Quantum phase transitions and the breakdown of classical general relativity

Chapline, George

doi:10.1080/13642810110037102

Cited by 75 publications

(128 citation statements)

References 16 publications

(27 reference statements)

Supporting

Mentioning

127

Contrasting

Order By: Relevance

“…Some models have been introduced to alleviate some of the black hole paradoxes [10,22,96]. In particular, we concentrate in the gravastar (vacuum condensate gravitational star) model proposed by Mazur and Mottola [60,61,62].…”

Section: Paradoxes and Unsolved Issuesmentioning

confidence: 99%

See 1 more Smart Citation

Slowly rotating supercompact Schwarzschild stars

Posada¹

2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

AcknowledgmentsI am grateful to the universe, for its harmony. The project is the study of integral and surface properties of slowly rotating homogeneous masses in the gravastar limit R → R s , where R s is the Schwarzschild radius. For this purpose we followed the perturbative method proposed by Hartle in 1967. In this model, the relativistic equations of structure for a slowly rotating star were derived at second order in the angular velocity Ω. An interesting, and educational, application of this model was investigated by Chandrasekhar and Miller. I am indebted to the Department of Physics andIn their approach, they solved numerically the structure equations of a homogeneous star (constant energy density) up to the Buchdahl bound (9/8)R s . Based on this work, our objective was to investigate the interesting region below the Buchdahl bound R s < R < (9/8)R s , which has not been studied previously in the literature.Our results were astonishing. We found that the surface properties and quadrupole mass moment approach the values corresponding to those of the Kerr metric when expanded at second order in angular momentum. This remarkable result provides a long sought solution to the problem of the source of rotation in the Kerr spacetime.iv

show abstract

Section: Paradoxes and Unsolved Issuesmentioning

confidence: 99%

“…Some alternatives to black holes have been proposed [22,27,30,53]. In particular, In the gravastar model, the spacetime suffers a quantum phase transition, which leads to p = − , starting at the center of the star and moving outwards thus releasing huge amounts of energy and entropy [63].…”

Section: Introductionmentioning

confidence: 99%

Slowly rotating supercompact Schwarzschild stars

Posada¹

2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…We demonstrate this by deriving the bulk geometry for a solvable field theory from quantum RG. For earlier ideas on possible connections between black hole horizons and phase transitions, see [12] and references there-in.…”

Section: Jhep09(2016)044mentioning

confidence: 99%

Horizon as critical phenomenon

Lee

2016

J. High Energ. Phys.

View full text Add to dashboard Cite

We show that renormalization group flow can be viewed as a gradual wave function collapse, where a quantum state associated with the action of field theory evolves toward a final state that describes an IR fixed point. The process of collapse is described by the radial evolution in the dual holographic theory. If the theory is in the same phase as the assumed IR fixed point, the initial state is smoothly projected to the final state. If in a different phase, the initial state undergoes a phase transition which in turn gives rise to a horizon in the bulk geometry. We demonstrate the connection between critical behavior and horizon in an example, by deriving the bulk metrics that emerge in various phases of the U(N ) vector model in the large N limit based on the holographic dual constructed from quantum renormalization group. The gapped phase exhibits a geometry that smoothly ends at a finite proper distance in the radial direction. The geometric distance in the radial direction measures a complexity: the depth of renormalization group transformation that is needed to project the generally entangled UV state to a direct product state in the IR. For gapless states, entanglement persistently spreads out to larger length scales, and the initial state can not be projected to the direct product state. The obstruction to smooth projection at charge neutral point manifests itself as the long throat in the anti-de Sitter space. The Poincare horizon at infinity marks the critical point which exhibits a divergent length scale in the spread of entanglement. For the gapless states with non-zero chemical potential, the bulk space becomes the Lifshitz geometry with the dynamical critical exponent two. The identification of horizon as critical point may provide an explanation for the universality of horizon. We also discuss the structure of the bulk tensor network that emerges from the quantum renormalization group.

show abstract

“…4 At such a phase boundary layer, the energy density ρ of the squeezed vacuum can increase very rapidly. Having positive vacuum energy ρ and negative pressure p = −ρ, the interior of the "black hole" acts as a repulsive core, preventing further collapse.…”

Section: Readers' Forummentioning

confidence: 99%

More on black holes and quantum information

Biswas

2013

Physics Today

View full text Add to dashboard Cite

Quantum phase transitions and the breakdown of classical general relativity

Cited by 75 publications

References 16 publications

Slowly rotating supercompact Schwarzschild stars

Slowly rotating supercompact Schwarzschild stars

Horizon as critical phenomenon

More on black holes and quantum information

Contact Info

Product

Resources

About