Book contents
- Frontmatter
- Contents
- Foreword
- Acknowledgments
- Introduction
- Notation
- 1 Superluminal motion in the quasar 3C273
- 2 Curved spacetime and SgrA*
- 3 Parallel transport and isometry of tangent bundles
- 4 Maxwell's equations
- 5 Riemannian curvature
- 6 Gravitational radiation
- 7 Cosmological event rates
- 8 Compressible fluid dynamics
- 9 Waves in relativistic magnetohydrodynamics
- 10 Nonaxisymmetric waves in a torus
- 11 Phenomenology of GRB supernovae
- 12 Kerr black holes
- 13 Luminous black holes
- 14 A luminous torus in gravitational radiation
- 15 GRB supernovae from rotating black holes
- 16 Observational opportunities for LIGO and Virgo
- 17 Epilogue: GRB/XRF singlets, doublets? Triplets!
- Appendix A Landau's derivation of a maximal mass
- Appendix B Thermodynamics of luminous black holes
- Appendix C Spin–orbit coupling in the ergotube
- Appendix D Pair creation in a Wald field
- Appendix E Black hole spacetimes in the complex plan
- Appendix F Some units, constants and numbers
- References
- Index
16 - Observational opportunities for LIGO and Virgo
Published online by Cambridge University Press: 17 August 2009
- Frontmatter
- Contents
- Foreword
- Acknowledgments
- Introduction
- Notation
- 1 Superluminal motion in the quasar 3C273
- 2 Curved spacetime and SgrA*
- 3 Parallel transport and isometry of tangent bundles
- 4 Maxwell's equations
- 5 Riemannian curvature
- 6 Gravitational radiation
- 7 Cosmological event rates
- 8 Compressible fluid dynamics
- 9 Waves in relativistic magnetohydrodynamics
- 10 Nonaxisymmetric waves in a torus
- 11 Phenomenology of GRB supernovae
- 12 Kerr black holes
- 13 Luminous black holes
- 14 A luminous torus in gravitational radiation
- 15 GRB supernovae from rotating black holes
- 16 Observational opportunities for LIGO and Virgo
- 17 Epilogue: GRB/XRF singlets, doublets? Triplets!
- Appendix A Landau's derivation of a maximal mass
- Appendix B Thermodynamics of luminous black holes
- Appendix C Spin–orbit coupling in the ergotube
- Appendix D Pair creation in a Wald field
- Appendix E Black hole spacetimes in the complex plan
- Appendix F Some units, constants and numbers
- References
- Index
Summary
“Measure what is measurable, and make measurable what is not so.”
Galileo Galilei (1564–1642), in H. Weyl, Mathematics and the Laws of Nature.“Wir müssen wissen. Wir werden wissen.”
David Hilbert (1862–1943), engraved on his tombstone in Göttingen.Gravitational wave detectors LIGO[2, 34], Virgo[78, 4, 503] shown in Figure 16.1, GEO[147, 601] and TAMA[15] are broad band detectors, sensitive in a frequency range of about 20–2000 Hz. The laser interferometric detectors are based on Michelson interferometry, and have a characteristic right angle between their two arms for optimal sensitivity for spin-2 waves[476]. At low frequencies (approximately less than 50 Hz), observation is limited by unfiltered seismic noise. In a middle band of up to about 150 Hz, it is limited by thermal noise and, at high frequencies above a few hundred Hz, by shot noise[495]. The design bandwidth of these detectors is chosen largely by the expected gravitational wave frequencies emitted in the final stages of binary neutron star coalescence, i.e. frequencies up to a few hundred Hz produced by compact stellar mass objects. At these frequencies, the detectors operate in the short wavelength limit, wherein the signal increases linearly with the length of the arms. It is therefore advantageous to build detectors with arm lengths as long as is practically feasible, given that many noise sources are independent of the arm length.
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- Publisher: Cambridge University PressPrint publication year: 2005