Balázs Mikóczi

Self-interaction spin effects in inspiralling compact binaries

Gravitational radiation drives compact binaries through an inspiral phase towards a final coalescence. For binaries with spin, mass quadrupole, and magnetic dipole moments, various contributions add to this process, which is characterized by the rate of increase

Kepler equation for inspiralling compact binaries

df/dt

Renormalized 2PN spin contributions to the accumulated orbital phase for LISA sources

of the gravitational wave frequency and the accumulated number

Spin supplementary conditions for spinning compact binaries

\mathcal{N}

Secular momentum transport by gravitational waves from spinning compact binaries

of gravitational wave cycles. We present here all contributions to

ORBITAL PHASE IN INSPIRALLING COMPACT BINARIES

df/dt

The second post-newtonian order generalized kepler equation

and

Renormalized spin coefficients in the accumulated orbital phase for unequal mass black hole binaries

\mathcal{N}

Self interaction of spins in binary systems

up to the second post-Newtonian order. Among them we give for the first time the contributions due to the self-interaction of individual spins. These are shown to be commensurable with the proper spin-spin contributions for the recently discovered J0737-3039 double pulsar and argued to represent the first corrections to the radiation reaction in the Lense-Thirring approach.

Second order spin effects in the spin precession of compact binaries

Compact binaries consisting of neutron stars/black holes on eccentric orbit undergo a perturbed Keplerian motion. The perturbations are either of relativistic origin or are related to the spin, mass quadrupole, and magnetic dipole moments of the binary components. The post-Newtonian motion of such systems decouples into radial and angular parts. We present here for the first time the radial motion of such a binary encoded in a generalized Kepler equation, with the inclusion of all above-mentioned contributions, up to linear order in the perturbations. Together with suitably introduced parametrizations, the radial motion is solved completely.