Melanie Chanona
Current Organizations / Institutes
The organizations/institutes from the scholar's latest article
Research Subjects
Melanie Chanona has a total of 8 co-authors. Here are the top co-authors by number of shared publications:
- Robert B. Mann
University of Waterloo
4 shared publications - Richard J. Epp
Department of Physics and Astronomy University of Waterloo 200 University Avenue West N2L 3G1 Waterloo Ontario Canada
2 shared publications Michael J Koop
Pennsylvania State University
1 shared publicationMichael J. Koop
Department of Physics The Pennsylvania State University 16802-6300 PA USA
1 shared publication- Paul L. McGrath
Department of Physics and Astronomy University of Waterloo N2L 3G1 Waterloo Ontario Canada
1 shared publication - Paul L. McGrath
Department of Physics and Astronomy University of Waterloo 200 University Avenue West N2L 3G1 Waterloo Ontario Canada
1 shared publication
Latest Publications
- 16 April 2014
- Published by IOP Publishing in Classical and Quantum Gravity
- Vol. 31 (9) , 95006
Post-Newtonian conservation laws in rigid quasilocal frames
- 16 April 2014
- Published by IOP Publishing in Classical and Quantum Gravity
- Vol. 31 (9) , 95006
Post-Newtonian conservation laws in rigid quasilocal frames
- 14 February 2014
- Published by American Physical Society (APS) in Physical Review D
- Vol. 89 (4)
Numerical boson stars with a single Killing vector. II. ThecaseWe complete the analysis of part I in this series [S. Stotyn et. al.,Phys. Rev. D 89, 044017 (2014)
- 14 February 2014
- Published by American Physical Society (APS) in Physical Review D
- Vol. 89 (4)
Numerical boson stars with a single Killing vector. II. ThecaseWe complete the analysis of part I in this series [S. Stotyn et. al.,Phys. Rev. D 89, 044017 (2014)
- Open Access
Post-Newtonian Conservation Laws in Rigid Quasilocal Frames
In recent work we constructed completely general conservation laws for energy and linear and angular momentum of extended systems in general relativity based on the notion of a rigid quasilocal frame (RQF). We argued at a fundamental level that these RQF conservation laws are superior to conservation laws based on the local stress-energy-momentum tensor of matter because (1) they do not rely on spacetime symmetries and (2) they properly account for both matter and gravitational effects. Moreover, they provide simple, exact, operational expressions for fluxes of gravitational energy and linear and angular momentum. In this paper we derive the form of these laws in a general first post-Newtonian (1PN) approximation, and then apply these approximate laws to the problem of gravitational tidal interactions. We obtain formulas for tidal heating and tidal torque that agree with the literature, but without resorting to the use of pseudotensors. We describe the physical mechanism of these tidal interactions not in the traditional terms of a Newtonian gravitational force, but in terms of a much simpler and universal mechanism that is an exact, quasilocal manifestation of the equivalence principle in general relativity. As concrete examples, we look at the tidal heating of Jupiter's moon Io and angular momentum transfer in the Earth-Moon system that causes a gradual spin-down of the Earth and recession of the Moon. In both examples we find agreement with observation.
Open AccessPost-Newtonian Conservation Laws in Rigid Quasilocal Frames
In recent work we constructed completely general conservation laws for energy and linear and angular momentum of extended systems in general relativity based on the notion of a rigid quasilocal frame (RQF). We argued at a fundamental level that these RQF conservation laws are superior to conservation laws based on the local stress-energy-momentum tensor of matter because (1) they do not rely on spacetime symmetries and (2) they properly account for both matter and gravitational effects. Moreover, they provide simple, exact, operational expressions for fluxes of gravitational energy and linear and angular momentum. In this paper we derive the form of these laws in a general first post-Newtonian (1PN) approximation, and then apply these approximate laws to the problem of gravitational tidal interactions. We obtain formulas for tidal heating and tidal torque that agree with the literature, but without resorting to the use of pseudotensors. We describe the physical mechanism of these tidal interactions not in the traditional terms of a Newtonian gravitational force, but in terms of a much simpler and universal mechanism that is an exact, quasilocal manifestation of the equivalence principle in general relativity. As concrete examples, we look at the tidal heating of Jupiter's moon Io and angular momentum transfer in the Earth-Moon system that causes a gradual spin-down of the Earth and recession of the Moon. In both examples we find agreement with observation.
- Open Access
Numerical Boson Stars with a Single Killing Vector II: the D=3 Case
We complete the analysis of part I in this series (Ref. \cite{Stotyn:2013yka}) by numerically constructing boson stars in 2+1 dimensional Einstein gravity with negative cosmological constant, minimally coupled to a complex scalar field. These lower dimensional boson stars have strikingly different properties than their higher dimensional counterparts, most noticeably that there exists a finite central energy density, above which an extremal BTZ black hole forms. In this limit, all of the scalar field becomes enclosed by the horizon; it does not contract to a singularity, but rather the origin remains smooth and regular and the solution represents a spinning boson star trapped inside a degenerate horizon. Additionally, whereas in higher dimensions the mass, angular momentum, and angular velocity all display damped harmonic oscillations as functions of the central energy density, in $D=3$ these quantities change monotonically up to the bound on the central energy density. Some implications for the holographic dual of these objects are discussed and it is argued that the boson star and extremal BTZ black hole phases are dual to a spontaneous symmetry breaking at zero temperature but finite energy scale.Open AccessNumerical Boson Stars with a Single Killing Vector II: the D=3 Case
We complete the analysis of part I in this series (Ref. \cite{Stotyn:2013yka}) by numerically constructing boson stars in 2+1 dimensional Einstein gravity with negative cosmological constant, minimally coupled to a complex scalar field. These lower dimensional boson stars have strikingly different properties than their higher dimensional counterparts, most noticeably that there exists a finite central energy density, above which an extremal BTZ black hole forms. In this limit, all of the scalar field becomes enclosed by the horizon; it does not contract to a singularity, but rather the origin remains smooth and regular and the solution represents a spinning boson star trapped inside a degenerate horizon. Additionally, whereas in higher dimensions the mass, angular momentum, and angular velocity all display damped harmonic oscillations as functions of the central energy density, in $D=3$ these quantities change monotonically up to the bound on the central energy density. Some implications for the holographic dual of these objects are discussed and it is argued that the boson star and extremal BTZ black hole phases are dual to a spontaneous symmetry breaking at zero temperature but finite energy scale.