Abstract
Relativistic jets can be modeled as magnetohydrodynamic flows. We analyze the related equations and discuss the involved acceleration mechanisms, their relation to the collimation, to the jet confinement by its environment, and to possible rarefaction waves triggered by pressure imbalances.
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- 1.
If Ω is the same in all streamlines as is often the case in pulsar winds, this surface is a cylinder, called light cylinder.
- 2.
Note that B ϕ < 0 so that both parts of the angular momentum are positive.
- 3.
As in the case of the angular momentum, both parts are positive since B ϕ < 0.
- 4.
The function M f shows where the fast-magnetosonic surface is located. Besides that, M f is related to the Mach-cone of the propagation of fast magnetosonic waves in the super-fast regime. This cone has half opening angle \(\arctan (M_{f}^{2} - 1)^{-1/2}\) (the cone’s symmetry axis coincides with the poloidal field line).
- 5.
Actually the equations describing the effect in planar geometry can be found from the corresponding ones in cylindrical geometry by replacing \(\varpi \rightarrow \varpi _{0} + x\), \(z \rightarrow z_{0} + z\), \(A/\varpi _{0} \rightarrow A\), \(\varpi _{0}\varOmega /c \rightarrow \chi\), \(x_{\mathrm{A}} \rightarrow \chi _{\mathrm{A}}\), \(L/\varpi _{0} \rightarrow P =\mu c\chi _{\mathrm{A}}^{2}/\chi\), \(\varpi _{\mathrm{A}}/\varpi _{0} \rightarrow \chi _{\mathrm{A}}/\chi\), and then taking the limit \(\varpi _{0} \rightarrow \infty \).
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Vlahakis, N. (2015). Theory of Relativistic Jets. In: Contopoulos, I., Gabuzda, D., Kylafis, N. (eds) The Formation and Disruption of Black Hole Jets. Astrophysics and Space Science Library, vol 414. Springer, Cham. https://doi.org/10.1007/978-3-319-10356-3_7
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