Hartle reviews on no-boundary quantum state of the universe pdf Dutton

Generalizing Everett’s Quantum Mechanics for Quantum Cosmology It was difficult for quantum cosmology to give an adequate description of the universe because the universe could be in any one of an infinite number of quantum states and different results follow from each state. However, in the early 1980s Hawking and Hartle suggested that the universe might be a “special ‘natural’ quantum state – a sort of ground state “(Davies, 2006, p.87). They

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SURSRVDODQGSRVVLEOHUHVROXWLRQV IOPscience. A number of theories discuss a quantum epoch in the emergence of the Universe from ‘nothing’, e.g., in the form of Vilenkin quantum tunneling , or of a similarly-defined Hartle–Hawking no-boundary wave function of the Universe ., presented the following argument against the Hartle–Hawking no-boundary proposal for the quantum state of the universe: it should most likely lead to a nearly empty large de Sitter universe, rather than to early rapid inflation. Even if one adds the condition of observers, they are most likely to form by quantum fluctuations in de Sitter and therefore not see the structure that we observe.

quantum state of the universe, and, since quantum mechanics is an inherently probabilistic theory, the information available about our speci c history. These are su cient for every Abstract We analyze the origin of the quasiclassical realm from the no-boundary proposal for the Universe’s quantum state in a class of minisuperspace models.

Quantum Mechanics for Quantum Cosmology James Hartle University of California, Santa Barbara . Quantum Cosmology • If the universe is a quantum system, it has a quantum state. • A theory of this state and calculations of its observable predictions are the objectives of quantum cosmology. • Such a theory is a necessary part of any final theory. Otherwise there are no predictions. ! Why the boundary condition of the universe are that has no boundary (Hartle & Hawking [4], Hawking [5]). Accord- ∗fujio@astr.tohoku.ac.jp †tof@astr.tohoku.ac.jp ing to this proposal the origin of the quasiclassical realm from the no-boundary proposal for the quantum state of the universe has been discussed by Hartle, Hawking and Hertog [6] in a class of minisuperspace models with ho …

William Lane Craig and the Hartle-Hawking No Boundary Proposal July 02, 2017 Classical standard hot Big Bang cosmology represents the universe as beginning from a singular dense point, with no prior description or explanation of classical spacetime. In particular James Hartle and Hawking's no boundary quantum state origin of the universe. I believe there may be some minor slight of hand imaginary time element to …

The No-Boundary Cosmological Measure Stephen Hawking, DAMTP, Cambridge Thomas Hertog, Institute of Physics, KU, Leuven Mark Srednicki, UCSB, Santa Barbara Stanford, March 2017 Jim Hartle Santa Fe Institute University of California, Santa Barbara . If the universe is a quantum mechanical Ψ system it has a quantum state. What is it? A Quantum Universe A theory of the quantum state … This means the universe has no unique origin in quantum cosmology The wave function predicts a prior over models, backgrounds and observables in inflationary cosmology which can be tested against

In the fourth part of their discussion, Jim Hartle and Bernard Carr discuss Jim Hartle’s no-boundary proposal. They explain how the proposal accounts for the quantum state of the universe as a whole, and how we find observers like us in a wholly quantum world. Hartle J, Hertog T. Arrows of time in the bouncing universes of the no-boundary quantum state Physical Review D - Particles, Fields, Gravitation and Cosmology. 85. DOI: 85. DOI: 10.1103/PhysRevD.85.103524

The Universe of GR in 1956 ``In the forty years that have elapsed [since the classic initial tests] these have remained the principal, and, with one exception the only universe --- quantum cosmology. This requires both a quantum theory of This requires both a quantum theory of gravity and a theory of the quantum state of the universe.

It is known that the no-boundary proposal in the traditional Einstein gravity does not prefer inflation, that is, the probability of realizing a large number of e-folds is exponentially suppressed. This situation may be changed drastically in a class of no... Abstract At the minisuperspace level of homogeneous models, the bare probability for a classical universe has a huge peak at small universes for the Hartle-Hawking ``no-boundary'' wave function, in contrast with the suppression at small universes for the ``tunneling'' wave function.

the boundary condition of the universe are that has no boundary (Hartle & Hawking [4], Hawking [5]). Accord- ∗fujio@astr.tohoku.ac.jp †tof@astr.tohoku.ac.jp ing to this proposal the origin of the quasiclassical realm from the no-boundary proposal for the quantum state of the universe has been discussed by Hartle, Hawking and Hertog [6] in a class of minisuperspace models with ho … of the Hartle-Hawking [2] “no-boundary” boundary con-ditions for the quantum state of the early universe. Test-ing this idea has proved difficult since a realistic model of the quantum state or wave function of the universe must describe the entire geometry and matter content of the universe. In order to make progress, a num-ber of simple models have been introduced. The most extensively

Abstract. At the minisuperspace level of homogeneous models, the bare probability for a classical universe has a huge peak at small universes for the Hartle-Hawking `no-boundary' wavefunction, in contrast to the suppression at small universes for the `tunneling' wavefunction. It is known that the no-boundary proposal in the traditional Einstein gravity does not prefer inflation, that is, the probability of realizing a large number of e-folds is exponentially suppressed. This situation may be changed drastically in a class of no...

of the Hartle-Hawking [2] “no-boundary” boundary con-ditions for the quantum state of the early universe. Test-ing this idea has proved difficult since a realistic model of the quantum state or wave function of the universe must describe the entire geometry and matter content of the universe. In order to make progress, a num-ber of simple models have been introduced. The most extensively A number of theories discuss a quantum epoch in the emergence of the Universe from ‘nothing’, e.g., in the form of Vilenkin quantum tunneling , or of a similarly-defined Hartle–Hawking no-boundary wave function of the Universe .

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SURSRVDODQGSRVVLEOHUHVROXWLRQV IOPscience. Abstract At the minisuperspace level of homogeneous models, the bare probability for a classical universe has a huge peak at small universes for the Hartle-Hawking ``no-boundary'' wave function, in contrast with the suppression at small universes for the ``tunneling'' wave function., William Lane Craig and the Hartle-Hawking No Boundary Proposal July 02, 2017 Classical standard hot Big Bang cosmology represents the universe as beginning from a singular dense point, with no prior description or explanation of classical spacetime..

At Home In The Universe Masters Of Modern Physics [PDF

Gravity An Introduction to Einstein's General Relativity. The Universe of GR in 1956 ``In the forty years that have elapsed [since the classic initial tests] these have remained the principal, and, with one exception the only 25/09/2017 · The Hartle–Hawking state is the wave function of the Universe—a notion meant to figure out how the Universe started—that is calculated from Feynman's path integral..

QUANTUM MECHANICS IN THE LIGHT OF Murray Gell-Mann

SPACE FOR BOTH NO-BOUNDARY AND TUNNELING QUANTUM

At the minisuperspace level of homogeneous models, the bare probability for a classical universe has a huge peak at small universes for the Hartle-Hawking ‘no-boundary ’ wavefunction, in contrast to the suppression at small universes for the ‘tunneling’ wavefunction. If the probability for a classical universe has a huge peak at small universes for the Hartle-Hawking ‘no-boundary’ wavefunction, in contrast to the suppression at small universes for the ‘tunneling’ wavefunction. If the probability distribution is cut o at the Planck density (say), this suggests that the former quantum state is inconsistent with our observations. For inhomogeneous models in which

of the Hartle-Hawking [2] “no-boundary” boundary con-ditions for the quantum state of the early universe. Test-ing this idea has proved difficult since a realistic model of the quantum state or wave function of the universe must describe the entire geometry and matter content of the universe. In order to make progress, a num-ber of simple models have been introduced. The most extensively It is known that the no-boundary proposal in the traditional Einstein gravity does not prefer inflation, that is, the probability of realizing a large number of e-folds is exponentially suppressed. This situation may be changed drastically in a class of no...

universe --- quantum cosmology. This requires both a quantum theory of This requires both a quantum theory of gravity and a theory of the quantum state of the universe. The Universe of GR in 1956 ``In the forty years that have elapsed [since the classic initial tests] these have remained the principal, and, with one exception the only

quantum state of the universe, and, since quantum mechanics is an inherently probabilistic theory, the information available about our speci c history. These are su cient for every This means the universe has no unique origin in quantum cosmology The wave function predicts a prior over models, backgrounds and observables in inflationary cosmology which can be tested against

It was difficult for quantum cosmology to give an adequate description of the universe because the universe could be in any one of an infinite number of quantum states and different results follow from each state. However, in the early 1980s Hawking and Hartle suggested that the universe might be a “special ‘natural’ quantum state – a sort of ground state “(Davies, 2006, p.87). They the boundary condition of the universe are that has no boundary (Hartle & Hawking [4], Hawking [5]). Accord- ∗fujio@astr.tohoku.ac.jp †tof@astr.tohoku.ac.jp ing to this proposal the origin of the quasiclassical realm from the no-boundary proposal for the quantum state of the universe has been discussed by Hartle, Hawking and Hertog [6] in a class of minisuperspace models with ho …

The quantum state of the universe is the key to the origin of classical spacetime. Minisuperspace Models Geometry: Homogeneous, isotropic, closed. Matter: cosmological constant О› plus homogeneous scalar field moving in a quadratic potential. Theory: Low-energy effective gravity. Classical Pred. in NRQM ---Key Points When S(q0) varies rapidly and A(q0) varies slowly, high probabilities are He is currently interested in the earliest moments of the Big Bang where the subjects of quantum mechanics, quantum gravity, and cosmology overlap. He has visited Cambridge often since 1971 and has collaborated closely with Stephen Hawking over many years, most notably on their famous "no boundary proposal" for the origin of the universe.

quantum state of the universe, and, since quantum mechanics is an inherently probabilistic theory, the information available about our speci c history. These are su cient for every The present note is concerned with two connected and highly important fundamental questions of physics and cosmology, namely if E8E8 Lie symmetry group describes the universe and where cosmic dark energy comes from. Furthermore, we reason following Wheeler, Hartle and Hawking that since the boundary of a boundary is an empty set which models

In my 1980 lecture I described how we had broken down the problem of finding a theory of everything into a number of more manageable parts. First of all we had divided the description of the universe around us into two parts. One part is a set of local laws that tell us how each region of the universe evolves in time, if we know its initial state, and how it is affected by other regions. The To describe the earliest moments of the Universe in quantum cosmology, we need to have some idea about the initial conditions, or "boundary conditions" at the beginning of time. One proposal, due to Hartle and Hawking, is that "the initial boundary condition of the Universe is that it had no boundary."

In the no-boundary Universe of Hartle and Hawking, the path integral for the quantum state of the Universe must be summed only over nonsingular histories. If the quantum corrections to the... Generalizing Everett’s Quantum Mechanics for Quantum Cosmology James Hartle University of California, Santa Barbara . Quantum Cosmology • If the universe is a quantum system, it has a quantum state. • A theory of this state and calculations of its observable predictions are the objectives of quantum cosmology. • Such a theory is a necessary part of any final theory. Otherwise there

Classical universes of the no-boundary quantum state James B. Hartle,1,* S.W. Hawking,2,+ and Thomas Hertog3,‡ 1Department of Physics, University of … Hartle J, Hertog T. Arrows of time in the bouncing universes of the no-boundary quantum state Physical Review D - Particles, Fields, Gravitation and Cosmology. 85. DOI: 85. DOI: 10.1103/PhysRevD.85.103524

presented the following argument against the Hartle–Hawking no-boundary proposal for the quantum state of the universe: it should most likely lead to a nearly empty large de Sitter universe, rather than to early rapid inflation. Even if one adds the condition of observers, they are most likely to form by quantum fluctuations in de Sitter and therefore not see the structure that we observe The Complex Model Of The Quantum Universe www.iosrjournals.org 22 Page temperature below 100oc, although it is then in an unstable state.

Fine-Tuning Conversations Jim Hartle and Bernard Carr 4

SURSRVDODQGSRVVLEOHUHVROXWLRQV IOPscience. It is known that the no-boundary proposal in the traditional Einstein gravity does not prefer inflation, that is, the probability of realizing a large number of e-folds is exponentially suppressed. This situation may be changed drastically in a class of no..., In the fourth part of their discussion, Jim Hartle and Bernard Carr discuss Jim Hartle’s no-boundary proposal. They explain how the proposal accounts for the quantum state of the universe as a whole, and how we find observers like us in a wholly quantum world..

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Gravity An Introduction to Einstein's General Relativity. The Bubble Multiverses of the No Boundary Quantum State Stephen Hawking, DAMTP, Cambridge Thomas Hertog, Institute of Physics, KU, Leuven Mark Srednicki, UCSB, Santa Barbara Hawking75, Cambridge, July 3, 2016 Jim Hartle Santa Fe Institute University of California, Santa Barbara . If the universe is a quantum mechanical Ψ system it has a quantum state. What is it? A Quantum Universe …, Abstract Given the observed cosmic acceleration, Leonard Susskind has presented the following argument against the Hartle Hawking no-boundary proposal for the quantum state of the universe: it should most likely lead to a nearly empty large de Sitter universe, rather than to early rapid inflation..

The present note is concerned with two connected and highly important fundamental questions of physics and cosmology, namely if E8E8 Lie symmetry group describes the universe and where cosmic dark energy comes from. Furthermore, we reason following Wheeler, Hartle and Hawking that since the boundary of a boundary is an empty set which models Abstract Given the observed cosmic acceleration, Leonard Susskind has presented the following argument against the Hartle Hawking no-boundary proposal for the quantum state of the universe: it should most likely lead to a nearly empty large de Sitter universe, rather than to early rapid inflation.

Abstract. A proposal is made for the quantum state of the universe that has an initial state that is macroscopically time symmetric about a homogeneous, isotropic bounce of extremal volume and that at that bounce is microscopically in the ground state for … Abstract At the minisuperspace level of homogeneous models, the bare probability for a classical universe has a huge peak at small universes for the Hartle-Hawking ``no-boundary'' wave function, in contrast with the suppression at small universes for the ``tunneling'' wave function.

The Hartle-Hawking "no boundary" proposal is based on the path integral, or "sum over histories," approach to quantum mechanics, in which a probability amplitude is computed by taking a weighted sum over all possible histories that lead from an initial condition (in this case, "nothing") to a quantum state of the universe, and, since quantum mechanics is an inherently probabilistic theory, the information available about our speci c history. These are su cient for every

The present note is concerned with two connected and highly important fundamental questions of physics and cosmology, namely if E8E8 Lie symmetry group describes the universe and where cosmic dark energy comes from. Furthermore, we reason following Wheeler, Hartle and Hawking that since the boundary of a boundary is an empty set which models quantum state of the universe, and, since quantum mechanics is an inherently probabilistic theory, the information available about our speci c history. These are su cient for every

Abstract. A proposal is made for the quantum state of the universe that has an initial state that is macroscopically time symmetric about a homogeneous, isotropic bounce of extremal volume and that at that bounce is microscopically in the ground state for … Generalizing Everett’s Quantum Mechanics for Quantum Cosmology James Hartle University of California, Santa Barbara . Quantum Cosmology • If the universe is a quantum system, it has a quantum state. • A theory of this state and calculations of its observable predictions are the objectives of quantum cosmology. • Such a theory is a necessary part of any final theory. Otherwise there

This means the universe has no unique origin in quantum cosmology The wave function predicts a prior over models, backgrounds and observables in inflationary cosmology which can be tested against This Casimir effect is then colossally amplified as a one internal quantum wave representing a Hartle-Hawking state vector of the universe pushing from the inside against the boundary of the universe with nothing balancing it from the non-existent outside. This strange situation becomes completely natural and logical when we remember that the boundary of the universe is a one sided Möbius

The State of the No-Boundary Wave Function Stephen Hawking, DAMTP, Cambridge Thomas Hertog, Universiteit Leuven Hawking70, Cambridge, January 7, 2012 James Hartle, UCSB, SantaBarbara based on work with . If the universe is a quantum mechanical Ψ system it has a quantum state. What is it? A Quantum Universe A theory of the quantum state is the objective of Quantum Cosmology. No State … At the minisuperspace level of homogeneous models, the bare probability for a classical universe has a huge peak at small universes for the Hartle-Hawking ‘no-boundary ’ wavefunction, in contrast to the suppression at small universes for the ‘tunneling’ wavefunction. If the probability

The quantum state of the universe is the key to the origin of classical spacetime. Minisuperspace Models Geometry: Homogeneous, isotropic, closed. Matter: cosmological constant О› plus homogeneous scalar field moving in a quadratic potential. Theory: Low-energy effective gravity. Classical Pred. in NRQM ---Key Points When S(q0) varies rapidly and A(q0) varies slowly, high probabilities are The Complex Model Of The Quantum Universe www.iosrjournals.org 22 Page temperature below 100oc, although it is then in an unstable state.

Abstract At the minisuperspace level of homogeneous models, the bare probability for a classical universe has a huge peak at small universes for the Hartle-Hawking ``no-boundary'' wave function, in contrast with the suppression at small universes for the ``tunneling'' wave function. the following argument against the Hartle-Hawking no-boundary proposal for the quantum state of the universe: It should most likely lead to a nearly empty large de Sitter universe, rather than to …

In particular James Hartle and Hawking's no boundary quantum state origin of the universe. I believe there may be some minor slight of hand imaginary time element to … Abstract We analyze the origin of the quasiclassical realm from the no-boundary proposal for the Universe’s quantum state in a class of minisuperspace models.

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QUANTUM MECHANICS IN THE LIGHT OF Murray Gell-Mann. Change of paradigm: initial state is a vacuum with only quantum fluctuations Hartle-Hawking (no-boundary) wavefunction of the Universe origin from a point – from “nothing” No rigorous operator interpretation of both no-boundary and tunneling wavefunctions Cosmology debate: no-boundary vs tunneling Ttunneling wavefunction Most probable at the minimum of inflaton potential ¤ eff 0, Furthermore, we reason following Wheeler, Hartle and Hawking that since the boundary of a boundary is an empty set which models the quantum wave of the cosmos, then it follows that dark energy is a fundamental physical phenomenon associated with the boundary of the holographic boundary. This leads directly to a clopen universe which is its own Penrose tiling-like multiverse with energy density.

Space for Both No-Boundary and Tunneling Quantum States of

SPACE FOR BOTH NO-BOUNDARY AND TUNNELING QUANTUM STATES. A number of theories discuss a quantum epoch in the emergence of the Universe from ‘nothing’, e.g., in the form of Vilenkin quantum tunneling , or of a similarly-defined Hartle–Hawking no-boundary wave function of the Universe . Dear friends, the Hartle-Hawking state is a rather complicated technical construct. It is the wavefunction of the Universe - a notion meant to figure out how the Universe started - that is calculated from Feynman's path integral in a specific way, using particular boundary conditions. I doubt there is a correct but much more penetrable explanation. If popular articles mention it, I don't.

Gravity An Introduction to Einstein's General Relativity

Gravity An Introduction to Einstein's General Relativity

Symmetric-Bounce Quantum State of the Universe CORE

Gravity An Introduction to Einstein's General Relativity

In the no-boundary Universe of Hartle and Hawking, the path integral for the quantum state of the Universe must be summed only over nonsingular histories. If the quantum corrections to the... universe --- quantum cosmology. This requires both a quantum theory of This requires both a quantum theory of gravity and a theory of the quantum state of the universe.

It is known that the no-boundary proposal in the traditional Einstein gravity does not prefer inflation, that is, the probability of realizing a large number of e-folds is exponentially suppressed. This situation may be changed drastically in a class of no... Quantum Mechanics for Quantum Cosmology James Hartle University of California, Santa Barbara . Quantum Cosmology • If the universe is a quantum system, it has a quantum state. • A theory of this state and calculations of its observable predictions are the objectives of quantum cosmology. • Such a theory is a necessary part of any final theory. Otherwise there are no predictions. ! Why

universe --- quantum cosmology. This requires both a quantum theory of This requires both a quantum theory of gravity and a theory of the quantum state of the universe. The No-Boundary Cosmological Measure Stephen Hawking, DAMTP, Cambridge Thomas Hertog, Institute of Physics, KU, Leuven Mark Srednicki, UCSB, Santa Barbara Stanford, March 2017 Jim Hartle Santa Fe Institute University of California, Santa Barbara . If the universe is a quantum mechanical Ψ system it has a quantum state. What is it? A Quantum Universe A theory of the quantum state …

Abstract. At the minisuperspace level of homogeneous models, the bare probability for a classical universe has a huge peak at small universes for the Hartle-Hawking `no-boundary' wavefunction, in contrast to the suppression at small universes for the `tunneling' wavefunction. At the minisuperspace level of homogeneous models, the bare probability for a classical universe has a huge peak at small universes for the Hartle-Hawking ‘no-boundary ’ wavefunction, in contrast to the suppression at small universes for the ‘tunneling’ wavefunction. If the probability

To describe the earliest moments of the Universe in quantum cosmology, we need to have some idea about the initial conditions, or "boundary conditions" at the beginning of time. One proposal, due to Hartle and Hawking, is that "the initial boundary condition of the Universe is that it had no boundary." the following argument against the Hartle-Hawking no-boundary proposal for the quantum state of the universe: It should most likely lead to a nearly empty large de Sitter universe, rather than to …

quantum state of the universe, and, since quantum mechanics is an inherently probabilistic theory, the information available about our speci c history. These are su cient for every The Universe of GR in 1956 ``In the forty years that have elapsed [since the classic initial tests] these have remained the principal, and, with one exception the only

no-boundary quantum state, Physical Review D 0803.1663 Hartle, Hertog, Replicaon regulates volume- Srednicki, Hartle, Science in a very large universe, Physical Review D 0906.0042 Eddington intended his fishing-net metaphor, not as a warning about selecon effects, but as a parable to teach more general limita4ons of the physical sciences. He writes (Philosophy of Physical Science, 1938 Dear friends, the Hartle-Hawking state is a rather complicated technical construct. It is the wavefunction of the Universe - a notion meant to figure out how the Universe started - that is calculated from Feynman's path integral in a specific way, using particular boundary conditions. I doubt there is a correct but much more penetrable explanation. If popular articles mention it, I don't

A number of theories discuss a quantum epoch in the emergence of the Universe from ‘nothing’, e.g., in the form of Vilenkin quantum tunneling , or of a similarly-defined Hartle–Hawking no-boundary wave function of the Universe . The Hartle–Hawking no-boundary wave function of the universe , is a unique construction in quantum cosmology which has been put forward to describe the early stages of the universe evolution. It is possible that this function describes the whole universe evolution defining the probability measure on classical spacetimes [3] .

quantum state of the universe, and, since quantum mechanics is an inherently probabilistic theory, the information available about our speci c history. These are su cient for every of the Hartle-Hawking [2] “no-boundary” boundary con-ditions for the quantum state of the early universe. Test-ing this idea has proved difficult since a realistic model of the quantum state or wave function of the universe must describe the entire geometry and matter content of the universe. In order to make progress, a num-ber of simple models have been introduced. The most extensively

Furthermore, we reason following Wheeler, Hartle and Hawking that since the boundary of a boundary is an empty set which models the quantum wave of the cosmos, then it follows that dark energy is a fundamental physical phenomenon associated with the boundary of the holographic boundary. This leads directly to a clopen universe which is its own Penrose tiling-like multiverse with energy density The Hartle-Hawking "no boundary" proposal is based on the path integral, or "sum over histories," approach to quantum mechanics, in which a probability amplitude is computed by taking a weighted sum over all possible histories that lead from an initial condition (in this case, "nothing") to a

Change of paradigm: initial state is a vacuum with only quantum fluctuations Hartle-Hawking (no-boundary) wavefunction of the Universe origin from a point – from “nothing” No rigorous operator interpretation of both no-boundary and tunneling wavefunctions Cosmology debate: no-boundary vs tunneling Ttunneling wavefunction Most probable at the minimum of inflaton potential ¤ eff 0 for a classical universe has a huge peak at small universes for the Hartle-Hawking ‘no-boundary’ wavefunction, in contrast to the suppression at small universes for the ‘tunneling’ wavefunction. If the probability distribution is cut o at the Planck density (say), this suggests that the former quantum state is inconsistent with our observations. For inhomogeneous models in which