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Institutsdirektor
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Scientific Interests
My main scientific interest is currently the two body problem for two black holes. The classical two body problem in physics is formulated for two point-like masses. In Newtonian physics this problem has the well-known solution in terms of Kepler orbits, but do we really understand how two masses move in their mutual gravitational field? As surprising as it may seem at first, the answer to this question is not really known, even if we restrict ourselves to classical, non-quantum physics and to no more than two bodies.
A modern treatment of the two body problem must be founded on Einstein's theory of general relativity, which by all accounts is an extremely successful description of the gravitational interaction in the classical regime. In the limit of velocities much below the speed of light and for weak gravitational fields, Newton's theory of gravity is an excellent approximation and with post-Newtonian approximations we can obtain good approximations for about one tenth of the speed of light. However, the question has to be asked how for example two black holes, which are prime examples for extreme gravity, move around each other when they approach each other at relativistic velocities.
Is there perhaps in general relativity a solution to the equations of motion for two black holes which is as simple and simultaneously as astrophysically relevant as the Kepler orbits of Newtonian physics? The answer is, in a rather satisfying manner, no! The motion of two masses generates gravitational waves, which remove energy and momentum from the system, such that a Kepler ellipse is no longer a stable solution for an orbit. Two black holes will rather move on an inward spiral, first slowly, then faster and faster, until they collide and merge to a single black hole.
This loss of stability in the Einstein equations is by no means tragic. Quite to the contrary, a growing international community of gravitational wave researchers hopes that gravitational waves can be detected in order to establish an entirely new branch of astronomy, namely gravitational wave astronomy. Gravitational waves have not been directly detected yet, but detectors are in operation and further improvements are under development, which should lead to the first detection in a matter of years.
My own work has been focussed on numerical simulations of black hole space times. The two-body problem of general relativity in the strong field regime is still not satisfactorily solved, although there has been significant progress in the last few years. The numerical solution of the full Einstein equations (in their standard form ten non-linear, coupled partial differential equations) is a very complex problem, and for two black holes there is the additional challenge to deal with the spacetime singularities that are encountered in the interior of black holes. Given initial data for configurations of two black holes, the time evolution of the system is computed. Currently, typical runs are limited by the achievable evolution time before the simulations become too inaccurate or before the computer code becomes unstable and crashes at numerical infinities. State of the art are simulations that cover about four full orbits of two black holes shortly before their merger.
Astrophysical considerations make it likely that the last few orbits of two black holes and the ensuing collision are the source of particularly strong gravitational waves. The final phase of a binary system of two black holes with a total mass of about 30 solar masses constitutes one of the most likely sources for the gravitational wave detectors GEO and LIGO based on the frequency dependent sensitivity of these interferometric detectors. The planned space based detector LISA will detect gravitational waves from the mergers of supermassive black holes at the center of galaxies, to which our numerical simulations apply equally well. This area of numerical relativity requires the development of new analytical and numerical methods, as well as their implementation on supercomputers.
FIGURES
Albert Einstein Institute: black hole merger
Link to the related paper in gr-qc.
This figure is based on the first ever simulations of the gravitational waves produced by the merger of two black holes in full numerical relativity. The black holes are represented by colored
balls
(actually the so-called apparent horizon), where the color indicates the local Gauss curvature. The wavy features are isosurfaces based on the psi4 Newman-Penrose scalar. The two black holes have just merged and a strong pulse of waves is sent into space.
(Phys.Rev.Lett. 87 (2001) 271103, simulations performed by our group at the Albert Einstein Institute, the Max Planck Institute of Gravitational Physics, visualisation by W. Benger, ZIB.)
Penn State University: Black hole orbit Link to the related paper in gr-qc.
Numerical simulations of black holes have to contend with the complexity of the Einstein equations, many sources of potential numerical instabilities, and the physical singularity lurking inside black holes. The figure shows a snapshot of the first numerical simulations of two black holes that was sufficiently stable so that the black holes completed even just one orbit.
My main scientific interest is currently the two body problem for two black holes. The classical two body problem in physics is formulated for two point-like masses. In Newtonian physics this problem has the well-known solution in terms of Kepler orbits, but do we really understand how two masses move in their mutual gravitational field? As surprising as it may seem at first, the answer to this question is not really known, even if we restrict ourselves to classical, non-quantum physics and to no more than two bodies.
A modern treatment of the two body problem must be founded on Einstein's theory of general relativity, which by all accounts is an extremely successful description of the gravitational interaction in the classical regime. In the limit of velocities much below the speed of light and for weak gravitational fields, Newton's theory of gravity is an excellent approximation and with post-Newtonian approximations we can obtain good approximations for about one tenth of the speed of light. However, the question has to be asked how for example two black holes or neutron stars, which are prime examples for extreme gravity, move around each other when they approach each other at relativistic velocities.
Is there perhaps in general relativity a solution to the equations of motion for two black holes which is as simple and simultaneously as astrophysically relevant as the Kepler orbits of Newtonian physics? The answer is, in a rather satisfying manner, no! The motion of two masses generates gravitational waves, which remove energy and momentum from the system, such that a Kepler ellipse is no longer a stable solution for an orbit. Two black holes will rather move on an inward spiral, first slowly, then faster and faster, until they collide and merge to a single black hole.
This loss of stability in the Einstein equations is by no means tragic. Quite to the contrary, a growing international community of gravitational wave researchers hopes that gravitational waves can be detected in order to establish an entirely new branch of astronomy, namely gravitational wave astronomy. In fact, the very first direct detection of gravitational waves happened on September 14, 2015, and there is strong evidence that the source was a binary black hole inspiral and merger.
My own work has been focussed on numerical simulations of black hole and neutron star space times. The two-body problem of general relativity in the strong field regime is still not satisfactorily solved, although there has been significant progress in the last few years. The numerical solution of the full Einstein equations (in their standard form ten non-linear, coupled partial differential equations) is a very complex problem, and for black holes there is the additional challenge to deal with the spacetime singularities that are encountered in the interior of black holes. Given initial data for configurations of two black holes or neutron stars, the time evolution of the system is computed.
Astrophysical considerations make it likely that the last few orbits of two compact objects like black holes or neutron stars and the ensuing collision are the source of particularly strong gravitational waves. The final phase of a binary system of two black holes with a total mass of about 30 solar masses constitutes one of the most likely sources for the gravitational wave detectors GEO and LIGO based on the frequency dependent sensitivity of these interferometric detectors. The planned space based detector LISA will detect gravitational waves from the mergers of supermassive black holes at the center of galaxies, to which our numerical simulations apply equally well. This area of numerical relativity requires the development of new analytical and numerical methods, as well as their implementation on supercomputers.
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Publications and Teaching
Teaching
Papers
<a class="wiki external" target="_blank" href="https://www.tpi.uni-jena.de/tiki-index.php?page=MasterProgramme " rel="external nofollow"> Guide to the M.Sc. in Physics with focus on "Gravitational- and Quantum Field Theory" at the University of Jena</a>
Teaching
Papers
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Photo
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Photo
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Email
Bernd.Bruegmann@uni-jena.de
Bernd.Bruegmann@uni-jena.de
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Curriculum Vitae
1987. M.S. in Mathematics, Syracuse University, USA
1993. Ph.D. in Physics, Syracuse University, USA
1993 - 1995. MPI for Physics, Munich, Germany
1995 - 2002. MPI for Gravitational Physics, Potsdam, Germany
2002 - 2004. Associate Professor, Penn State University, USA
2004 - ... Professor, Chair for Gravitational Theory, University of Jena, Germany
1987. M.S. in Mathematics, Syracuse University, USA
1993. Ph.D. in Physics, Syracuse University, USA
1993 - 1995. MPI for Physics, Munich, Germany
1995 - 2002. MPI for Gravitational Physics, Potsdam, Germany
2002 - 2004. Associate Professor, Penn State University, USA
2004 - ... Professor, Chair for Gravitational Theory, University of Jena, Germany
2
02:28
83
Curriculum Vitae
1987. M.S. in Mathematics, Syracuse University, USA
1993. Ph.D. in Physics, Syracuse University, USA
1993 - 1995. MPI for Physics, Munich, Germany
1995 - 2002. MPI for Gravitational Physics, Potsdam, Germany
2002 - 2004. Associate Professor, Penn State University, USA
2004 - ... Professor, Chair for Gravitational Theory, University of Jena, Germany
1987. M.S. in Mathematics, Syracuse University, USA
1993. Ph.D. in Physics, Syracuse University, USA
1993 - 1995. MPI for Physics, Munich, Germany
1995 - 2002. MPI for Gravitational Physics, Potsdam, Germany
2002 - 2004. Associate Professor, Penn State University, USA
2004 - ... Professor, Chair for Gravitational Theory, University of Jena, Germany
1
02:28
34
Publications and Teaching
https://lsf.uni-jena.de/qisserver/rds?state=wsearchv&search=1&subdir=veranstaltung&choice.veranstaltung.semester=y&alias_pord.pordnr=r_zuordpos.pordnr&personal.nachname=br%C3%BCgmann&veranstaltung.semester=20092&alias_pord.pordnr=r_zuordpos.pordnr&P_start=0&P_anzahl=10&P.sort=&_form=display
http://www.slac.stanford.edu/spires/find/hep/www?rawcmd=FIND+A+BRUGMANN%2C+BERND+OR+A+BRUEGMANN%2C+BERND&FORMAT=www&SEQUENCE=
Teaching
Papers
1
02:28
83
Curriculum Vitae
1987. M.S. in Mathematics, Syracuse University, USA
1993. Ph.D. in Physics, Syracuse University, USA
1993 - 1995. MPI for Physics, Munich, Germany
1995 - 2002. MPI for Gravitational Physics, Potsdam, Germany
2002 - 2004. Associate Professor, Penn State University, USA
2004 - ... Professor, Chair for Gravitational Theory, University of Jena, Germany
1987. M.S. in Mathematics, Syracuse University, USA
1993. Ph.D. in Physics, Syracuse University, USA
1993 - 1995. MPI for Physics, Munich, Germany
1995 - 2002. MPI for Gravitational Physics, Potsdam, Germany
2002 - 2004. Associate Professor, Penn State University, USA
2004 - ... Professor, Chair for Gravitational Theory, University of Jena, Germany
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