The detection of gravitational waves emitted by binary black holes raises a question of the binaries’ origin. There are several models present in the literature involving binary evolution in both field and clusters. Here I aim to compare predictions of these models with the observations.
Using the Bayesian inference I compare the models with the up-to-date detections using the distributions of...
The angles between the spins of binary black holes and the binary's orbital angular momentum (often known as tilt angles) give important information about the evolution of the binary. For instance, for the isolated binary formation channel, the tilt angles when the binary is formed give information about supernova kicks. One can obtain the tilt angles at the binary's formation computationally...
Just like visible light, gravitational waves can be lensed by heavy masses between source and observer. Hence, a fraction of the observed distant binary black hole mergers could be magnified by lensing, some sources may have produced multiple observable images, and individual waveforms may be affected by wave optics and microlensing effects.
The predicted rate of such lensing is small for the...
We investigate the visibility of single Galactic pulsars in the gravitational waves. We integrate the signal for a period of one year, a comparable length to the current O3 LIGO/Virgo observing run, by computing the interferometr response and compering it to the design sensitives of LIGO and Virgo detectors. With an assumption of single radio pulsar population model, classical rotating...
The evolution of massive stars remains highly uncertain due to a number of poorly constrained factors such as internal mixing, angular momentum transport, mass loss rates, or effects of binarity. Detections of gravitational waves from BH binary mergers offer a unique opportunity to probe the evolution of a particular subset of massive stars: those that have (most likely) initiated and survived...
We explore the different formation channels of merging double compact objects (DCOs: BH-BH/BH-NS/NS-NS) that went through an ULX phase (X-ray sources with luminosity exceeding the Eddington luminosity of a 10 $M_{\odot}$ black hole). There are two major formation channels which can naturally explain the formation of DCO systems: isolated binary evolution and dynamical evolution inside dense...
In the new era of gravitational-wave astronomy, understanding the properties of the host galaxies of merging compact objects is crucial.
I will present a method to explore the galaxies where merging compact objects form and merge, by combining galaxy catalogs from cosmological simulations together with state of the art population synthesis models.
I will show that the merger rate per galaxy...
All of the ten LIGO/Virgo BH-BH merger O1/O2 detections have near zero effective spins. One explanation makes BH spin magnitudes small.
We test this hypothesis with the classical isolated binary evolution scenario. We test three models of angular momentum transport in massive stars: mildly efficient transport by meridional currents (as employed in the Geneva code), efficient transport by...
