= Collapse vacuum for Hawking radiation
In a collapse spacetime, choose the quantum field's incoming state to have no incoming particles at <past null infinity> and to be regular in freely falling coordinates near the forming <event horizon>. The late outgoing modes then have the <Hawking temperature>, while there is no incoming thermal bath. This collapse-state boundary condition differs from an equilibrium state on an eternal <black hole>. The <Hawking exponential ray map> and the <thermal ratio of Hawking Bogoliubov coefficients> determine the leading late-time particle spectrum; <greybody factors> describe scattering outside the <event horizon>.
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