Research
1. Gravitational self-force in the time domain
i. What is gravitational self-force(GSF)?
Gravitational self-force is an approach to the two-body problem in GR in which the smaller object’s equation of motion is written perturbatively to model its non-geodesic motion in the spacetime produced by a much larger object.
\[\begin{align} \frac{dp^{\alpha}}{d\tau} = \epsilon F_{1}^{\alpha} + \epsilon^2 F_{2}^{\alpha} + \mathcal{O}(\epsilon^3) \end{align}\]2. Boundary conditions for wave-like equations in black hole perturbation theory(BHPT)
i. What are the wave-like equations in the context of BHPT
There are 3 wave-like equations in Black Hole perturbation theory. They are the Regge-Wheeler equation, the Zerilli equation and the Teukolsky equation. The first two describe perturbations in the spacetime of Schwarzschild black holes, while the third describes perturbations of Kerr black holes.
3. Observational implications for Gravitational hair from extremal Kerr black holes
i. What is hair in the context of black holes?
Rather than directly answering the question, it is easier to understand the no-hair theorem in general relativity. It states that a black hole is fully characterized by three parameters namely the mass, spin and charge. In that sense there are no other(independent) quantities that can distinguish between two black holes.
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