FIG 10 - uploaded by Aake Nordlund
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![ÈSame as Fig. 9, but for seismic events exceeding a maximum seismic Ñux of 40 kW m~2. The number of events that contribute to each displayed value varies between 2861 and 4455, and the number of velocity data values between 2861 and 1,766,766. The displayed contrast ranges between [10 and ]10 m s~1 in panels a, b, c, between 222 and 306 m s~1 in panels d, e, and between 222 and 255 m s~1 in panel f.](profile/Aake-Nordlund/publication/2741231/figure/fig2/AS:341306695012356@1458385265577/ESame-as-Fig-9-but-for-seismic-events-exceeding-a-maximum-seismic-Nux-of-40-kW-m2-The.png)
ÈSame as Fig. 9, but for seismic events exceeding a maximum seismic Ñux of 40 kW m~2. The number of events that contribute to each displayed value varies between 2861 and 4455, and the number of velocity data values between 2861 and 1,766,766. The displayed contrast ranges between [10 and ]10 m s~1 in panels a, b, c, between 222 and 306 m s~1 in panels d, e, and between 222 and 255 m s~1 in panel f.
Source publication
. We compare observations of the excitation of solar oscillations with simulations. We pass synthetic line profile data through the same analysis scheme used for observed line profiles. We find in both cases that seismic events exciting the oscillations are largely confined to the dark intergranular lanes. The excitation is closely associated with...
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Citations
... The Goode et al. results were based on the mixing length approximation that postulates that upflows and downflows are symmetric, simulations of convection have shown that this is not the case at all, and in fact that the downflows are fast and cold and are what are observed as intergranular lanes, and that upflows are slow and hot. Observations now suggest that the sources of excitation are not exploding granules, instead they are located in the dark intergranular lanes (Rimmele et al. 1995) and are related to the collapse of these lanes (Goode et al. 1999). ...
The seismic study of the Sun and other stars offers a unique window into the interior of these stars. Thanks to helioseismology, we know the structure of the Sun to admirable precision. In fact, our knowledge is good enough to use the Sun as a laboratory. We have also been able to study the dynamics of the Sun in great detail. Helioseismic data also allow us to probe the changes that take place in the Sun as solar activity waxes and wanes. The seismic study of stars other than the Sun is a fairly new endeavour, but we are making great strides in this field. In this review I discuss some of the techniques used in helioseismic analyses and the results obtained using those techniques. In this review I focus on results obtained with global helioseismology, i.e., the study of the Sun using its normal modes of oscillation. I also briefly touch upon asteroseismology, the seismic study of stars other than the Sun, and discuss how seismic data of others stars are interpreted.
... Поэтому стоит задаться вопросом связи Тунгусского феномена с выбросом с Солнца не только плазмоида, но и маскона тяжелых частиц. С учетом наших скудных знаний о Солнце, сегодня можно допускать эжекцию в 1908 г. с Солнца тёмной материи в форме зеркальной [Foot, 2001], вимпов 146 [Faulkner, 1986], сверхтяжелых ядер «острова стабильности», антивещества [NASA-GSFC], сверхпроводящих водорода или железа и т.д. Например, в июне, когда скорость вращения Земли складывается со скоростью вращения Солнечной системы вокруг центра Галактики, вимп-потоки обтекания Земли должны быть максимальны. ...
Книга - научное исследование основных альтернативных гипотез Тунгусского феномена 1908 г. (in Russian).
