The charged spacetime Penrose inequality in upper-area form for Einstein-Maxwell initial data

Principal (Theorem 2.3): for one-ended three-dimensional data with arbitrary $K$, nonzero ADM momentum, disconnected weakly future trapped boundary and the stated decay, $m\ge|Q|$ and $r_A\le m+\sqrt{m^2-Q^2}$ with $A$ the minimal enclosing area; positive area and timelike ADM vector are conclusions. Equality (for $m>|Q|$, connected outermost horizon) identifies the data as a slice of dyonic Reissner-Nordstrom. Companions: the purely electric case in every dimension $n\ge4$; a Kerr-Newman Penrose inequality for axisymmetric electrovacuum exteriors with zero ADM momentum that assumes the area condition $A\ge4\pi\sqrt{Q^4+4J^2}$; and counterexamples to the Kerr-Newman bound when $J$ is the bare gravitational angular momentum and fields decay only like $r^{-2}$. Not shown: magnetic charge in dimensions four and up, or a general rotating inequality.

Principal (Theorem 2.3): for one-ended three-dimensional data with arbitrary $K$, nonzero ADM momentum, disconnected weakly future trapped boundary and the stated decay, $m\ge|Q|$ and $r_A\le m+\sqrt{m^2-Q^2}$ with $A$ the minimal enclosing area; positive area and timelike ADM vector are conclusions. Equality (for $m>|Q|$, connected outermost horizon) identifies the data as a slice of dyonic Reissner-Nordstrom. Companions: the purely electric case in every dimension $n\ge4$; a Kerr-Newman Penrose inequality for axisymmetric electrovacuum exteriors with zero ADM momentum that assumes the area condition $A\ge4\pi\sqrt{Q^4+4J^2}$; and counterexamples to the Kerr-Newman bound when $J$ is the bare gravitational angular momentum and fields decay only like $r^{-2}$. Not shown: magnetic charge in dimensions four and up, or a general rotating inequality.