Abstract
In the 1990s Christodoulou introduced an idealized fluid model intended to capture some of the features of the gravitational collapse of a massive star to form a neutron star or a black hole. This was the two-phase model introduced in ‘Self-gravitating relativistic fluids: a two phase model’ (Demeterios, Arch Ration Mech Anal 130:343–400, 1995). The present work deals with the formation of a free phase boundary in the phase transition from hard to soft in this model. In this case the phase boundary has corners at the null points; the points which separate the timelike and spacelike components of the interface between the two phases. We prove the existence and uniqueness of a free phase boundary. Also the local form of the shock near the null point is established.
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Demeterios C.: Self-gravitating relativistic fluids: a two-phase model. Arch. Ration. Mech. Anal. 130, 343–400 (1995)
Demeterios C.: Self-gravitating relativistic fluids: the continuation and termination of a free phase boundary. Arch. Ration. Mech. Anal. 133, 333–398 (1996)
Demeterios C.: Self-gravitating relativistic fluids: the formation of a free phase boundary in the phase transition from soft to hard. Arch. Ration. Mech. Anal. 134, 97–154 (1996)
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Communicated by F. Lin
Work supported by ERC Advanced Grant 246574 Partial Differential Equations of Classical Physics.
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Christodoulou, D., Lisibach, A. Self-Gravitating Relativistic Fluids: The Formation of a Free Phase Boundary in the Phase Transition from Hard to Soft. Arch Rational Mech Anal 222, 927–1010 (2016). https://doi.org/10.1007/s00205-016-1015-x
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DOI: https://doi.org/10.1007/s00205-016-1015-x