On stability of rotation of the mean magnetic field of the Sun
On stability of rotation of the mean magnetic field of the Sun
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DOI：
10.1051/0004-6361:20030426
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发表时间：
2003-06
影响因子：
6.5
通讯作者：
V. I. Haneychuk;V. Kotov;T. Tsap
中科院分区：
文献类型：
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作者：
V. I. Haneychuk;V. Kotov;T. Tsap
本文介绍了克里米亚天体物理天文台1998-2001年测量的太阳平均磁场（MMFS）的新数据。本文考虑了使用其他三个观测站类似数据的34年MMFS时间序列（1968-2001年，每日MMFS值总数N = 12 428）。结果表明：(a)近34年来太阳磁场赤道旋转的主要合势周期$P_\odot = 26.929 \pm 0.015$ d没有变化，但(b)光球大尺度场的平均强度h0按模量计算下降了约4.5%（置信水平约为80%）。得出的结论是，较长的90年周期可能是h0可能逐渐减少的原因。MMFS随主旋转周期的平均变化曲线显示出明显的N - S极性不对称，这可能与太阳整体的四极分量和“磁不平衡”有关。
New data on the mean magnetic field of the Sun (MMFS) as a star measured at the Crimean Astrophysical Observatory in 1998–2001 are presented. The 34-year time series of the MMFS using similar data from three other observatories (1968–2001, with the total number of daily MMFS values N = 12 428), is considered. It is found that (a) the primary synodic period of the equatorial rotation of solar magnetic field, $P_\odot = 26.929 \pm 0.015$ days, did not vary over the last 34 years, but (b) the average intensity H 0 of the photospheric large-scale fields, by modulus, decreased by about 4.5% (with a confidence level of about 80%). The conclusion is made that the longer, 90-year, cycle might be responsible for this potential gradual decrease of H 0 . The average curve of MMFS variation as plotted with the primary rotational period $P_\odot$ demonstrates an obvious N - S asymmetry of polarities, perhaps associated with the quadrupole component and “magnetic disequilibrium” of the Sun as a whole.