[en] If the magnetic field in a type-I comet tail were of internal origin, it would decrease with distance along the tail axis, and the comet tail would increase in cross-section. The tail of Comet Arend-Roland (1957 III) was shown not to expand with distance from the nucleus, whence it is concluded that the magnetic field in the tail is of external origin. The magnetic field in type-I comet tails estimated from different considerations turns out to be of the order of the interplanetary field, so that one may suppose that it results from the captured solar wind magnetic field. (author)

[en] The return-flux sunspot model is generalized by including azimuthal magnetic field Bsub(PHI). The basic equation is obtained and numerical solutions are compared with the analogous solutions for the Schlueter-Temesvary sunspot theory for two cases: Bsub(PHI)proportionalBsub(r) and Bsub(PHI)proportionalrBsub(r). The solutions demonstrate that the twisting of the sunspot magnetic field decreases with height. Our models confirm Yun's early statement: the azimuthal field only slightly influences sunspot structure. (orig.)

[en] Magnetic field generation and evolution in celestial bodies—the subject matter of the theory of the dynamo—held Ya B Zeldovich's interest for years. Over the time since then, the study of the dynamo process has developed from a part of astrophysics and geophysics to a self-contained domain of physics, with the possibility of laboratory dynamo physics experiments. We give some theoretical background and discuss laboratory dynamo experiments (including those conducted in Russia), as well as their impact on dynamo theory and its astrophysical applications. (100th anniversary of the birth of ya b zeldovich)

[en] All of the new quadrupoles for the Fermilab Main Injector ring have been built and measured. The magnets are 2.95 m and 2.54 m in length with a 41.7 mm bore. In operation, the magnets run from 1.61 T/m at 8. 9 GeV/c to 15.7 T/m at 120 GeV/c and 19.6 T/m at 150 GeV/c. These points correspond to injection, Main Injector fixed target physics and antiproton production, and extraction for transfer to the Tevatron. Good field uniformity is required to ensure a stable beam over the whole acceleration cycle. A significant octupole is included to assist in resonant extraction. The performance of these quadrupoles, in both integrated strength and field uniformity, is presented. All magnets produced meet the accelerator requirements

No abstract available

[en] The effective ripple is analysed for the final version of the quasi-axisymmetric stellarator configuration with a low aspect ratio, CHS-qa. For the computation, a method is used that is based on the integration along magnetic field lines in a given magnetic field. Computations are done for magnetic fields presented in Boozer magnetic coordinates as well as for magnetic fields produced directly by currents in the modular coils of the device. The computations show the significant advantage of CHS-qa over a conventional stellarator resulting from the reduced effective ripple

[en] Some experimental observations of rotamak equilibria made in a high-power, short-duration (approx.80-μs) experiment and a complementary low-power, long-duration experiment are summarized. In the high-power experiment two possible equilibrium phases have been identified: an oblate, compact torus configuration and a β = 1, mirrorlike configuration. In the low-power experiment toroidal plasma current has been driven, and a compact torus configuration has been maintained, for several milliseconds

[en] We present the optical observations of the July 26--27, 1982 flares in Hale region 17760. Study of data in Hα, Hα-0.5 A, He ID₃, and videomagnetograms leads to the following conclusions:

[en] A model for solar quiescent prominensces nested in a ''Figure 8'' magnetic field topology is developed. This topology is argued to be the natural consequence of the distention of bipolar regions upward into the corona. If this distention is slow enough so that hydrostatic equilibrium holds approximately along the field lines, the transverse gas pressure forces fall exponentially with height whereas the inward Lorentz forces fall as a power law. At a low height in the cornona, the pressure forces cannot balance the Lorentz forces provided the field lines remain tied to the photosphere and an inward collapse with subsequent reconnection at the point closest approach should occur. Because of initial shear in the magnetic field, the reconnection would produce isolated helices above the point of reconnection since field lines would not interact with themselves but with their neighbors. This resulting topology produces a field above the elevated neutral line which is opposite in polarity to that of the photospheric field as in the current sheet models of Kuperus and Tandberg-Hanssen (1967). Raadu and Kuperus (1973), Kuperus and Raadu (1974), and Raadu (1979) and in agreement with recent observations of Leroy (1982), and Leroy et al. (1983). (orig./WL)

[en] Magnetic sectors on the sun are a feature, when the solar dipole field is subtracted, reminiscent of grapefruit sections in terms of the boundaries described by the magnetic field polarity change. One possible suggestion for the origin of these sectors is that they are hydromagnetic waves controlled by the rotation, toroidal magnetic field, and stratification within the convection zone of the sun. The merits of this suggestion are evaluated with respect to the observations and a specific theoretical model. 4 figs, 38 refs. (U.S.)