Supergiant Complexes of Solar Activity and Convection Zone

被引：6
作者：
Arkhypov, O. V. [1 ,2 ]
Antonov, O. V. [1 ,2 ]
Khodachenko, M. L. [3 ]
机构：
[1] Natl Acad Sci Ukraine, Inst Radio Astron, UA-61002 Kharkov, Ukraine
[2] Kharkiv VN Karazin Natl Univ, Kharkov, Ukraine
[3] Austrian Acad Sci, Space Res Inst, A-8010 Graz, Austria
来源：
SOLAR PHYSICS | 2011年 / 270卷 / 01期
基金：
奥地利科学基金会;
关键词：
Active regions; Convection zone; Turbulence; EMERGING FLUX TUBES; TURBULENT CONVECTION; ROTATION; FIELDS; CELLS;
D O I：
10.1007/s11207-011-9734-5
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
The global distribution of solar surface activity (active regions) is apparently connected with processes in the convection zone. The large-scale magnetic structures above the tachocline could in a pronounced way be observable in the surface magnetic field. To get the information regarding large-scale magnetic formations in the convection zone, a set of solar synoptic charts (Mount Wilson 1998 2004, Fe I, 525.02 nm) have been analyzed. It is shown that the longitudinal dimensions and dynamics of supergiant complexes of solar surface activity carry valuable information about the processes in the convection zone of the Sun. A clear effect of large-scale (global) turbulence is found. This is a 'fingerprint' of deep convection, because there are no such large-scale turbulent eddies in the solar photosphere. The preferred scales of longitudinal variations in surface solar activity are revealed. These are: similar to 24 degrees (gigantic convection cells), 90 degrees, 180 degrees and 360 degrees.
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页码：1 / 8
页数：8
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