We study the expected spin misalignments of merging binary black holes formed in isolation by combining state-of-the-art population-synthesis models with efficient post-Newtonian evolutions, thus tracking sources from stellar formation to gravitational-wave detection. present extensive predictions properties detectable both current and future interferometers. account for fact that detectors are more sensitive spinning black-hole binaries suitable orientations find this significantly impacts...

Inflationary gravitational waves (GW) contribute to the curl component in polarization of cosmic microwave background (CMB). Cosmic shear--gravitational lensing CMB--converts a fraction dominant gradient component. Higher-order correlations can be used map shear and subtract this contribution curl. Arcminute resolution will required pursue GW amplitudes smaller than those accessible by Planck surveyor mission. The blurring small-scale CMB power leads with reconstruction technique minimum...

A supermassive black hole can disrupt a star when its tidal field exceeds the star's self-gravity, and directly capture stars that cross event horizon. For holes with mass $M\ensuremath{\gtrsim}{10}^{7}{M}_{\ensuremath{\bigodot}}$, disruption of main-sequence occurs close enough to horizon Newtonian treatment is no longer valid. The fraction are captured also negligible. We calculate generically oriented stellar orbits in Kerr metric, evaluate relativistic tensor at pericenter for those not...

We study the influence of astrophysical formation scenarios on precessional dynamics spinning black-hole binaries by time they enter observational window second- and third-generation gravitational-wave detectors, such as Advanced LIGO/Virgo, LIGO-India, KAGRA, Einstein Telescope. Under plausible assumption that tidal interactions are efficient at aligning spins few-solar mass progenitors with orbital angular momentum, we find should be expected to preferentially lie in a plane when become...

The dynamics of precessing binary black holes (BBHs) in the post-Newtonian regime has a strong timescale hierarchy: orbital is very short compared to spin-precession which, turn, much shorter than radiation-reaction on which orbit shrinking due gravitational-wave emission. We exploit this hierarchy develop multiscale analysis BBH elaborating Kesden et al. [Phys. Rev. Lett. 114, 081103 (2015)]. solve equations analytically precession time and then implement quasiadiabatic approach evolve...

We derive an effective potential for binary black hole (BBH) spin precession at second post-Newtonian order. This allows us to solve the orbit-averaged spin-precession equations analytically arbitrary mass ratios and spins. These solutions are quasiperiodic functions of time: after a fixed period, BBH spins return their initial relative orientations jointly precess about total angular momentum by angle. Using these solutions, we classify into three distinct morphologies between which BBHs...

Weak gravitational lensing by an intervening large-scale structure induces a distinct signature in the cosmic microwave background (CMB) that can be used to reconstruct weak-lensing displacement map. Estimators for individual Fourier modes of this map combined produce estimator lensing-potential power spectrum. The naive quantity will biased upwards uncertainty associated with reconstructing modes; we present iterative scheme removing bias. variance and covariance spectrum are calculated...

Satellite galaxies currently undergoing tidal disruption offer a unique opportunity to constrain an effective violation of the equivalence principle in dark sector. While matter standard scenario interacts solely through gravity on large scales, new long-range force between dark-matter particles may naturally arise theories which couples light scalar field. An inverse-square-law this kind would manifest itself as dynamics compared baryons form gas or stars. In previous paper, we showed that...

We present the numerical code precession, a new open-source python module to study dynamics of precessing black-hole binaries in post-Newtonian regime. The provides comprehensive toolbox (i) evolution spins along their precession cycles, (ii) perform gravitational-wave-driven binary inspirals using both orbit-averaged and precession-averaged integrations, (iii) predict properties merger remnant through fitting formulas obtained from numerical-relativity simulations. is ready-to-use tool add...

We compare binary evolution models with different assumptions about black-hole natal kicks to the first gravitational-wave observations performed by LIGO detectors. Our comparisons attempt reconcile merger rate, masses, spins, and spin-orbit misalignments of all current state-of-the-art formation scenarios black holes formed in isolation. estimate that (BHs) should receive at birth order $\sigma\simeq 200$ (50) km/s if tidal processes do (not) realign stellar spins. is driven two simple...

Event horizons are among the most intriguing of general relativity's predictions. Although on firm theoretical footing, direct indications their existence have yet to be observed. With this motivation in mind, we explore here possibility finding a signature for event gravitational waves (GWs) produced during inspiral stellar-mass compact objects (COs) into supermassive ($\ensuremath{\sim}{10}^{6}{M}_{\ensuremath{\bigodot}}$) that lie at center galaxies. Such inspirals will major source LISA,...

Satellite galaxies are tidally disrupted as they orbit the Milky Way. If dark matter (DM) experiences a stronger self-attraction than baryons, stars will preferentially gain rather lose energy during tidal disruption, leading to an enhancement in trailing compared stream. The Sgr dwarf galaxy is seen have roughly equal streams, challenging models which DM and baryons accelerate differently by more 10%. Future observations better understanding of distribution should allow detection...

We regard binary-black-hole (BBH) merger as a map from simple initial state (two Kerr black holes, with dimensionless spins and b) to final (a hole mass m, spin s, kick velocity k). By expanding this around a=b=0 applying symmetry constraints, we obtain formalism that is remarkably successful at explaining existing BBH simulations. It also makes detailed predictions suggests more efficient way of mapping the parameter space binary black-hole merger. Since rely on rather than dynamics, our...

Numerical-relativity simulations indicate that the black hole produced in a binary merger can recoil with velocity up to vmax ≃ 4000 km s−1 respect center of mass initial binary. This challenges paradigm most galaxies form through hierarchical mergers, yet retain supermassive holes (SBHs) at their centers despite having escape velocities much less than vmax. Interaction circumbinary disk align spins orbital angular momentum, reducing final subsequent merger. However, effectiveness this...

The inspiral of binary black holes is governed by gravitational radiation reaction at separations $r\ensuremath{\lesssim}1000M$, yet it too computationally expensive to begin numerical-relativity simulations with initial $r\ensuremath{\gtrsim}10M$. Fortunately, evolution between these well described post-Newtonian equations motion. We examine how this affects the distribution spin orientations $r\ensuremath{\simeq}10M$ where typically begin. Although isotropic distributions...

A star orbiting a supermassive black hole can be tidally disrupted if the hole's gravitational tidal field exceeds star's self gravity at pericenter. Some of this stellar debris become gravitationally bound to hole, leading bright electromagnetic flare with bolometric luminosity proportional rate which material falls back In Newtonian limit, will have light curve that scales as t^-5/3 has flat distribution in binding energy. We investigate time dependence black-hole mass accretion when...

Binary black holes (BBHs) can form from the collapsed cores of isolated high-mass binary stars. The masses and spins these BBHs are determined by complicated interplay phenomena such as tides, winds, accretion, common-envelope evolution (CEE), supernova natal kicks, stellar core-envelope coupling. gravitational waves emitted during mergers depend on their thus constrain phenomena. We present a simplified model identify regions parameter space that produce with large misaligned orbital...

In a recent paper [L. Boyle, M. Kesden, and S. Nissanke, Phys. Rev. Lett. 100, 151101 (2008)], we introduced spin expansion that provides simple yet powerful way to understand aspects of binary black hole merger. This approach relies on the symmetry properties initial final quantities like mass $m$, kick velocity $\mathbf{k}$, vector $\mathbf{s}$, rather than detailed understanding merger dynamics. this paper, expand proposal, examine how well its predictions agree with current simulations,...

Binary black holes on quasicircular orbits with spins aligned their orbital angular momentum have been testbeds for analytic and numerical relativity decades, not least because symmetry ensures that such configurations are equilibrium solutions to the spin-precession equations. In this work, we show these can be unstable when spin of higher-mass hole is lower-mass anti-aligned. Spins in precession large misalignment binary separation $r$ between values $r_{\rm ud\pm}= (\sqrt{\chi_1} \pm...

If binary black holes form following the successive core collapses of sufficiently massive stars, precessional dynamics may align their spins $\mathbf S_1$ and S_2$ orbital angular momentum L$ into a plane in which they jointly precess about total J$. These spin orientations are known as spin-orbit resonances since S_1$, S_2$, all at same frequency to maintain planar configuration. Two families such exist, alike dignity but differentiated by whether components two either aligned or...

Gravitational waves carry away both energy and angular momentum as binary black holes inspiral merge. The relative efficiency with which they are radiated determines whether the final hole of mass ${M}_{f}$ spin ${S}_{f}$ saturates Kerr limit (${\ensuremath{\chi}}_{f}\ensuremath{\equiv}{S}_{f}/{M}_{f}^{2}\ensuremath{\le}1$). Extrapolating from test-particle limit, we propose expressions for mergers initial spins aligned or anti-aligned orbital momentum. We predict at plunge equal-mass...

Recent numerical relativity simulations have shown that the final black hole produced in a binary merger can recoil with velocity as large 5,000 km/s. Because of enhanced gravitational-wave emission so-called "hang-up" configurations, this maximum occurs when black-hole spins are partially aligned orbital angular momentum. We revisit our previous statistical analysis post-Newtonian evolutions binaries light these new findings. demonstrate despite configurations velocities, spin alignment...

Gravitational waves from coalescing binary black holes encode the evolution of their spins prior to merger. In post-Newtonian regime and on precession timescale, this has one three morphologies, with either librating around two fixed points ("resonances") or circulating freely. work we perform full parameter estimation resonant binaries masses spin magnitudes, changing parameters: a conserved "projected effective spin" $\xi$ family $\Delta\Phi=0,\pi$ (which uniquely label source),...