Outline made by GN and Sterl Phyinney years ago for planned LRR

Galactic LISA science

Abstract
General properties of stellar binaries that make LISA sources
1. orbital periods 3mins-hour. → not main sequence. Must involve spiral-in (in Galaxy) or capture (dense clusters)
2. Ultra compact binaries: white dwarf, neutron star, black hole
Verification binaries -guaranteed LISA calibration sources
1. Known sources.
2. Observational plans that could lead to more known sources.
Order of magnitude estimates of disk/bulge populations, and identificationof what these are sensitive to:
1. White dwarf binaries:
  1. double spiral-in, double-degenerate channel(cf central binaries in planetary nebulae, CVs as evidence for spiral-in). 1-2.5Msun progenitors, initial separation=red giant-AGB star radii.
  2. single-degenerate, `Tutukov/Podsiadlowski' channel
  3. Sensitivity to spiral-in physics/parameters. Observational and theoretical constraints.
  4. Detached and semi-detached (AM CVn) systems. -Sensitivity to tides/transfer stability.
2. Neutron star binaries
  1. Double spiral-in. >10Msun progenitors.
  2. Sensitivity to spiral-in physics/parameters and NS natal kicks.
3. Black hole binaries
4. The universal dN/df ~ f^{-11/3} frequency spectrum for GW inspiral sources.
LISA measurements/quick overview of data analysis
1. Source f, fdot, fddot position determination precision
2. Source confusion -3mHz and individual sources > vs background+spikes <
3. Mock data challenge results demonstrating feasibility.
4. What do GW add to EM observations
  1. Completeness -no extinction, no selection, whole galaxy. Populations!
  2. Polarisations → orbit inclinations (may check 1 or 2 nearby cases with SIM-like interferometers -otherwise big help on mass determinations for EM id's), position angles.
  3. If pure 2 point mass systems, f, fdot → chirp mass; fddot → mass ratio and hence M1, M2
5. Joint EM-GW data
Gravitational wave signal
1. Pure 2 point mass GW (f, fdot → distance → galactic structure.
2. vs tides (no distance
  1. Tidal effects on fdot, fddot.
  2. Tidal heating -electromagnetic consequences (deep-none; shallow-bright)
3. mass transfer (no distance, but
  1. RXJ0806 wrong fdot sign… -confusion -can't tell pure 2 point mass from mass transfer from GW alone. Need GW+EM.
Detailed population synthesis estimates and observational constraints for disk/bulge populations:
1. White dwarf binaries I: double white dwarfs
  1. Formation, population estimates (obs. & theory)
  2. Uncertainties
  3. LISA science: foreground (#, masses) indiv. sources (#, parameters), distribution, tidal interaction
2. White dwarfs binaries II: AM CVn stars
  1. Formation, population estimates (obs. & theory)
  2. Uncertainties
  3. LISA science: #, parameters, distribution, mass transfer stability
3. Neutron star binaries (inc. UCXBs)
  1. Types, formation, population estimates (obs & theory)
  2. Uncertainties
  3. LISA science: #, eccentricities, kicks, progenitor masses?
4. Black hole binaries
  1. Types, formation, population estimates (theory)
  2. Uncertainties
  3. LISA science: existence, numbers, kicks, progenitor masses?
5. Others: CVs, WD+Mstar, W UMa's, sdB binaries
Formation processes in dense stellar clusters
1. Tidal capture (UCXBs)
2. Exchange
3. Other (collision, gw capture…)
4. Galactic Center (brown dwarfs EMRIs -cf Freitag)
Galactic sources that are not binaries
1. Strongly magnetised rapidly spinning WDs
Galactic structure
1. Components: discs(s), spiral arms, bulge, Halo, Galactic center(?)
2. LISA science: tracing mass distribution, (Halo) binary fraction, IMF and star formation history , globular clusters, open clusters(?)
Extra-galactic sources
1. Discrete sources (LMC, SMC, M31, M87…)
2. Cosmological background
3. LISA science…
4. Connections to BBO/Decigo rates
Connecting LISA and LIGO/VIRGO
1. Possibilities, sources
2. Combined science
Summary for each source category, of
1. unique LISA science (cf 5)
2. convolved LISA science (e.g. populations+synthesis trace bulge/disk, binary fractions, IMF, star formation history)
3. Joint EM-GW science (e.g. inclinations, tidal heating)
Conclusions and outlook