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D. N. Rachkovsky T. T. Tsap V. G. Lozitsky 《Journal of Astrophysics and Astronomy》2005,26(4):435-445
We analyse different observational data related to the problem of intrinsic magnetic field strength in small-scale fluxtubes
outside sunspots. We conclude that the kG range of fluxtube fields follows from not only classical line ratio method, but
also from other old and new techniques. For the quiet regions on the Sun, the most probable mode of such fields has a magnetic
field strength of 1.2–1.5 kG assuming the rectangular field profile. To best interpret the observations, a weak background
field between fluxtubes should be assumed, and its magnetic field strength is expected to increase with the filling factor
of fluxtubes. The alternative point of view about subkilogauss fluxtube fields is critically examined, and possible sources
of different conclusions are presented. 相似文献
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Measurements of the fluxtube field strength B and filling α in solar flares, active regions and faculae have been analyzed. To estimate the values of B, Stokes V peak separations of the Fe I 5247 Å and Fe I 5250 Å lines have been used. It was found that the value of B in an In-flare (˜ 1.1 kG) was slightly smaller than that in faculae (˜ 1.3 kG) and a non-flare active region (˜ 1.4kG). On the other hand, in a more power 2b-flare the value of B was in the range from. 1.1 kG (the start of the flare) to 1.55kG. (during the peak). Thus the values of the field strength of flares somewhat differ from those both of faculae and active regions. The magnetic filling factor is approximately equal in flares (0.2-0.40) and active regions (0.3) but several times larger as compared with faculae. 相似文献
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