= Solution
An isolated collapse emits transient matter and <gravitational waves>. The exterior is expected to settle to an asymptotically flat <stationary spacetime>. Because the star is uncharged, the <black-hole uniqueness theorem> identifies the regular final state with a <Kerr black hole>. Its higher <multipole moments> are fixed by its conserved charges: the <black-hole no-hair theorem> leaves only the total <mass> $M$ and <angular momentum> $J$. Thus \b[the late-time spacetime is characterized by $M$ and $J$].
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