Dynamics of the photospheric magnetic field in the vicinity of the solar equator |
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| Authors: | V N Obridko V E Chertoprud |
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| Institution: | 1.Pushkov Institute of Terrestrial Magnetism, the Ionosphere, and Radio Wave Propagation,RAN,Moscow,Russia |
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| Abstract: | SOHO-MDI daily magnetic field synoptic data (a 14-year series of daily maps of the solar magnetic field intensity B available at the site ) have been used to analyze the dynamics of the photospheric magnetic field in the vicinity of the solar equator. The standard
deviation s
B
of the field B calculated over areas of tens of square degrees on the solar disk was taken as a basic index. An 11-year variation similar
to that observed at higher latitudes is observed in the vicinity of the equator, and is similar for weak and strong fields;
i.e., the solar cycle exists in the sunspot-free zone. New qualitative data support the idea that the weak background magnetic
field increases toward the solar limb. This angular dependence suggests the existence of a transverse component of the background
field. The magnetic fields in the vicinity of the equator were significantly different in the initial phases of Cycles 23
and 24. Annual variations of s
B
were observed near the center of the solar disk. These variations are due to two factors: the annual variation of the distance
from the equator to the disk center and the increase of s
B
with with distance from the equator. Reliable detection of these variations is an evidence of high accuracy of the s
B
estimates. |
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