共查询到19条相似文献，搜索用时 109 毫秒
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综合APIA、HONOLULU、PAMATAI 3个地磁台三分量的11年周期变化的形态后，可定性地提出该变化源于内场。如内源为核幔边界的电涡流，则其中心点应位于3台之间。 相似文献
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地磁太阳黑子周变化起源的讨论 总被引：1，自引：1，他引：1
为了避开60年代末和70年代末Jerk(H)、Jerk(Z)的影响,分析了1979～1998年西欧4个台和1979～1999年亚洲东部6个台的H、Z资料,结果表明各台间H(或X)分量的太阳黑子周变化一致性较好.但Z分量的太阳黑子周变化显示出非常特别的现象,Z变化的相位随台站经度变化而变化,东亚地区的Z变化几乎与西欧地区的变化反向.因此,东亚地区的Z变化与H变化的关系不符合P01模式的假设,外源场之说似乎不能解释. 相似文献
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利用小波变换,分析了1749年以来每个太阳活动周太阳黑子相对数的最强周期以及第1～22太阳活动周的最强周期. 分析结果表明,在第5和第6个太阳活动周,太阳黑子相对数最强的周期分别为64.67年和69.31年;在第13～15太阳活动周,太阳黑子相对数的最强周期分别为98.02年,105.06年和105.06年. 在第1～22太阳活动周中,太阳黑子相对数最强的周期是128个月,约10.67年,其他太阳活动周的最强周期介于9.29～11.43年之间. 本文最后给出了128个月周期的幅度随时间的变化. 相似文献
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地磁日变幅的时空变化 总被引：3，自引：0，他引：3
胡久常 《地震地磁观测与研究》1992,13(3):73-77
本文利用13个全国Ⅰ类基准地磁台和3个Ⅱ类地磁台的《地磁观测报告》,通过对偏角、水平和垂直三分量日变幅值求季平均、年平均以及年滑动平均,再用各种均值点图,从而发现,(1)三分量日变幅皆有以一年为周期的季节变化和以约11年为周期的太阳黑子周变化;(2)三分量日变幅随地磁纬度的变化存在区域性,在区域内日变幅值与地磁纬度有明显的线性关系。此外,本文还对分析结果作了进一步的讨论。 相似文献
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北京地磁场变化特征分析 总被引：1，自引：1，他引：0
《地震地磁观测与研究》2015,(6)
根据北京国家地球观象台北京地震台1987—2013年地磁观测资料,分析该台地磁场长期变化和短期变化,认为北京地磁场长期变化具有缓慢上升、缓慢下降和逐渐恢复上升的形态,短期变化受太阳黑子活动强度影响,对了解北京地区地磁场变化特征具有一定意义。 相似文献
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本文用格林威治台1904——1953年的太阳黑子与磁暴资料及国家地震局编的全球7级以上地震的同期资料,对太阳黑子、磁暴与地震的关系作了统计分析。主要有以下几点结果: 1.太阳黑子、磁暴与地震数的逐年变化之间经11年流动平均后具有相当高的相关性,而后者与地震的相关性更显著; 2.地震频率的季节分布在统计上有类似磁暴的季节分布的倾向; 3.太阳黑子、磁暴对地震的触发作用有一个滞后效应,前者为3——4个月,后者为1——3个月;也还出现有同时性效应; 4.太阳黑子周期内地震最多的年份常发生在太阳黑子下降相位期间。 相似文献
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Matthew T. DeLand Richard P. Cebula Ernest Hilsenrath 《Studia Geophysica et Geodaetica》1998,42(2):83-91
The Shuttle SBUV (SSBUV) and NOAA-11 SBUV/2 instruments measured solar spectral UV irradiance during the maximum and declining phase of solar cycle 22. The SSBUV data accurately represent the absolute solar UV irradiance between 200–405 nm, and also show the long-term variations during eight flights between October 1989 and January 1996. These data have been used to correct long-term sensitivity changes in the NOAA-11 SBUV/2 data, which provide a near-daily record of solar UV variations over the 170–400 nm region between December 1988 and October 1994. The NOAA-11 data demonstrate the evolution of short-term solar UV activity during solar cycle 22. 相似文献
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An inspection of the long-term behaviour of the range of the daily geomagnetic field variation from comprehensive modelling 总被引：1，自引：0，他引：1
J. Miquel Torta Luis R. Gaya-Piqu Juan J. Curto David Altadill 《Journal of Atmospheric and Solar》2009,71(13):1497-1510
This paper attempts to reveal whether long-term trends in the ionosphere are reflected in the amplitude range of the geomagnetic daily variation recorded at ground level. The smooth and regular variation observed in the magnetograms on magnetically quiet days is induced by the ionospheric currents flowing in the dynamo region. So it is likely that trends in the conductivity or in the dynamics of this region could produce changes in the current densities, and consequently in the range of the geomagnetic variation. The crucial aspect is how to separate the changes produced by the geomagnetic activity itself, or by secular changes of the Earth's magnetic field, from the part of the variation produced by factors affecting trends in the ionosphere, which could have an anthropogenic origin. To investigate this, we synthesized for several geomagnetic observatories the daily ranges of the geomagnetic field components with a comprehensive model of the quiet-time, near-Earth magnetic field, and finally we removed the synthetic values from the observed ranges at those observatories. This comprehensive model accounts for contributions from Earth's core, lithosphere, ionosphere, magnetosphere and coupling currents, and, additionally, accounts for influences of main field and solar activity variations on the ionosphere. Therefore, any trend remaining in the residuals, assuming that all the contributions mentioned above are properly described and thus removed by the comprehensive model, should reflect the influence of other sources. Results, based on series of magnetic data from observatories worldwide distributed, are presented. Trends in the X and Z components are misleading, since the current system changes in form as well as in intensity, producing changes of the focus latitude in the course of a solar cycle and from one cycle to another. Some differences exist between the long-term trends in the Y component between the real and modelled ranges, suggesting that other non-direct solar causes to the amplitude changes of the solar quiet geomagnetic variation should not be ruled out. Nevertheless, the results also reflect some short-comings in the way that the comprehensive modelling accounts for the influence of the solar activity on the range of the daily geomagnetic variation. 相似文献
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The relationships between a number of the main characteristic parameters of the cycle—amplitude, half-width, and growth phase duration—and the approximation parameters, which make it possible to estimate the average behavior of 11-year activity, have been derived based on the obtained analytical representations of the regularities in the solar activity variations during the cycle. Quasibiennial variations proceeding against a background of the cycle are distinctly associated with the solar magnetic field structure and the structure representation variations in the corona and in the flux of the solar neutrino radiation. This makes it possible to state that all these processes are parts of the common physical mechanism of solar variability. 相似文献
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本文将G.M.Brown等人对离Sq电流体系焦点较远处台站的异常静日（AQD）的H分量分析,发展为对包括Sq电流体系焦点附近台站和Z、D分量在内的AQD分析。主要分析了中国五个地磁台D、H、Z三要素静日最大值和最小值出现时间的分布,及其季节变化和逐年变化规律。结果表明,D、Z也有和H类似的AQD现象,其出现的年频度,也有与太阳黑子数反相变化的趋势。在有三个多太阳周资料的佘山台,太阳极小年AQD(Zmax)出现的频度,和随后的太阳极大年的黑子数R呈近似线性的关系。最后,本文对今后我国开展变化磁场的分析研究提出了建议。 相似文献
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The model of variations in the orthohelium 1083 nm emission intensity has been constructed based on the measurements at different stations. The analytical approximations of the nighttime intensity variations depending on the phase age of the Moon, season, solar activity during the 11-year cycle, and geomagnetic disturbances are presented. 相似文献
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B. Soukharev 《Annales Geophysicae》1997,15(12):1595-1603
The interaction between the factors of the quasi-biennial oscillation (QBO) and the 11-year solar cycle is considered as an separate factor influencing the interannual January–March variations of total ozone over Northeastern Europe. Linear correlation analysis and the running correlation method are used to examine possible connections between ozone and solar activity at simultaneous moment the QBO phase. Statistically significant correlations between the variations of total ozone in February and, partially, in March, and the sunspot numbers during the different phases of QBO are found. The running correlation method between the ozone and the equatorial zonal wind demonstrates a clear modulation of 11-y solar signal for February and March. Modulation is clearer if the QBO phases are defined at the level of 50 hPa rather than at 30 hPa. The same statistical analyses are conducted also for possible connections between the index of stratospheric circulation C1 and sunspot numbers considering the QBO phase. Statistically significant connections are found for February. The running correlations between the index C1 and the equatorial zonal wind show the clear modulation of 11-y solar signal for February and March. Based on the obtained correlations between the interannual variations of ozone and index C1, it may be concluded that a connection between solar cycle – QBO – ozone occurs through the dynamics of stratospheric circulation. 相似文献
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R. T. Gushchina A. V. Belov E. A. Eroshenko V. N. Obridko E. Paouris B. D. Shelting 《Geomagnetism and Aeronomy》2014,54(4):430-436
Recent years allowed us to study long-term variations in the cosmic ray (CR) intensity at an unusually deep solar activity (SA) minimum between cycles 23 and 24 and during the SA growth phase in cycle 24, which was the cycle when SA was the lowest for the epoch of regular ground-based CR observations since 1951. The intensity maximum, the value of which depends on the particle energy, was observed in CR variations during the period of an unusually prolonged SA minimum: the CR density during the aformentioned period (2009) is higher than this density at previous CR maxima in cycles 19–23 for low-energy particles (observed on spacecraft and in the stratosphere) and medium-energy particles (observed with neutron monitors). After 2009 CR modulation at the SA growth phase was much weaker over three years (2010–2012) than during the corresponding SA growth periods in the previous cycles. The possible causes of this anomaly in CR variations, which are related to the CR residual modulation value at a minimum between cycles 23 and 24 and to variations in SA characteristics during this period, were examined. The contribution of different solar magnetic field characteristics and indices, taking into account sporadic solar activity, has been estimated. 相似文献
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Data from three solar observatories (Learmonth, Holloman, and San Vito) are used to study the variations in the average number of sunspots per sunspot group. It is found that the different types of sunspot groups and the number of sunspots in these groups have different solar cycle and cycle to cycle variations. The varying ratio between the average number of sunspots and the number of sunspot groups is shown to be a real feature and not a result of changing observational instruments, observers’ experience, calculation schemes, etc., and is a result of variations in the solar magnetic fields. Therefore, the attempts to minimize the discrepancies between the sunspot number and sunspot group series are not justified, and lead to the loss of important information about the variability of the solar dynamo. 相似文献