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Radiating scalar fields,aOnaaCaaaleqabaGaeqiVd0Ma% eqyVd4gaaOGaeyOaIy7aaSbaaSqaaiabe27aUbqabaGccqWGMbGzcq% GGUaGlaaa!5E49![p^mu = frac{{partial L}}{{partial f_{,mu } }} =- sqrt { - det eta _{alpha eta } } eta ^{mu
u } partial _
uf.] The canonical momentum . is defined as in equation (3.18): . Let ℊ be any piecewise smoot
0940-7677the case of Einstein gravity. The Hamiltonian role of the Trautman--Bondi mass is exhibited. A Hamiltonian definition of angular momentum at null infinity is derived and analysed.978-3-642-07681-7978-3-540-45604-9Series ISSN 0940-7677
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https://doi.org/10.1007/978-3-319-63847-8 to consider motions of hypersurfaces which do not arise from the flow of a vector field; we shall indeed encounter such motions in Sect. 4.5 below. The purpose of this chapter is to generalize the framework of Kijowski and Tulczyjew to allow for such situations.
Preliminaries,e following chapters that the dynamics of the massless scalar field in the radiation regime, as well as that of the gravitational field in the radiation regime, satisfies the requirements of the definitions given in this chapter.
Hamiltonian flows for geometric field theories, to consider motions of hypersurfaces which do not arise from the flow of a vector field; we shall indeed encounter such motions in Sect. 4.5 below. The purpose of this chapter is to generalize the framework of Kijowski and Tulczyjew to allow for such situations.