Stochastic quasiclassical wave function of the Universe from the third quantization procedure
We study quantized solutions of the Wheeler de Witt (WdW) equation describing a closed Friedmann-Robertson-Walker universe with a [Lambda] term and a set of massless scalar fields. We show that when [Lambda][
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| Veröffentlicht in: | Physical review. D 2015-09, Vol.92 (6), Article 063507 |
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| container_title | Physical review. D |
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| creator | Ivanov, P. Chernov, S. V. |
| description | We study quantized solutions of the Wheeler de Witt (WdW) equation describing a closed Friedmann-Robertson-Walker universe with a [Lambda] term and a set of massless scalar fields. We show that when [Lambda][ |
| doi_str_mv | 10.1103/PhysRevD.92.063507 |
| format | Article |
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V.</creator><creatorcontrib>Ivanov, P. ; Chernov, S. V.</creatorcontrib><description>We study quantized solutions of the Wheeler de Witt (WdW) equation describing a closed Friedmann-Robertson-Walker universe with a [Lambda] term and a set of massless scalar fields. We show that when [Lambda][<][<]1 in the natural units and the standard invacuum state is considered, either wave function of the universe, [Psi], or its derivative with respect to the scale factor, a, behave as random quasi-classical fields at sufficiently large values of a. The probability distribution to find a universe with particular values of the scale factor and field amplitudes following from this density matrix is again proportional to that of the Hartle-Hawking wave function, while the probability distribution over field velocities is nontrivial and different from what follows from the Hartle and Hawking formalism. 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D</title><description>We study quantized solutions of the Wheeler de Witt (WdW) equation describing a closed Friedmann-Robertson-Walker universe with a [Lambda] term and a set of massless scalar fields. We show that when [Lambda][<][<]1 in the natural units and the standard invacuum state is considered, either wave function of the universe, [Psi], or its derivative with respect to the scale factor, a, behave as random quasi-classical fields at sufficiently large values of a. The probability distribution to find a universe with particular values of the scale factor and field amplitudes following from this density matrix is again proportional to that of the Hartle-Hawking wave function, while the probability distribution over field velocities is nontrivial and different from what follows from the Hartle and Hawking formalism. 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D</jtitle><date>2015-09-08</date><risdate>2015</risdate><volume>92</volume><issue>6</issue><artnum>063507</artnum><issn>1550-7998</issn><issn>2470-0010</issn><eissn>1550-2368</eissn><eissn>2470-0029</eissn><abstract>We study quantized solutions of the Wheeler de Witt (WdW) equation describing a closed Friedmann-Robertson-Walker universe with a [Lambda] term and a set of massless scalar fields. We show that when [Lambda][<][<]1 in the natural units and the standard invacuum state is considered, either wave function of the universe, [Psi], or its derivative with respect to the scale factor, a, behave as random quasi-classical fields at sufficiently large values of a. The probability distribution to find a universe with particular values of the scale factor and field amplitudes following from this density matrix is again proportional to that of the Hartle-Hawking wave function, while the probability distribution over field velocities is nontrivial and different from what follows from the Hartle and Hawking formalism. Either [Psi] can be regarded as a stochastic classical quantity or the system can be viewed as being in a mixed state defined over classical solutions to the WdW equation.</abstract><doi>10.1103/PhysRevD.92.063507</doi><oa>free_for_read</oa></addata></record> |
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| ispartof | Physical review. D, 2015-09, Vol.92 (6), Article 063507 |
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| language | eng |
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| source | American Physical Society Journals |
| subjects | Density Derivatives Formalism Mathematical analysis Probability distribution Stochasticity Universe Wave functions |
| title | Stochastic quasiclassical wave function of the Universe from the third quantization procedure |
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