Force-Free Black Hole Magnetospheres

Details Force-Free Black Hole Magnetospheres Force-Free Black Hole Magnetospheres

Oct 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009pasj...61..971o&link_type=abstract

Publications of the Astronomical Society of Japan, Vol.61, No.5, pp.971--990

Astronomy and Astrophysics

Astronomy

Black Holes, Mhd, Ism: Magnetic Fields, Stars: Winds And Outflows

Scientific paper

It is argued that a force-free degenerate electrodynamic (FFDE) magnetosphere of a Kerr black hole with 0 < ΩF < ΩH consists of the outer classical and inner general-relativistic domains. This is described by a simple DC dual-circuit model, with dissipative membranes as two loads at a ``force-free infinity surface'' (Sff∞) with ω = 0 and at a ``force-free horizon surface'' (SffH) with ω = ΩH, where ω, ΩH, and ΩF, are the frame-dragging, the horizon and the field line angular frequencies. It is beneath upper null surface, SN, at ω = ΩF between the two domains that dual unipolar batteries (double EMF's) exist back-to-back, oppositely directed, with a pair-creation gap between. The total energy flux boldsymbol{S}E is a linear sum of the two fluxes: the hole's outward spin-down energy flux boldsymbol{S}SD originating at SffH and the Poynting flux boldsymbol{S}EM emitted at SN in both the outward and inward directions, with boldsymbol{S}E being proportional to ΩF, boldsymbol{S}SD to ω and boldsymbol{S}EM to (ΩF - ω) along each field line. Applying a perturbation method for a split-monopolar field with a spin-parameter h ≪ 1, the analytic solution of the stream equation is given, and the double eigenvalue problem due to the `criticality condition' at the outer/inner fast surfaces SoF/SiF and the `boundary condition' at SN is solved to yield the final eigenvalue ΩF, in terms of ΩH and ≥H = 0.5676. The ratio of the output power reaching Sff∞ to to the dissipation on SffH is ɛ = 1 + (4/5) (1-≥H)h².

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