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Inspiral of Comparable Mass Binaries
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[Web Page]
[Group members]
[Mailing list and Archive]
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| Source Analysis Facilitators:
Bala Iyer (PN) and Thomas Baumgarte
(numerical) | |
| Data Analysis Facilitator: Jolien
Creighton | |
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The late stages of inspiral, up to the final plunge and merger,
for BH/BH, NS/BH, and NS/NS binaries, including spin-induced
precession. Source analysis currently being carried out via
post-Newtonian methods, resummation methods (Pade approximates,
effective one-body), and numerical relativity methods (with
helical killing vector field, and/or conformally flat space
slices, and/or standing-wave boundary conditions). Data
analysis currently via matched filters using post-Newtonian or
kludged waveforms, and by fast chirp transform.
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BH/BH Merger
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[Web Page]
[Group members]
[Mailing list and Archive]
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| Source Analysis Facilitators: Berndt Bruegmann and Luis Lehner | |
| Data Analysis Facilitator: Patrick
Brady | |
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[LIGO/VIRGO/GEO/TAMA, Bars, and LISA] Plunge from the isco
and final merger. Source analysis is currently by numerical
relativity techniques. Data analysis is currently via various
time-frequency techniques.
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NS/NS and NS/BH Merger
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[Web Page]
[Group members]
[Mailing list and Archive]
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| Source Analysis Facilitators: Fred Rasio and Masaru Shibata | |
| Data Analysis Facilitator: Ben
Owen | |
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[LIGO/VIRGO/GEO/TAMA and Bars] For NS/NS binaries: plunge
induced by combined GR and tidal couplings; bar formation and
evolution; oscillations. For NS/BH: tidal disruption of the NS
by the BH. Source analysis is currently by numerical
simulations (Newtonian, post-Newtonian, and fully
relativistic). Data analysis is currently via various
time-frequency techniques.
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Stellar Collapse
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[Web Page]
[Group members]
[Mailing list and Archive]
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| Source Analysis Facilitators: Tony
Mezzacappa | |
| Data Analysis Facilitator: Warren
Anderson | |
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[LIGO/VIRGO/GEO/TAMA, Bars, and LISA] Core collapse at end of
stellar evolution, to form a neutron star, a centrifugally
hung-up protoneutron star, and/or a black hole.
Accretion-induced collapse of a white dwarf. Collapse of a
supermassive star [LISA]. Instabilities: dynamical or secular
bar formation, CFS instabilities, r-modes. Convection. Source
analysis is currently by numerical simulations (Newtonian,
post-Newtonian, and fully relativistic), and by construction of
equilibria and study of their stability and dynamics. Data
analysis is currently via time-frequency techniques.
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Stochastic
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[Web Page]
[Group members]
[Mailing list and Archive]
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| Source Analysis Facilitator:
Tania Regimbau | |
| Data Analysis Facilitator:
John Whelan | |
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[LIGO/VIRGO/GEO/TAMA, Bars, and LISA] Primordial waves from
inflation; waves from processes in very early universe (phase
transitions, topological defects, brane scenarios); background
due to superposition of discrete sources (white dwarf binaries,
compact body inspiral, ...). Source analysis by a variety of
techniques, depending on the source. Data analysis by cross
correlation of detector outputs.
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Compact Body Inspiral into SMBH
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[Web Page]
[Group members]
[Mailing list and Archive]
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| Source Analysis Facilitators: Scott
Hughes | |
| Data Analysis Facilitator: Curt
Cutler | |
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[LISA] WD's, NS's, and stellar mass BH's captured into
small-periastron orbits around a supermassive black hole (SMBH)
in a galactic nucleus; evolution of the orbits under radiation
reaction and via pertubations of other orbiting objects and via
interaction with accretion disks; transition to plunge and
capture. Source analysis via black-hole perturbation theory
(waveform computations) and via N-body simulations (capture
computations as input for estimating capture rates) Data
analysis expected to be by hierarchical techniques that involve
mixed coherent (matched-filter) and incoherent methods. Data
analysis work includes separating the strongest sources from
the background of weaker inpiral waves and WD/WD binary waves.
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