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It is demonstrated that, at high rigidities (50 GV and beyond), all the main features of cosmic-ray anisotropy of solar origin
can be explained in terms of regular particle motion —without diffusion being involved — in the large-scale interplanetary
magnetic field (IMF). A simple model of the IMF is adopted with a corotating warped neutral sheet separating the regions of
alternative polarities; the warped shape is indispensable for obtaining any form of anisotropy. Energy losses occurring along
various computed trajectories are calculated to give the sidereal, solar and antisidereal intensity waves. The reliability
of the variations obtained are checked by changing the parameters of the IMF model. Both the sense and amplitude of the polarity-dependent
sidereal vector are compatible with those established experimentally. Also reproduced are the predictions of corotation in
addition to the 3-hour phase of the semi-diurnal wave. The corotation is found to be near perfect at 50 GV, while it reduces
at 100 GV. The model presented accounts for the change of solar daily vector that was observed in 1969. 相似文献
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K. Vida Zs. Kőovári M. Švanda K. Oláh K.G. Strassmeier J. Bartus 《Astronomische Nachrichten》2007,328(10):1078-1080
We re-investigate UZ Libræ spectra obtained at KPNO in 1998 and 2000. From the 1998 data we compose 11 consecutive Doppler images using the Ca I-6439, Fe I-6393 and Fe I-6411 lines. Applying the method of average cross-correlation of contiguous Doppler images we find anti-solar differential rotation with a surface shear of α ≈ –0.03. The pilot application of the local correlation tracking technique for the same data qualitatively confirms this result and indicates complex flow pattern on the stellar surface. From the cross-correlation of the two available Doppler images in 2000 we also get anti-solar differential rotation but with a much weaker shear of α ≈ –0.004. (© 2007 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim) 相似文献
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