Postdoctoral Researcher

Ph.D:

Physics, The Pennsylvania State University

Research:

Numerical Relativity

Publications:

Select Publications:

- Unstable flip-flopping spinning binary black holes Arxiv:1601.05086, 2016.
- Spin flips in generic black hole binaries Phys. Rev. D 93, 044031, 2016.
- Perturbative extraction of gravitational waveforms generated with numerical relativity Phys. Rev. D 91, 104022, 2015.
- High Energy Collisions of Black Holes Numerically Revisited Arxiv:1506.06153, 2015.
- New Puncture Initial Data for Black-Hole Binaries: High Spins and High Boosts Arxiv:1410.8607, 2014.
- Flip-flopping binary black holes Physical Review Letters, 114:141101, 2015.
- Remnant mass, spin, and recoil from spin-aligned black-hole binaries Phys. Rev. D 90, 104004, 2014.
- Modelling Ringdown: Beyond the Fundamental Quasi-normal Modes Phys. Rev. D 90, 124032, 2014.
- Critical Collapse of Scalar Fields Beyond Axisymmetry Gen. Rel. Grav. 46 1722, 2014.
- Impact of Higher-order Modes on the Detection of Binary Black Hole Coalescence Phys. Rev. D 87, 084008, 2013.
- Late Inspiral and Merger of Binary Black Holes in Scalar-Tensor Theories of Gravity Class.Quant.Grav. 29 232002, 2012.
- Final Mass and Spin of Merged Black Holes and the Golden Black Hole Phys. Rev. D 81, 081501, 2010.
- Zoom-Whirl Orbits in Black Hole Binaries Phys. Rev. Lett. 103:131101, 2009.
- Superkicks in Hyperbolic Encounters of Binary Black Holes Phys. Rev. Lett. 102:041101, 2009.
- Binary Black Hole Encounters, Gravitational Burst and Maximum Final Spin Phys. Rev. Lett. 101:061102, 2008.

Background:

Through numerical relativity, or the solving of Einstein's equations of gravity using numerical techniques, we are able to evolve a binary black hole (BBH) system from initially two separate black holes slowly inspirally, until they eventually coalesce and settle down into a single Kerr black hole. Numerical relativity gives us the opportunity to pose the following question: given two initial black holes with some mass, spin, and momentum, what is the final mass, spin, and momentum of the merged remnant black hole, and what gravitational radiation is generated from this process?

With this question in mind, I've studied a large collection of initial BBH configurations using numerical relativity ranging from quasicircular orbits to highly eccentric orbits to direct plunges. By exploring this wide range of BBH parameter space, my collaborators and I have found some interesting and exciting results, including kick velocities as high as 12,000 km/s and final spins close to maximal from direct plunges. We have also found highly accurate analytic models to determine the final mass and spin from the initial configuration of aligned-spin BBH systems in quasicircular orbits.

- 2013 - Present Postdoc, Center For Computational Relativity and Gravitation, RIT
- 2010 - 2013 Postdoc, Center for Relativistic Astrophysics, Georgia Tech
- 2006 - 2009 Ph.D., Physics, The Pennsylvania State University
- 2002 - 2006 B.S., Physics, University of Delaware

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