Sean Stotyn
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The organizations/institutes from the scholar's latest article
Previous Organizations / Institutes
The organizations / institutes from the scholar's other articles in the past ten years
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Sean Stotyn has a total of 23 co-authors. Here are the top co-authors by number of shared publications:
- Robert B. Mann
University of Waterloo
13 shared publications Laura J. Henderson
Department of Physics and Astronomy, University of Waterloo, Waterloo, Ontario, Canada N2L 3G1
4 shared publications- Amitabh Virmani
Chennai Mathematical Institute
2 shared publications - C. Danielle Leonard
Astrophysics University of Oxford Denys Wilkinson Building Keble Road OX1 3RH Oxford UK
2 shared publications - Geoffrey Compère
University of California CA-93106 Santa Barbara Santa Barbara United States
2 shared publications - Marius Oltean
Department of Physics and Astronomy University of Waterloo N2L 3G1 Waterloo Ontario Canada
2 shared publications
Latest Publications
- Open Access
- 15 April 2021
- Published by Springer Nature in The European Physical Journal C
- Vol. 81 (4) , 1-15
Quasilocal Smarr relation for an asymptotically flat spacetime
We investigate the thermodynamics of Einstein–Maxwell (-dilaton) theory for an asymptotically flat spacetime in a quasilocal frame. We firstly define a quasilocal thermodynamic potential via the Euclidean on-shell action and formulate a quasilocal Smarr relation from Euler’s theorem. Then we calculate the quasilocal energy and surface pressure by employing a Brown–York quasilocal method along with Mann–Marolf counterterm and find entropy from the quasilocal thermodynamic potential. These quasilocal variables are consistent with the Tolman temperature and the entropy in a quasilocal frame turns out to be same as the Bekenstein–Hawking entropy. As a result, we found that a surface pressure term and its conjugate variable, a quasilocal area, do not participate in a quasilocal thermodynamic potential, but should be present in a quasilocal Smarr relation and the quasilocal first law of black hole thermodynamics. For dyonic black hole solutions having dynamic dilaton field, a non-trivial dilaton contribution should occur in the quasilocal first law but not in the quasilocal Smarr relation.
- 15 April 2021
- Published by Springer Nature in The European Physical Journal C
- Vol. 81 (4) , 1-15
Open AccessQuasilocal Smarr relation for an asymptotically flat spacetime
We investigate the thermodynamics of Einstein–Maxwell (-dilaton) theory for an asymptotically flat spacetime in a quasilocal frame. We firstly define a quasilocal thermodynamic potential via the Euclidean on-shell action and formulate a quasilocal Smarr relation from Euler’s theorem. Then we calculate the quasilocal energy and surface pressure by employing a Brown–York quasilocal method along with Mann–Marolf counterterm and find entropy from the quasilocal thermodynamic potential. These quasilocal variables are consistent with the Tolman temperature and the entropy in a quasilocal frame turns out to be same as the Bekenstein–Hawking entropy. As a result, we found that a surface pressure term and its conjugate variable, a quasilocal area, do not participate in a quasilocal thermodynamic potential, but should be present in a quasilocal Smarr relation and the quasilocal first law of black hole thermodynamics. For dyonic black hole solutions having dynamic dilaton field, a non-trivial dilaton contribution should occur in the quasilocal first law but not in the quasilocal Smarr relation.
- Open Access
Quasilocal Smarr relation for an asymptotically flat spacetime
We investigate the thermodynamics of Einstein-Maxwell(-Dilaton) theory for an asymptotically flat spacetime in a quasilocal frame. We firstly define a quasilocal thermodynamic potential via the Euclidean on-shell action and formulate a quasilocal Smarr relation from Eulerian theorem. Then we calculate quasilocal energy and surface pressure by employing Brown-York quasilocal method along with Mann-Marolf counterterm and find entropy from the quasilocal thermodynamic potential. These quasilocal variables are consistent with Tolman temperature and the entropy in a quasilocal frame turns out to be same as the Bekenstein-Hawking entropy. As a result, we found that a surface pressure term and its conjugate variable, a quasilocal area, do not participate in a quasilocal thermodynamic potential, but should present in a quasilocal Smarr relation and the quasilocal first law of black hole thermodynamics. For dyonic black hole solutions having dynamic dilaton field, non-trivial dilaton contribution should take part in the quasilocal first law but not in the quasilocal Smarr relation.
Open AccessQuasilocal Smarr relation for an asymptotically flat spacetime
We investigate the thermodynamics of Einstein-Maxwell(-Dilaton) theory for an asymptotically flat spacetime in a quasilocal frame. We firstly define a quasilocal thermodynamic potential via the Euclidean on-shell action and formulate a quasilocal Smarr relation from Eulerian theorem. Then we calculate quasilocal energy and surface pressure by employing Brown-York quasilocal method along with Mann-Marolf counterterm and find entropy from the quasilocal thermodynamic potential. These quasilocal variables are consistent with Tolman temperature and the entropy in a quasilocal frame turns out to be same as the Bekenstein-Hawking entropy. As a result, we found that a surface pressure term and its conjugate variable, a quasilocal area, do not participate in a quasilocal thermodynamic potential, but should present in a quasilocal Smarr relation and the quasilocal first law of black hole thermodynamics. For dyonic black hole solutions having dynamic dilaton field, non-trivial dilaton contribution should take part in the quasilocal first law but not in the quasilocal Smarr relation.
- 1 September 2015
- Published by Canadian Science Publishing in Canadian Journal of Physics
- Vol. 93 (9) , 995-998
A tale of two horizons
I revisit the fate of coinciding horizons and the volume between them in the extremal limit of spherically symmetric black holes in four space–time dimensions, focusing on the Schwarzschild – de Sitter black hole for concreteness. The two Killing horizons in the limit space–time that are traditionally identified with the limiting event horizons of the non-extremal black hole are shown to instead be generated by an enhanced symmetry of the near horizon geometry (NHG). This dismantles the interpretation of the four-volume between the horizons remaining finite in the extremal limit. The NHG is reinterpreted as a tangent space–time to the degenerate black hole horizon, and geometrical objects, such as Killing vectors and Killing horizons, are carefully mapped between the bulk and the NHG. The implications for extremal black hole entropy are then discussed.
- 1 September 2015
- Published by Canadian Science Publishing in Canadian Journal of Physics
- Vol. 93 (9) , 995-998
A tale of two horizons
I revisit the fate of coinciding horizons and the volume between them in the extremal limit of spherically symmetric black holes in four space–time dimensions, focusing on the Schwarzschild – de Sitter black hole for concreteness. The two Killing horizons in the limit space–time that are traditionally identified with the limiting event horizons of the non-extremal black hole are shown to instead be generated by an enhanced symmetry of the near horizon geometry (NHG). This dismantles the interpretation of the four-volume between the horizons remaining finite in the extremal limit. The NHG is reinterpreted as a tangent space–time to the degenerate black hole horizon, and geometrical objects, such as Killing vectors and Killing horizons, are carefully mapped between the bulk and the NHG. The implications for extremal black hole entropy are then discussed.
- 6 January 2015
- Published by American Physical Society (APS) in Physical Review D
- Vol. 91 (2) , 024009
Gauss-Bonnet boson stars with a single Killing vector
We construct asymptotically anti–de Sitter boson stars in Einstein-Gauss-Bonnet gravity coupled to a -tuplet of complex massless scalar fields both perturbatively and numerically in dimensions. These solutions possess just a single helical Killing symmetry due to the choice of scalar fields. The energy density at the center of the star characterizes the solutions, and for each choice of the Gauss-Bonnet coupling we obtain a one parameter family of solutions. All solutions respect the first law of thermodynamics, in the numerical case to within 1 part in . We describe the dependence of the angular velocity, mass, and angular momentum of the boson stars on and on the dimensionality. For these quantities reach maximum values and then decrease to eventually approach finite values as the central energy density tends to infinity. In the limit of diverging central energy density, the Kretschmann invariant at the center of the boson star also diverges. This is in contrast to the case, where the Kretschmann invariant diverges at a finite value of the central energy density.- 6 January 2015
- Published by American Physical Society (APS) in Physical Review D
- Vol. 91 (2) , 024009
Gauss-Bonnet boson stars with a single Killing vector
We construct asymptotically anti–de Sitter boson stars in Einstein-Gauss-Bonnet gravity coupled to a -tuplet of complex massless scalar fields both perturbatively and numerically in dimensions. These solutions possess just a single helical Killing symmetry due to the choice of scalar fields. The energy density at the center of the star characterizes the solutions, and for each choice of the Gauss-Bonnet coupling we obtain a one parameter family of solutions. All solutions respect the first law of thermodynamics, in the numerical case to within 1 part in . We describe the dependence of the angular velocity, mass, and angular momentum of the boson stars on and on the dimensionality. For these quantities reach maximum values and then decrease to eventually approach finite values as the central energy density tends to infinity. In the limit of diverging central energy density, the Kretschmann invariant at the center of the boson star also diverges. This is in contrast to the case, where the Kretschmann invariant diverges at a finite value of the central energy density.- Open Access
Gauss-Bonnet Boson Stars with a Single Killing Vector
We construct asymptotically anti-de Sitter boson stars in Einstein-Gauss-Bonnet gravity coupled to a $\frac{D-1}{2}$-tuplet of complex massless scalar fields both perturbatively and numerically in D=5,7,9,11 dimensions. These solutions possess just a single helical Killing symmetry due to the choice of scalar fields. The energy density at the centre of the star characterizes the solutions, and for each choice of the Gauss-Bonnet coupling $\alpha$ we obtain a one parameter family of solutions. All solutions respect the first law of thermodynamics; in the numerical case to within 1 part in $10^6$. We describe the dependence of the angular velocity, mass, and angular momentum of the boson stars on $\alpha$ and on the dimensionality. For D>5, these quantities exhibit damped oscillations about finite central values as the central energy density tends to infinity, where the amplitude of oscillation increases nonlinearly with $\alpha$. In the limit of diverging central energy density, the Kretschmann invariant at the centre of the boson star also diverges. This is in contrast to the D=5 case, where the Kretschmann invariant diverges at a finite value of the central energy density.Open AccessGauss-Bonnet Boson Stars with a Single Killing Vector
We construct asymptotically anti-de Sitter boson stars in Einstein-Gauss-Bonnet gravity coupled to a $\frac{D-1}{2}$-tuplet of complex massless scalar fields both perturbatively and numerically in D=5,7,9,11 dimensions. These solutions possess just a single helical Killing symmetry due to the choice of scalar fields. The energy density at the centre of the star characterizes the solutions, and for each choice of the Gauss-Bonnet coupling $\alpha$ we obtain a one parameter family of solutions. All solutions respect the first law of thermodynamics; in the numerical case to within 1 part in $10^6$. We describe the dependence of the angular velocity, mass, and angular momentum of the boson stars on $\alpha$ and on the dimensionality. For D>5, these quantities exhibit damped oscillations about finite central values as the central energy density tends to infinity, where the amplitude of oscillation increases nonlinearly with $\alpha$. In the limit of diverging central energy density, the Kretschmann invariant at the centre of the boson star also diverges. This is in contrast to the D=5 case, where the Kretschmann invariant diverges at a finite value of the central energy density. - 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)
- 14 February 2014
- Published by American Physical Society (APS) in Physical Review D
- Vol. 89 (4)
Numerical boson stars with a single Killing vector. I. ThecaseWe numerically construct asymptotically anti\char21{}de Sitter boson star solutions using a minimally coupled $\frac{D$-${}1}{2}$-tuplet complex scalar field in $D=5$, 7, 9, 11 dimensions. The metric admits multiple Killing vector fields in general, however the scalar fields are only invariant under a particular combination, leading to such boson star solutions possessing just a single helical Killing symmetry. These boson stars form a one parameter family of solutions, which can be parametrized by the energy density at their center. As the central energy density tends to infinity, the angular velocity, mass, and angular momentum of the boson star exhibit damped harmonic oscillations about finite central values, while the Kretschmann invariant diverges, signaling the formation of a black hole in this limit.- 14 February 2014
- Published by American Physical Society (APS) in Physical Review D
- Vol. 89 (4)
Numerical boson stars with a single Killing vector. I. ThecaseWe numerically construct asymptotically anti\char21{}de Sitter boson star solutions using a minimally coupled $\frac{D$-${}1}{2}$-tuplet complex scalar field in $D=5$, 7, 9, 11 dimensions. The metric admits multiple Killing vector fields in general, however the scalar fields are only invariant under a particular combination, leading to such boson star solutions possessing just a single helical Killing symmetry. These boson stars form a one parameter family of solutions, which can be parametrized by the energy density at their center. As the central energy density tends to infinity, the angular velocity, mass, and angular momentum of the boson star exhibit damped harmonic oscillations about finite central values, while the Kretschmann invariant diverges, signaling the formation of a black hole in this limit.- Open AccessNumerical Boson Stars with a Single Killing Vector I: the $D\ge5$ CaseWe numerically construct asymptotically anti-de Sitter boson star solutions using a minimally coupled $\frac{D-1}{2}$-tuplet complex scalar field in $D=5,7,9,11$ dimensions. The metric admits multiple Killing vector fields in general, however the scalar fields are only invariant under a particular combination, leading to such boson star solutions possessing just a single helical Killing symmetry. These boson stars form a one parameter family of solutions, which can be parametrized by the energy density at their center. As the central energy density tends to infinity, the angular velocity, mass, and angular momentum of the boson star exhibit damped harmonic oscillations about finite central values, while the Kretschmann invariant diverges, signaling the formation of a black hole in this limit.Open AccessNumerical Boson Stars with a Single Killing Vector I: the $D\ge5$ CaseWe numerically construct asymptotically anti-de Sitter boson star solutions using a minimally coupled $\frac{D-1}{2}$-tuplet complex scalar field in $D=5,7,9,11$ dimensions. The metric admits multiple Killing vector fields in general, however the scalar fields are only invariant under a particular combination, leading to such boson star solutions possessing just a single helical Killing symmetry. These boson stars form a one parameter family of solutions, which can be parametrized by the energy density at their center. As the central energy density tends to infinity, the angular velocity, mass, and angular momentum of the boson star exhibit damped harmonic oscillations about finite central values, while the Kretschmann invariant diverges, signaling the formation of a black hole in this limit.
- 4 September 2012
- Published by IOP Publishing in Journal of Physics A: Mathematical and Theoretical
- Vol. 45 (37)
Another mass gap in the BTZ geometry?
- 4 September 2012
- Published by IOP Publishing in Journal of Physics A: Mathematical and Theoretical
- Vol. 45 (37)
Another mass gap in the BTZ geometry?
- 15 February 2012
- Published by American Physical Society (APS) in Physical Review D
- Vol. 85 (4)
Black holes and boson stars with one Killing field in arbitrary odd dimensions
We extend the recent D=5 results of Dias, Horowitz, and Santos by finding asymptotically anti\char21{}de~Sitter rotating black hole and boson star solutions with scalar hair in arbitrary odd spacetime dimension. Both the black holes and the boson stars are invariant under a single Killing vector field which corotates with the scalar field and, in the black hole case, is tangent to the generator of the horizon. Furthermore, we explicitly construct boson star and small black hole (r+$\ll${}$\ell${}) solutions perturbatively assuming a small amplitude for the scalar field, resulting in solutions valid for low energies and angular momenta. We find that just as in D=5, the angular momentum is primarily carried by the scalar field in D>5, whereas unlike D=5 the energy is also primarily carried by the scalar field in D>5; the thermodynamics in D=5 are governed by both the black hole and scalar field whereas in D>5 they are governed primarily by the scalar field alone. We focus on cataloging these solutions for the spacetime dimensions of interest in string theory, namely D=5,7,9,11.
- 15 February 2012
- Published by American Physical Society (APS) in Physical Review D
- Vol. 85 (4)
Black holes and boson stars with one Killing field in arbitrary odd dimensions
We extend the recent D=5 results of Dias, Horowitz, and Santos by finding asymptotically anti\char21{}de~Sitter rotating black hole and boson star solutions with scalar hair in arbitrary odd spacetime dimension. Both the black holes and the boson stars are invariant under a single Killing vector field which corotates with the scalar field and, in the black hole case, is tangent to the generator of the horizon. Furthermore, we explicitly construct boson star and small black hole (r+$\ll${}$\ell${}) solutions perturbatively assuming a small amplitude for the scalar field, resulting in solutions valid for low energies and angular momenta. We find that just as in D=5, the angular momentum is primarily carried by the scalar field in D>5, whereas unlike D=5 the energy is also primarily carried by the scalar field in D>5; the thermodynamics in D=5 are governed by both the black hole and scalar field whereas in D>5 they are governed primarily by the scalar field alone. We focus on cataloging these solutions for the spacetime dimensions of interest in string theory, namely D=5,7,9,11.