吴尚时对中国近代地理学的贡献与学术思想探讨

吴尚时（1904-1947）是中国近代地理学重要开创者之一。1928年吴尚时获金牌毕业于中山大学,次年考取公费前往法国学习地理学。他先后就读于里昂大学和格日诺布尔大学,授业于A. 阿历克斯,M.巴尔台和R.布朗夏尔等,布氏是维达尔·布拉什知名弟子。1934年吴氏学成归国,任中山大学地理系教授,1939-1945年任地理系主任。时逢日军侵华,学校不断搬迁逃避战火,华南、西南千里迁徙之途成为先生的野外考察路线,这需要非同一般的坚毅意志和对科学的献身精神。先生学术文稿泰半完成于此艰危时期,过度的劳累和极度困苦的环境严重损害了他的健康。1947年,先生去世,年仅43岁。     

典型的太阳质子事件峰值流量的一种预报方法

分析了1988~2006年中62个典型的太阳质子事件,发现其归一化后峰值流量变化具有很好的统计规律,根据该规律提出了一种对太阳质子事件峰值流量进行预报的方法.试验预报结果表明,太阳质子事件峰值流量的预报值和实测值都在同一个量级以内,平均相对误差为32％,预报误差在可接受范围内.本文方法对于日常预报业务而言是实用和可行的.     

第22太阳周活动区M级以上X射线耀斑指数的统计

本文对第２２太阳周（１９８７年１月至１９９２年１２月）中发生过Ｍ级以上的Ｘ射线耀斑（Ｈα耀斑级别≥Ｍ级，并伴有Ｘ射线的耀斑）对应的３９５个活动区资料进行了耀斑指数的统计，得到的结果：１．２２太阳周Ｍ级以上Ｘ射线耀斑级别综合指数表，２．２２太阳周Ｍ级以上Ｘ射线耀斑总指数表，３．第２２太阳周Ｍ级以上Ｘ射线耀斑总指数随时间的变化曲线，４．第２２太阳周Ｍ级以上Ｘ射线濯斑总指数直方图，该图表明第２２太阳周活动的极大年分别是１９８９和１９９１年，为第２３周太阳活动预报提供了可用参数。     

Morlet小波显著性检验和精度分析在地磁场和地震活动性周期分析中的应用

首先通过对加入随机噪声的合成信号进行Morlet小波变换并进行显著性检验, 分析所得信号的周期成分的显著性和非显著性, 然后研究信号周期长短、 信号观测时间段长短与精度之间的关系．在此基础上,以活动周期比较稳定的太阳黑子活动作为实例分析,结果显示本文的精度分析和显著性检验方法对于周期谱的精度和显著性研究是可行的．最后将该方法应用于全球地震活动周期谱的分析,求出全球地震活动周期谱及其显著性与精度．研究结果表明,在利用Morlet小波分析地磁场和地震活动性周期时引入显著性检验,并结合本文给出的精度, 可以从数据中提取出周期谱及其显著性和精度．      

On the interaction of internal gravity waves with a magnetic field – I. Artificial wave forcing

We present results from numerical simulations of the interaction of internal gravity waves (IGW) with a magnetic field. In accordance with the dispersion relation governing IGW in the presence of magnetism and rotation, when the IGW frequency is approximately that of the Alfvén frequency, strong reflection of the wave occurs. Such strong reflection markedly changes the angular momentum transport properties of the waves. In these simple models a strong, time-independent shear layer develops, in contrast to the oscillating shear layer that develops in the purely hydrodynamic case.     

太阳中微子问题

文中从中微子物理学、太阳中微子的探测、标准太阳模型的建立等方面对太阳中微子问题的提出进行了回顾。各为太阳中微子探测器测量结果不同程度的偏低，以及不同类探测器测量结果之间的矛盾，使得人们对太阳中微子的研究表现出浓厚的兴趣。对太阳中微子问题可从粒子物理和天体物理两个方面进行研究。文中分别对这两个研究领域中提取的企图解决太阳中微子问题的模型作了简要评述。     

Search for periodicities of the solar irradiance data from the Earth Radiation Budget Satellite (ERBS) using the periodogram method

We have analyzed the solar irradiance data from the Earth Radiation Budget Satellite(ERBS)during the time period from 1984 October 15 to 2003 October 15.By first filtering the data by Simple Exponential Smoothing,we have applied the periodogram method to the processed data in order to search for its time variation.The study exhibits multi-periodicities on these data around 110,118,574 and 740d with very high confidence levels(more than 99%).These periods are significantly similar to the periods of other solar activities which may suggest that solar irradiance may be associated with other solar activities.     

解决太阳横向磁场方向测定中180°不确定性的一个方法

本文提出了一种解决太阳横向磁场方向测定中１８０°不确定性的方法。该方法首先将Ｇａｒｙ等提出的方法定量化，客观地确定每一点的横场方向；然后由独立的Ｈ＿α观测或磁场演化历史，分析和确定磁力线的拓扑联接性，对客观确定的横场方向做经验修正。对活动区的应用表明，该方法是一个可供选择的解决横场方向不确定性的有效方法。     

Grand Minima of Solar Activity and the Mean-Field Dynamo

We demonstrate that a simple solar dynamo model, in the form of a Parker migratory dynamo with random fluctuations of the dynamo governing parameters and algebraic saturation of dynamo action, can at least qualitatively reproduce all the basic features of solar Grand Minima as they are known from direct and indirect data. In particular, the model successfully reproduces such features as an abrupt transition into a Grand Minimum and the subsequent gradual recovery of solar activity, as well as mixed-parity butterfly diagrams during the epoch of the Grand Minimum. The model predicts that the cycle survives in some form during a Grand Minimum, as well as the relative stability of the cycle inside and outside of a Grand Minimum. The long-term statistics of simulated Grand Minima appears compatible with the phenomenology of the Grand Minima inferred from the cosmogenic isotope data. We demonstrate that such ability to reproduce the Grand Minima phenomenology is not a general feature of the dynamo models but requires some specific assumption, such as random fluctuations in dynamo governing parameters. In general, we conclude that a relatively simple and straightforward model is able to reproduce the Grand Minima phenomenology remarkably well, in principle providing us with a possibility of studying the physical nature of Grand Minima.     

Submillimeter-wave and observations of the event on 28 November, 2001

We present a detailed study of a 1B/M6.9 impulsive flare combining high time resolution (1 ms) and instantaneous emission source localization observations at submillimeter frequencies (212 GHz), obtained with the solar submillimeter telescope (SST), and Hα data from the Hα solar telescope for argentina (HASTA). The flare, starting at 16:34 UT, occurred in active region (AR) 9715 (NOAA number) on November 28, 2001, and was followed by an Hα surge. We complement our data with magnetograms from the Michelson Doppler Imager (SOHO/MDI). SST observed a short impulsive burst at 212 GHz, presenting a weak bulk emission (of about 90 sfu) composed of a few shorter duration structures. The integrated Hα and the 212 GHz light curves present a remarkable agreement during the impulsive phase of the event. The delay between both curves stays below 12 s (the time resolution of the Hα telescope). The flare as well as the surge are linked to new flux emergence very close to the main AR bipole. Taking into account the AR magnetic field evolution, we infer that magnetic field reconnection, occurring at low coronal levels, could have been at the origin of the flare; while in the case of surge this would happen at the chromospheric level.