A New Solution to the Plasma Starved Event Horizon Magnetosphere:
  Application to the Forked Jet in M87
  Very Long Baseline Interferometry observations at 86 GHz reveal an almost
hollow jet in M87 with a forked morphology. The detailed analysis presented
here indicates that the spectral luminosity of the central spine of the jet in
M87 is a few percent of that of the surrounding hollow jet $200 -400
\mu\rm{as}$ from the central black hole. Furthermore, recent jet models in
indicate that a hollow "tubular" jet can explain a wide range of plausible
broadband spectra originating from jetted plasma located within $\sim
30\mu\rm{as}$ of the central black hole, including the 230 GHz correlated flux
detected by the Event Horizon Telescope. Most importantly, these hollow jets
from the inner accretion flow have an intrinsic power capable of energizing the
global jet out to kiloparsec scales. Thus motivated, this paper considers new
models of the event horizon magnetosphere (EHM) in low luminosity accretion
systems. Contrary to some models, the spine is not an invisible powerful jet.
It is an intrinsically weak jet. In the new EHM solution, the accreted poloidal
magnetic flux is weak and the background photon field is weak. It is shown how
this accretion scenario naturally results in the dissipation of the accreted
poloidal magnetic flux in the EHM not the accumulation of poloidal flux
required for a powerful jet. The new solution indicates less large scale
poloidal magnetic flux (and jet power) in the EHM than in the surrounding
accretion flow and cannot support significant EHM driven jets.
