Inflation in an accreting, rotating black hole is followed by BKL oscillatory collapse
(Hamilton 2017)
Belinski, Khalatnikov & Lifshitz (1972)
argued that collapse to a spacelike singularity would generically
be chaotic and oscillatory.
The spatial metric can be thought of as ellipsoid with 3 axes \(a_i\).
In BKL collapse, power-law “Kasner” epochs
are punctuated by bounces.
During a Kasner epoch, the scale factors \(a_i\) evolve as
\[
a_i \propto ( a_1 a_2 a_3 )^{q_i}
\ , \quad
\sum_i q_i = 1
\ , \quad
\sum_i q_i^2 = 1
\ .
\]
Inflation and conformally separable collapse
(Hamilton & Polhemus 2011)
are just the first two Kasner epochs of BKL collapse.
The Kasner exponents of the second epoch are those of Schwarzschild.
Conclusion
