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Mid-Term Quasi-Periodicities and Solar Cycle Variation of the White-Light Corona from 18.5 Years (1996.0-2014.5) of LASCO Observations

机译:LASCO观测18.5年(1996.0-2014.5)的白光电晕的中期准周期和太阳周期变化

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We report on the analysis of the temporal evolution of the solar corona based on 18.5 years (1996.0 -aEuro parts per thousand 2014.5) of white-light observations with the SOHO/LASCO-C2 coronagraph. This evolution is quantified by generating spatially integrated values of the K-corona radiance, first globally, then in latitudinal sectors. The analysis considers time series of monthly values and 13-month running means of the radiance as well as several indices and proxies of solar activity. We study correlation, wavelet time-frequency spectra, and cross-coherence and phase spectra between these quantities. Our results give a detailed insight on how the corona responds to solar activity over timescales ranging from mid-term quasi-periodicities (also known as quasi-biennial oscillations or QBOs) to the long-term 11 year solar cycle. The amplitude of the variation between successive solar maxima and minima (modulation factor) very much depends upon the strength of the cycle and upon the heliographic latitude. An asymmetry is observed during the ascending phase of Solar Cycle 24, prominently in the royal and polar sectors, with north leading. Most prominent QBOs are a quasi-annual period during the maximum phase of Solar Cycle 23 and a shorter period, seven to eight months, in the ascending and maximum phases of Solar Cycle 24. They share the same properties as the solar QBOs: variable periodicity, intermittency, asymmetric development in the northern and southern solar hemispheres, and largest amplitudes during the maximum phase of solar cycles. The strongest correlation of the temporal variations of the coronal radiance - and consequently the coronal electron density - is found with the total magnetic flux. Considering that the morphology of the solar corona is also directly controlled by the topology of the magnetic field, this correlation reinforces the view that they are intimately connected, including their variability at all timescales.
机译:我们报告了基于SOHO / LASCO-C2日冕仪的18.5年白光观测结果(1996.0 -a欧元每千欧元2014.5)的太阳日冕时间演变分析。通过首先在全球范围内,然后在纬度范围内生成K-电晕辐射的空间积分值,可以量化这种演变。该分析考虑了月度值的时间序列和辐射的13个月运行平均值以及太阳活动的多个指标和代理。我们研究这些量之间的相关性,小波时频频谱以及互相干和相位频谱。我们的研究结果提供了关于电晕如何在从中期准周期(也称为准两年周期振荡或QBO)到长期11年太阳周期的时间范围内对太阳活动做出反应的详细见解。连续的太阳最大值和最小值之间的变化幅度(调制因子)在很大程度上取决于循环的强度和日照纬度。在太阳周期24的上升阶段观察到不对称现象,在皇家和极地地区尤为明显,北偏。最突出的QBO在太阳周期23的最大阶段是一个近似一年的周期,在太阳周期24的上升和最大阶段是一个较短的周期(七到八个月)。它们具有与太阳QBO相同的特性:周期性可变,间歇性,北部和南部太阳半球的不对称发展以及在太阳周期最大阶段的最大振幅。发现总辐射通量的时间变化与冠状辐射的时间变化之间存在最强的相关关系,因此也与冠状电子密度相关。考虑到太阳电晕的形态也直接受磁场拓扑控制,因此这种相关性增强了这样一种观点,即它们紧密相连,包括在所有时间范围内的可变性。

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