Numerical Relativity
The aim of Numerical Relativity is to solve Einstein's equations by numerical means.
This approach allows to survey the unknown solution space of the Einstein equations.
Perhaps the main current focus is to provide gravitational waveform templates for the
upcoming laser interferometers.
Challenging problems:
Mathematical difficulties (PDEs with hundreds of terms, mixed hyperbolic
and elliptic character, stability, gauge conditions, etc).
Enormous computational resources needed in 3D.
Experience in different formulations of the relativistic field equations:
3+1 formulation:
Papadopoulos, Font
Phys. Rev. D, 59, 044014 (1999)
Brandt, Font, Ibanez, Masso, Seidel
Comp. Phys. Comm., 124, 169 (2000)
Font, Miller, Suen, Tobias
Phys. Rev. D, 61, 044011 (2000)
Alcubierre et al
Phys. Rev. D, 62, 044034 (2000)
Font et al
Phys. Rev. D, 65, 084024 (2002)
Baiotti et al
Phys. Rev. D, submitted (2004)
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Characteristic formulation:
Papadopoulos, Font
Phys. Rev. D, 61, 024015 (2000)
Papadopoulos, Font
Phys. Rev. D, 63, 044016 (2001)
Linke, Font, Janka, Müller, Papadopoulos
Astron. Astrophys. 376, 568 (2001)
Siebel, Font, Papadopoulos
Phys. Rev. D, 65, 024021 (2002)
Siebel, Font, Müller, Papadopoulos
Phys. Rev. D, 65, 064038 (2002)
Siebel, Font, Müller, Papadopoulos
Phys. Rev. D, 67, 124018 (2003)
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Conformally-flat metric (Isenberg-Wilson):
Dimmelmeier, Font, Müller
Astrophys. J. Lett. 560, L163-L166 (2001)
Dimmelmeier, Font, Müller
Class. Quantum Grav. 19, 1291-1296 (2002)
Dimmelmeier, Font, Müller
Astron. Astrophys. 388, 917-935 (2002)
Dimmelmeier, Font, Müller
Astron. Astrophys. 393, 523-542 (2002)
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Click here for recent
results on 3D simulations performed with the
whisky code
showing the formation of Kerr black holes as a result of the gravitational collapse
of rotating relativistic stars.
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