=== AMALDI GW sources ===

Deirdre Shoemaker - NR waveforms for data analysis

- PSU waveforms
- Do match (not FF) between no-spin and spinning with quadrupole only; very high values
- A bit lower (5-10%) by including higher modes and considering higher inclinations
- No precession---aligned spins ("axial case")

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Alessandro Spallicci - Radiation reaction of capture sources for LISA

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Ulrich Sperhake - Mining information from unequal-mass binaries (w/Berti, Cardoso, ...)

- two code families: generalized harmonic and moving punctures
- three categories of results: astrophysics (kicks), GW detection, mathematics
- comparison with analytic results: consistency, convergence, etc.

- nonspinning, unequal mass (1:1-4) BHs, 7M separation (~600M duration)

- total Erad, jfin decrease at larger mass ratios
- Erad in higher modes - 10%
- excellent agreement with 2.5PN inspiral frequences
- ringdown predictions for j_fin agree well with radiation estimates
- quality factor nearly constant

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Gabe Perez-Giz - Kerr dynamics and their imprint on gravitational waves

- qualitative distinction between two types of Kerr perihelion-precessing orbits: ordinary and zoom-whirl
- very specific waves!
	- is this behavior generic?
	- is there a definable boundary?
	- are they detectable
- zoom-whirl is an extreme form of perihelion precession, not usually captured by perturbative treatments of circular orbits
- rethink perihelion precession from the Hamiltonian system
	- Poincaré section
	- there is a measure zero set of orbits where perihelion precession does not happen (2pi-periodic orbits); that's the beginning of zoom-whirl
		- these are dense in phase space, and are close to zoom-whirl
		- homoclinic orbits
	- can use linearized equations
- dynamical generality of homoclinic orbits

- adiabatic evolution through whirl phase? may be able to look for localized power excess

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Sam Finn - measuring the propagation speed of gravitational waves

- 1676: Roemer predicts eclipse time variations from finite speed of light
- use GW periodic sources to measure c_gw from Doppler effect
- clocks for GWs:
	- GEO, LIGO: NS (1-10 ms) -> 1e-6 in c_gw at SNR = 10
	- LISA: WD (100-1000 s) -> 1e-4 in c_gw at SNR = 10
- compare how with graviton

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Ryuichi Takahashi - lensing of amplitude and phase in gravitational waveforms

- GW propagating across CDM density perturbation
- lensing errors: few percent in luminosity distance
	- geometrical optics
- for LISA redshift determination, lensing errors exceed intrinsic LISA errors
- using wave optics, phase is also changed
	- 10^-3 rad rms phase fluctuation

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Laszlo Gergely - supermassive BH binary mergers

- in X-shaped radio galaxies, angles between jets 45 deg
- spin flip: dominant BH spin changes direction due to interaction with smaller BH
- galactic mergers lead to SMBH mergers via dynamical friction + radiation reaction
- most common mass ratios should range from 30:1 to 3:1
- find that spin flip occurs in inspiral
- orbital momentum dominates at beginning, spin at end
- spin turns to direction of orbital angular momentum
- spin precession causes superwind

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Daniel Figueroa - GW background from reheating after inflation

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J de Araujo - GW background from NS phase transition

- hadron-quark phase transition in inner NS shells
- star formation according to Springel & Hernquist (2003)
- with NS spin down, centrifugal force decreases and the central density increases
	-> phase transition with formation of strange-matter core