... M for the case 1 0 2 are as follows: MM 11 = cos ( g ) cosh ( f ) k 1 sin ( g ... m ) / c , 2 2 M f k2 ( L x1 ) , Note that the eigenvalues of the matrix M, which ...
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Ссылки http://www.izmiran.rssi.ru/~gchernov/PlasPhys2_09LaptukovlLO.pdf -- 275.9 Кб -- 13.05.2009 Похожие документы
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... 12. B. Vrsnak, M. Temmer, and A. M. Veronig, Solar Phys. 240, 315 (2007). 13. ... 13. B. Vrsnak, M. Temmer, and A. M. Veronig, Solar Phys. 240, 331 (2007). 14. ...
... atmospheric radioactivity V. M. Sorokin1 , A. K. Yaschenko1 , and M. Hayakawa2 1 2 ... m 1 12 Er, max , mV/m 12 8 8 4 2 3 4 100 200 300 400 0 -40 r , km 0 2 4 6 8 Ez , V/m ...
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Ссылки http://www.izmiran.rssi.ru/~sova/Copies/nhess-7-155-2007.pdf -- 448.1 Кб -- 02.02.2007 Похожие документы
... 12 A band contains both the transition-region HeII (Te 0.05 M) line and the lower-intensity coronal SiXI (Te 1.6 M) line ... 5 2004 SOLAR ERUPTIVE EVENT 411 (b) 10 3 () SOHO/LASCO/C2 10 F, W m2 4 X GOES 18 е M 10 5 10 6 C 107 GOES 0.5 4 е 108 ...