal canonical transformations of the phase space time evolution that preserves the Poincaré invariant. In this way, we have also obtained a sensitive improvement in the accuracy of the Hamiltonian constraint, as well as in the computing time. We confirm our previous results; in a spatially closed universe, the route to chaos is reached by sucessive breakage of the resonant tori due to the action of 1∶1 resonances. Phase Space Time Evolution Computing Time Differential Geometry Space Time Costa, A. aut Rosso, O. A. aut Enthalten in General relativity and gravitation Kluwer Academic Publishers-Plenum Publishers, 1970 27(1995), 12 vom: Dez., Seite 1295-1307 (DE-627)129605735 (DE-600)242130-6 (DE-576)015100022 0001-7701 nnns volume:27 year:1995 number:12 month:12 pages:1295-1307 https://doi.org/10.1007/BF02153318 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_30 GBV_ILN_31 GBV_ILN_40 GBV_ILN_60 GBV_ILN_70 GBV_ILN_2009 GBV_ILN_2409 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4306 AR 27 1995 12 12 1295-1307 |
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10.1007/BF02153318 doi (DE-627)OLC2113759497 (DE-He213)BF02153318-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Blanco, S. verfasserin aut Chaos in classical cosmology (II) 1995 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Plenum Publishing Corporation 1995 Abstract We present a new dynamical calculation about the Friedman-Robertson-Walker universe considered as an autonomous Hamiltonian. The time evolution of this Hamiltonian presents numerical instabilities so we apply a symplectic integration via infinitesimal canonical transformations of the phase space time evolution that preserves the Poincaré invariant. In this way, we have also obtained a sensitive improvement in the accuracy of the Hamiltonian constraint, as well as in the computing time. We confirm our previous results; in a spatially closed universe, the route to chaos is reached by sucessive breakage of the resonant tori due to the action of 1∶1 resonances. Phase Space Time Evolution Computing Time Differential Geometry Space Time Costa, A. aut Rosso, O. A. aut Enthalten in General relativity and gravitation Kluwer Academic Publishers-Plenum Publishers, 1970 27(1995), 12 vom: Dez., Seite 1295-1307 (DE-627)129605735 (DE-600)242130-6 (DE-576)015100022 0001-7701 nnns volume:27 year:1995 number:12 month:12 pages:1295-1307 https://doi.org/10.1007/BF02153318 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_30 GBV_ILN_31 GBV_ILN_40 GBV_ILN_60 GBV_ILN_70 GBV_ILN_2009 GBV_ILN_2409 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4306 AR 27 1995 12 12 1295-1307 |
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10.1007/BF02153318 doi (DE-627)OLC2113759497 (DE-He213)BF02153318-p DE-627 ger DE-627 rakwb eng 530 VZ 16,12 ssgn Blanco, S. verfasserin aut Chaos in classical cosmology (II) 1995 Text txt rdacontent ohne Hilfsmittel zu benutzen n rdamedia Band nc rdacarrier © Plenum Publishing Corporation 1995 Abstract We present a new dynamical calculation about the Friedman-Robertson-Walker universe considered as an autonomous Hamiltonian. The time evolution of this Hamiltonian presents numerical instabilities so we apply a symplectic integration via infinitesimal canonical transformations of the phase space time evolution that preserves the Poincaré invariant. In this way, we have also obtained a sensitive improvement in the accuracy of the Hamiltonian constraint, as well as in the computing time. We confirm our previous results; in a spatially closed universe, the route to chaos is reached by sucessive breakage of the resonant tori due to the action of 1∶1 resonances. Phase Space Time Evolution Computing Time Differential Geometry Space Time Costa, A. aut Rosso, O. A. aut Enthalten in General relativity and gravitation Kluwer Academic Publishers-Plenum Publishers, 1970 27(1995), 12 vom: Dez., Seite 1295-1307 (DE-627)129605735 (DE-600)242130-6 (DE-576)015100022 0001-7701 nnns volume:27 year:1995 number:12 month:12 pages:1295-1307 https://doi.org/10.1007/BF02153318 lizenzpflichtig Volltext GBV_USEFLAG_A SYSFLAG_A GBV_OLC SSG-OLC-PHY SSG-OLC-AST SSG-OPC-AST GBV_ILN_11 GBV_ILN_20 GBV_ILN_30 GBV_ILN_31 GBV_ILN_40 GBV_ILN_60 GBV_ILN_70 GBV_ILN_2009 GBV_ILN_2409 GBV_ILN_4012 GBV_ILN_4046 GBV_ILN_4306 AR 27 1995 12 12 1295-1307 |
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Abstract We present a new dynamical calculation about the Friedman-Robertson-Walker universe considered as an autonomous Hamiltonian. The time evolution of this Hamiltonian presents numerical instabilities so we apply a symplectic integration via infinitesimal canonical transformations of the phase space time evolution that preserves the Poincaré invariant. In this way, we have also obtained a sensitive improvement in the accuracy of the Hamiltonian constraint, as well as in the computing time. We confirm our previous results; in a spatially closed universe, the route to chaos is reached by sucessive breakage of the resonant tori due to the action of 1∶1 resonances. © Plenum Publishing Corporation 1995 |
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Abstract We present a new dynamical calculation about the Friedman-Robertson-Walker universe considered as an autonomous Hamiltonian. The time evolution of this Hamiltonian presents numerical instabilities so we apply a symplectic integration via infinitesimal canonical transformations of the phase space time evolution that preserves the Poincaré invariant. In this way, we have also obtained a sensitive improvement in the accuracy of the Hamiltonian constraint, as well as in the computing time. We confirm our previous results; in a spatially closed universe, the route to chaos is reached by sucessive breakage of the resonant tori due to the action of 1∶1 resonances. © Plenum Publishing Corporation 1995 |
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Abstract We present a new dynamical calculation about the Friedman-Robertson-Walker universe considered as an autonomous Hamiltonian. The time evolution of this Hamiltonian presents numerical instabilities so we apply a symplectic integration via infinitesimal canonical transformations of the phase space time evolution that preserves the Poincaré invariant. In this way, we have also obtained a sensitive improvement in the accuracy of the Hamiltonian constraint, as well as in the computing time. We confirm our previous results; in a spatially closed universe, the route to chaos is reached by sucessive breakage of the resonant tori due to the action of 1∶1 resonances. © Plenum Publishing Corporation 1995 |
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The time evolution of this Hamiltonian presents numerical instabilities so we apply a symplectic integration via infinitesimal canonical transformations of the phase space time evolution that preserves the Poincaré invariant. In this way, we have also obtained a sensitive improvement in the accuracy of the Hamiltonian constraint, as well as in the computing time. We confirm our previous results; in a spatially closed universe, the route to chaos is reached by sucessive breakage of the resonant tori due to the action of 1∶1 resonances.</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Phase Space</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Time Evolution</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Computing Time</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Differential Geometry</subfield></datafield><datafield tag="650" ind1=" " ind2="4"><subfield code="a">Space Time</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Costa, A.</subfield><subfield code="4">aut</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Rosso, O. A.</subfield><subfield code="4">aut</subfield></datafield><datafield tag="773" ind1="0" ind2="8"><subfield code="i">Enthalten in</subfield><subfield code="t">General relativity and gravitation</subfield><subfield code="d">Kluwer Academic Publishers-Plenum Publishers, 1970</subfield><subfield code="g">27(1995), 12 vom: Dez., Seite 1295-1307</subfield><subfield code="w">(DE-627)129605735</subfield><subfield code="w">(DE-600)242130-6</subfield><subfield code="w">(DE-576)015100022</subfield><subfield code="x">0001-7701</subfield><subfield code="7">nnns</subfield></datafield><datafield tag="773" ind1="1" ind2="8"><subfield code="g">volume:27</subfield><subfield code="g">year:1995</subfield><subfield code="g">number:12</subfield><subfield code="g">month:12</subfield><subfield code="g">pages:1295-1307</subfield></datafield><datafield tag="856" ind1="4" ind2="1"><subfield code="u">https://doi.org/10.1007/BF02153318</subfield><subfield code="z">lizenzpflichtig</subfield><subfield code="3">Volltext</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_USEFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SYSFLAG_A</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_OLC</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-PHY</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OLC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">SSG-OPC-AST</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_11</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_20</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_30</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_31</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_40</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_60</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_70</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2009</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_2409</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4012</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4046</subfield></datafield><datafield tag="912" ind1=" " ind2=" "><subfield code="a">GBV_ILN_4306</subfield></datafield><datafield tag="951" ind1=" " ind2=" "><subfield code="a">AR</subfield></datafield><datafield tag="952" ind1=" " ind2=" "><subfield code="d">27</subfield><subfield code="j">1995</subfield><subfield code="e">12</subfield><subfield code="c">12</subfield><subfield code="h">1295-1307</subfield></datafield></record></collection>
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