我国低钛月海型模拟月壤初始物质选择的地球化学依据   总被引：1，自引：0，他引：1  

刘春茹  王世杰  冯俊明  李雄耀  付绍洪  欧阳自远  郑永春 《矿物岩石》2007,27(3):28-33

以Apollo14月壤样品和美国JSC-1模拟月壤的地球化学特征为基础,结合我国低钛玄武岩火山的分布,对我国不同地区新生代玄武岩的化学成分、年龄、储量等方面进行对比分析结果表明,滇西北金沙江地区和吉林辉南红旗林场-四海地区的玄武质火山喷发物的化学成分与Apollo14月壤样品和美国JSC-1模拟月壤相似,比较适合用于我国低钛月海玄武岩模拟月壤研制的初始物质。野外地质调查发现,吉林省辉南县金川镇红旗林场—四海一带产出的玄武质火山渣为距今1600 a的该玄武质火山岩的喷发物,其储量大、质地纯、粒度均匀,而且比滇西北金沙江地区最近一期的玄武质火山渣新鲜,最适合作为我国低钛月海玄武岩模拟月壤研制的初始物质。  相似文献   

陆相沉积的天文地层研究方法简介——以井下地层为例   总被引：2，自引：5，他引：2  

XU Dao-yi )  ZHANG Hai-feng )  HAN Yan-ben )  YIN Zhi-qiang )  LI Bao-li )  YAO Yi-min ) ) Institute of Geology  China Earthquake Administration  Beijing    ) Geological Scientific Research Institute of Shengli Oilfield Company  SINOPEC  Dongying    ) National Astronomical Observatories  Chinese Academy of Sciences  Beijing 《地层学杂志》2007,(Z2)

通过对我国大陆三十余口井的测井资料研究成果,归纳出对陆相地层进行天文地层研究的方法。介绍了所用的新的天文周期理论值、测井资料的选取及预处理方法,重点说明谱分析的数据点数的选定、不同参数(自然伽玛、自然电位和岩屑)的测井资料谱分析结果的对比,以实例说明如何选定主要优势旋回和AR值,以及FIR数字滤波器的基本性质和数字滤波结果,小波分析的特点和通过小波图进行调频的方法,并介绍了地层单位的延续时间计算和年龄确定方法。  相似文献   

流感世界大流行的气候特征     

杨冬红  杨学祥 《沙漠与绿洲气象(新疆气象)》2007,1(3):1-8

流感爆发与气候的剧烈变化有关。本文揭示了拉马德雷冷位相、拉尼娜、太阳黑子极值年、厄尔尼诺、低温冷害、沙尘暴、潮汐南北震荡异常与流行性感冒世界大流行相互对应的关系及其物理机制,对气候及其相关灾害的预测有重大科学意义。规律表明,在拉马德雷冷位相时期,全球强震、低温、飓风伴随拉尼娜、全球性流感伴随厄尔尼诺将越来越强烈。面对日益增大的全球灾害,长期气候预报意义重大。  相似文献   

潮汐和地震对全球气候变化的影响   总被引：1，自引：0，他引：1  

杨冬红  杨学祥 《沙漠与绿洲气象(新疆气象)》2007,1(4):5-12

2004年12月26日印尼地震海啸后,全球低温冻害和暴雪灾害频繁发生。"潮汐调温说"和"深海巨震降温说"是一种合理的解释。根据"潮汐调温说"和"深海巨震降温说"理论,2005年全球气温将因为印尼地震海啸和强潮汐南北震荡而降低。美国国家航空航天局(NASA)的科学家认为,一个较弱的厄尔尼诺现象和人类排放的温室气体将使2005年成为人类有记载以来最热的一年。事实上,2005年的温度低于1998年。现在,西方科学家也承认了2005—2007年自然气候的变化抵消了全球气候变暖效应这一客观事实。  相似文献   

The properties of jet in luminous blazars under the equipartition condition     

《New Astronomy》2017

In this work, we study the physical properties of the high-energy (HE) emission region by modeling the quasi-simultaneous multi-wavelength(MWL) spectral energy distributions (SEDs) of 27 Fermi-LAT detected low-synchrotron-peaked (LSP) blazars. We model the jets MWL SEDs in framework of a well accepted single-zone leptonic model including synchrotron self-Compton and external Compton (EC) processes for the jets in a state of equipartition between particle and magnetic field energy densities. In the model the GeV γ-ray spectrum is modeled by a combination of two different external Compton-scattered components: (i) EC scattering of photons coming from disk and broad line region (BLR), and (ii) EC scattering of photons originating from the dust tours (DT) and BLR. We find that the SEDs can be well reproduced by the equipartition model for the most majority of the sources, and the results are in agreement with many recent studies. Our results suggest that the SEDs modelling alone may not provide a significant constraint on the location of the HE emission region if we do not know enough about the physical properties of the external environment.  相似文献   

Optical monitoring observations of two γ-ray narrow-line Seyfert 1 galaxies     

《New Astronomy》2016

1H 0323+342 is a rather radio-loud narrow-line Seyfert 1 galaxy (NLS1) with γ-ray emission. Optical observations were carried out in B and R bands which covered 6 nights in 2011 to obtain light curves of 1H 0323+342. The difference image subtraction method was used to deal with the data of 1H 0323+342 because of the existence of extended host galaxy. Optical variability on day timescale was reported here. We also monitored the first γ-ray NLS1 SDSS J094857.3+002225 and confirmed the existence of intranight optical variability (INOV). These indicated the existence of a relativistic jet in these NLS1s.  相似文献   

Eruption of an Active-Region Filament Driven by an Emerging Bipole     

Yun-Chun Jiang  Yuan-Deng Shen  Jing-Xiu Wang National Astronomical Observatories / Yunnan Observatory  Chinese Academy of Sciences  Kunming  National Astronomical Observatories  Chinese Academy of Sciences  Beijing 《中国天文和天体物理学报》2007,7(1):129-140

1 INTRODUCTION Filaments are cool, dense material suspended in the hot, tenuous corona. It is widely accepted that the global magnetic field surrounding the filaments plays a key role in their formation, structure and stability (Tandberg-Hanssen1995). Fil…  相似文献   

天文底片保存和我国天文底片数字化的建议     

金文敬  唐正宏  王叔和  姚保安  田凯平  陈力  赵永恒  蒋世仰 《天文学进展》2007,25(1):1-12

阐述了国际上天文照相底片数字化工作的进展:底片的保存、底片数字化的意义和相关技术。扼要地介绍了国际虚拟天文台的情况及其与底片数字化的关系。分析了我国天文底片资料的保存现状,并提出了底片数字化建议:成立由各天文台专家组成的全国底片数字化协调小组,建立各单位保存底片的信息库、改进底片的保存条件、有步骤地对有价值底片上的全部目标进行扫描,以便将其与现代高精度的观测资料相结合,开展有意义的课题研究。  相似文献   

The X10 Flare on 29 October 2003: Was It Triggered by Magnetic Reconnection between Counter-Helical Fluxes?     

Yu Liu  Hiroki Kurokawa  Chang Liu  David H. Brooks  Jingping Dun  Takako T. Ishii  Hongqi Zhang 《Solar physics》2007,240(2):253-262

Vector magnetograms taken at Huairou Solar Observing Station (HSOS) and Mees Solar Observatory (MSO) reveal that the super active region (AR) NOAA 10486 was a complex region containing current helicity flux of opposite signs. The main positive sunspots were dominated by negative helicity fields, while positive helicity patches persisted both inside and around the main positive sunspots. Based on a comparison of two days of deduced current helicity density, pronounced changes associated with the occurrence of an X10 flare that peaked at 20:49 UT on 29 October 2003 were noticed. The average current helicity density (negative) of the main sunspots decreased significantly by about 50%. Accordingly, the helicity densities of counter-helical patches (positive) were also found to decay by the same proportion or more. In addition, two hard X-ray (HXR) “footpoints” were observed by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) during the flare in the 50 – 100 keV energy range. The cores of these two HXR footpoints were adjacent to the positions of two patches with positive current helicity that disappeared after the flare. This strongly suggested that the X10 flare on 29 October 2003 resulted from reconnection between magnetic flux tubes having opposite current helicity. Finally, the global decrease of current helicity in AR 10486 by ∼50% can be understood as the helicity launched away by the halo coronal mass ejection (CME) associated with the X10 flare. Electronic Supplementary Material The online version of this article () contains supplementary material, which is available to authorized users.  相似文献   

天体物理环境中的硅酸盐尘粒   总被引：1，自引：0，他引：1  

李墨萍  赵刚  李爱根 《天文学进展》2007,25(2):132-146

硅酸盐尘粒是宇宙尘埃的主要成分之一,它广泛存在于许多天体物理环境中,其特性随环境而变化。由于近年来观测数据的不断增加和红外光谱质量的逐步提高,宇宙空间中的硅酸盐尘粒正受到越来越多的关注．该文详细地介绍了在各种天体环境(星际空间、演化晚期恒星的星周尘埃包层、绕年轻恒星和主序星的星周尘埃盘、彗星的彗发和行星际空间)中的硅酸盐尘粒的观测特征,并分别对其物理和化学性质进行了综合比较．观测已经证实在星际尘埃演化的前身(演化晚期恒星的星周尘埃包层)和其遗迹(彗星)均有可观数量的结晶硅酸盐存在。但是至今还没有在其中间态(弥散星际介质)找到结晶硅酸盐存在的证据。这一尚未解决的难题突出了结晶态硅酸盐在天体物理研究中的重要意义。  相似文献