GWAWG Gravitational Wave Analysis Groups     
    
ACIGA | GEO | LIGO | LISA | TAMA | VIRGO  
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Inspiral of Comparable Mass Binaries [Web Page] [Group members] [Mailing list and Archive]
Source Analysis Facilitators: Bala Iyer (PN) and Thomas Baumgarte (numerical) 
Data Analysis Facilitator: Jolien Creighton 
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.

BH/BH Merger [Web Page] [Group members] [Mailing list and Archive]
Source Analysis Facilitators: Berndt Bruegmann and Luis Lehner 
Data Analysis Facilitator: Patrick Brady 
[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.

NS/NS and NS/BH Merger [Web Page] [Group members] [Mailing list and Archive]
Source Analysis Facilitators: Fred Rasio and Masaru Shibata 
Data Analysis Facilitator: Ben Owen 
[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.

Stellar Collapse [Web Page] [Group members] [Mailing list and Archive]
Source Analysis Facilitators: Tony Mezzacappa 
Data Analysis Facilitator: Warren Anderson 
[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.

Stochastic [Web Page] [Group members] [Mailing list and Archive]
Source Analysis Facilitator: Tania Regimbau 
Data Analysis Facilitator: John Whelan 
[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.

Compact Body Inspiral into SMBH [Web Page] [Group members] [Mailing list and Archive]
Source Analysis Facilitators: Scott Hughes 
Data Analysis Facilitator: Curt Cutler 
[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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Last modified: Wed Dec 31 18:00:00 1969