Chris M. Chambers

Radiative falloff in Schwarzschild-de Sitter space-time

We consider the time evolution of a scalar field propagating in Schwarzschild-de Sitter spacetime. At early times, the field behaves as if it were in pure Schwarzschild spacetime; the structure of spacetime far from the black hole has no influence on the evolution. In this early epoch, the fields initial outburst is followed by quasi-normal oscillations, and then by an inverse power-law decay. At intermediate times, the power-law behavior gives way to a faster, exponential decay. At late times, the field behaves as if it were in pure de Sitter spacetime; the structure of spacetime near the black hole no longer influences the evolution in a significant way. In this late epoch, the fields behavior depends on the value of the curvature-coupling constant xi. If xi is less than a critical value 3/16, the field decays exponentially, with a decay constant that increases with increasing xi. If xi > 3/16, the field oscillates with a frequency that increases with increasing xi; the amplitude of the field still decays exponentially, but the decay constant is independent of xi.

Phases of massive scalar field collapse

We study critical behavior in the collapse of massive spherically symmetric scalar fields. We observe two distinct types of phase transition at the threshold of black hole formation. Type II phase transitions occur when the radial extent

Nonlinear instability of Kerr-type Cauchy horizons.

(\ensuremath{\lambda})

Spinning Down a Black Hole with Scalar Fields

of the initial pulse is less than the Compton wavelength

Evaporation of a Kerr black hole by emission of scalar and higher spin particles

({\ensuremath{\mu}}^{\ensuremath{-}1})

Telling tails in the presence of a cosmological constant

of the scalar field. The critical solution is that found by Choptuik in the collapse of massless scalar fields. Type I phase transitions, where the black hole formation turns on at finite mass, occur when

The Cauchy Horizon In Black Hole-de Sitter Spacetimes

\ensuremath{\lambda}\ensuremath{\mu}\ensuremath{\gg}1

The `Ups' and `Downs' of a Spinning Black Hole

. The critical solutions are unstable soliton stars with masses

Some Cosmological Tails of Collapse

\ensuremath{\lesssim}0.6{\ensuremath{\mu}}^{\ensuremath{-}1}

A Critical Look At Massive Scalar Field Collapse

. Our results in combination with those obtained for the collapse of a Yang-Mills field [M. W. Choptuik, T. Chmaj, and P. Bizon, Phys. Rev. Lett. 77, 424 (1996)] suggest that unstable, confined solutions to the Einstein-matter equations may be relevant to the critical point of other matter models.