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Quasilocal formulations of black hole are of immense importance since theyreveal the essential and minimal assumptions required for a consistentdescription of black hole horizon, without relying on the asymptotic boundaryconditions on fields. Using the quasilocal formulation of Isolated Horizons, weconstruct the Hamiltonian charges corresponding to local Lorentztransformations on a spacetime admitting isolated horizon as an internalboundary. From this construction, it arises quite generally that the\emph{area} of the horizon of an isolated black hole is the Hamiltonian chargefor local Lorentz boost on the horizon. Using this argument further, it isshown that, observers at a fixed proper distance $l_{0}$, very close to thehorizon, may define a notion of horizon energy given by $E=A/8\pi G l_{0}$, thesurface gravity is given by $\kappa=1/l_{0}$, and consequently, the first lawcan be written in the quasilocal setting as $\delta E=(\kappa/8\pi G)\deltaA$..

Quasilocal first law of black hole dynamics from local Lorentz transformations