By Rev. T.W.; Edited and Revised By Margaret W. Mayall Webb
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Additional info for Celestial Objects for Common Telescopes. Edited and Rev. By Margaret W. Mayall
We thank Robert Bingham, Gert Brodin, Arshad Mirza, and Oleg Pokhotelov for their valuable collaboration on diﬀerent parts presented in this paper. This research was partially supported by the Deutsche Forschungsgemeinschaft through the Sonderforschungsbereich 191 and the European Union (Brussels) through the INTAS grant (INTAS-GEORG-52-98), as well as by the Swedish Natural Science Research Council and the International Space Science Institute (ISSI) at Bern (Switzerland). The authors gratefully acknowledge the warm hospitality of Prof.
2) to ∂2F ∂ ∂2F (∇ · E) + + − 2 2 ∂z ∂x ∂x ∂2G ∂2G ∂ (∇ · E) + + − ∂z 2 ∂x2 ∂x ω2 ( + g)F = 0, c2 ω2 ( − g)G = 0. c2 (11a) (11b) Instead of the z-projection of Eq. (2), we use Eq. (3) that can be written as ∂ 1 ∂ (ηEz ) + [( + g)F + ( − g)G] = 0. ∂z 2 ∂x (12) This is the third equation,containing Ez that appears in ∇·E≡ ∂Ez 1 ∂ . I. Karpman Equations (11) and (12), together with the given function N = N (x), constitute a complete system. At N (x) = const, the simplest solution to this system, describes a whistler wave, propagating parallel to the ambient magnetic ﬁeld (z-axis) .
Speciﬁcally, in a cold (Tj → 0) dusty plasma 2 = 0. The latter shows that coupling we have from (79) ω 2 − ωωsv − ωIA between the Shukla-Varma mode and the inertial Alfv´en wave arises due to the consideration of the parallel electron dynamics in the electromagnetic ﬁelds. Third, when the perpendicular wavelength is much larger than λe , we obtain from (79) for ω ωi∗ 2 2 2 2 ω 2 − ωωsv − kz2 vA (ω − ωe∗ ) = kz2 vA ky ρss (ω − ωsv ) , (80) which exhibits the coupling between the drift-Alfv´en waves and the ShuklaVarma mode due to ﬁnite Larmor radius correction of the ions at the electron temperature.
Celestial Objects for Common Telescopes. Edited and Rev. By Margaret W. Mayall by Rev. T.W.; Edited and Revised By Margaret W. Mayall Webb