木星大气探测综述     

魏强  胡永云 《大气科学》2018,42(4):890-901

我国计划在2030年发射木星探测飞船,相关工程技术、科学目标论证的前期准备工作已经开始。为了更好地规划我国木星探测的科学目标,我们在本文系统地总结了美欧在过去几十年所进行的历次木星探测项目及其大气探测成果。到目前为止,已成功发射的有关木星的探测飞船共有9次,其中7次为飞越探测（飞船在飞越木星时顺带进行了木星的探测）,另外2次为专门探测（专门为了探测木星而发射的飞船）,分别为伽利略号和朱诺号飞船。这些飞船携带了大量的探测仪器,对木星大气的动力、物理和化学性质,磁层、电离层和内部结构等进行了综合探测。我们在本文中将主要集中在木星大气探测方面,对7次飞越探测做简要的介绍,对两次专门的探测进行详细介绍,并对一部分尚未解决的科学问题进行简单讨论。  相似文献   

与冬季北太平洋大范围海温异常相联系的海气特征          下载免费PDF全文

徐海明  崔梦雪 《大气科学学报》2018,41(3):330-343

采用1948—2014年NCEP/NCAR大气再分析资料以及延伸重建海温资料,基于大气海洋间不同的主导关系对冬季北太平洋大范围海温异常进行分类,探究其相应的海气结构特征。结果表明:1)大气影响海洋的个例多于海洋影响大气的个例,即在冬季北太平洋大气强迫海洋占主要地位,但也存在海洋对大气的反馈作用。2)对于大气影响海洋而言,SST(Sea Surface Temperature)暖异常区上空主要伴随着东北—西南走向的相当正压高低压异常(东北高西南低),对应东南风异常以及显著的深厚暖异常,表现出相当正压暖/脊结构,冷异常情况与此相反。SST异常为净热通量异常与风速异常共同作用引起。3)对于海洋影响大气而言,在SST暖异常区上空西部为南北向高低压异常(北高南低),东部为低压异常,对应偏东风异常。在SST冷异常区上空为偶极型的南北向高低压异常(南高北低),对应偏西风异常;位势高度异常表现出相当正压结构且较大气影响海洋时相对偏弱,大气暖(冷)温度异常比较浅薄且主要局限于对流层低层。4)海洋温度结构异常主要表现为,在大气影响海洋时海温异常由表层下传,海洋影响大气时为上下一致的温度异常。  相似文献   

白天工作条件下大气激光雷达探测的实验研究     

宋小全  刘智深  贺岩  刘金涛 《中国海洋大学学报(自然科学版)》2001,31(4):593-598

作者在已完成大气激光雷达系统夜间工作的基础上 ,对白天工作条件下的各种环境背景光的干扰进行了理论与实验分析 ,得出太阳直射光和天空光为白天工作的主要背景干扰。实验结果表明 ,经过激光发射与接收视场角严格匹配及使用干涉滤光器 (2 .6 nm和 0 .15nm)进行窄带滤波 ,背景干扰被明显地剔除 ,可进一步压低背景干扰约 2 0倍。证明采取视场匹配及干涉滤光器的措施可基本保证激光雷达系统在白天条件下工作。  相似文献   

南极中山站大气气溶胶的化学组成及其来源的判别   总被引：1，自引：1，他引：1  

黄自强  暨卫东  杨绪林  黄荣坦  汤荣坤  于涛  张功勋 《台湾海峡》2003,22(3):334-346

从1998年3月7日至1999年11月23日历时21个月，在南极中山站连续采集89个海洋气溶胶样品，本文提供全部样品的13种化学元素Cu、Pb、Zn、Cd、Fe、Al、Mn、Cr、V、K、Na、Ca、Mg含量的实测值．研究表明中山站气溶胶化学成份的含量具有季节性变化的特征．通过相关分析、因子分析、富集因子等方法判别不同时间段中山站气溶胶化学成份的来源。  相似文献   

Material exchange as heat engine for the corona-chromosphere transition region     

Ni Xiang-bin 《Chinese Astronomy and Astrophysics》1988,12(4):320-323

We think that a steady material exchange in the upper solar atmosphere can act as a heat engine that cools the corona and heats the corona-chromosphere transition region. We have considered heat conduction from the corona and radiation loss in the transition region and have calculated the temperature, density and velocity distributions in the transition region. Also discussed is the relation between the material flux, the velocity boundary value and the thickness of the transition region.  相似文献   

提高中性大气折射延迟改正精度的可能途径     

冒蔚  张捍卫  李彬华  杨磊  铁琼仙 《天文学报》2006,47(4):432-440

针对空间大地测量技术对中性大气折射延迟改正精度的要求,阐述了折射延迟改正值应随测站和随方位而异的必要性．指出,在尚不能直接测定天文大气折射值的情况下,现有的各种改正模型对大气分布模型的依赖性,不能达到预期的精度和降低观测的截止角．根据云南天文台低纬子午环的特殊结构,和测定大气折射的实践,提出了提高折射延迟改正精度的新方法,即：利用各观测站不同方位从天顶附近直到低地平高度角的天文大气折射实测数据,求解得到折射率差和映射函数的参数,从而建立随测站和随方位而异的大气折射延迟改正模型．这一新方法的实施,将能在不需采用大气分布模型的情况下,把天顶延迟的改正精度提高到1 mm以内,低地平高度角的折射延迟改正精度提高到厘米级,并且把截止高度角压缩到5°以内．  相似文献   

Seasonal surface frost at low latitudes on Mars     

Norbert Schorghofer  Kenneth S. Edgett 《Icarus》2006,180(2):321-334

During the past 4 Mars years, Mars Orbiter Camera imaging capabilities have been used to document occurrence of seasonal patches of frost at latitudes as low as 33° S, and even 24° S. Monitoring reveals bright patches on pole-facing slopes; these appear in early southern winter and disappear in mid winter. The frost forms annually. Thermal Emission Spectrometer and daytime Thermal Emission Imaging System observations show surface temperatures on and near pole facing slopes reach the condensation temperature of CO₂, indicating the patches consist of carbon dioxide rather than water frost. For several months, temperatures on pole-facing crater walls are so low that even carbon dioxide condenses on them, although the slopes are illuminated by the Sun every day. Thermal model calculations show slopes accumulate a several centimeter thick layer of CO₂ frost. The frost becomes visible only months after it has begun to form, and has an orientational preference which is due to illumination bias at the time of observation. H₂O condenses at higher temperatures and water frost must therefore also be present. Potential opportunities to observe seasonal water frost at low latitudes are also described.  相似文献   

Atmospheric entry profiles from the Mars Exploration Rovers Spirit and Opportunity     

Paul Withers  Michael D. Smith 《Icarus》2006,185(1):133-142

Accelerometer measurements made by Spirit and Opportunity during their entries through the martian atmosphere are reported. Vertical profiles of atmospheric density, pressure, and temperature with sub-km vertical resolution were obtained using these data between 10 and 100 km. Spirit's temperature profile is ∼10 K warmer than Opportunity's between 20 and 80 km. Unlike all other martian entry profiles, Spirit's temperature profile does not contain any large amplitude, long wavelength oscillations and is nearly isothermal below 30 km. Opportunity's temperature profile contains a strong inversion between 8 and 12 km. A moderate dust storm, which occurred on Mars shortly before these two atmospheric entries, may account for some of the differences between the two profiles. The poorly known angle of attack and unknown wind velocity may cause the temperature profiles to contain errors of tens of Kelvin at 10 km, but these errors would be an order of magnitude smaller above 30 km. On broad scales, the two profiles are consistent with Mars Global Surveyor Thermal Emission Spectrometer (TES) pressure/temperature profiles. Differences exist on smaller scales, particularly associated with the near-isothermal portion of Spirit's profile and the temperature inversion in Opportunity's profile.  相似文献   

On the Line Formation in Stellar Magnetized Atmospheres     

Zhong-Quan Qu  Xiao-Yu Zhang  Zhi Xu 《中国天文和天体物理学报》2001,1(2):161-175

1 INTRODUCTIONIn the previous paper (on et al. 1999, hereafter Paper I), we investigated the wavelength-dependence of four colltribution functions (CFs) derived from dmerent formal solutions andreferring to different emergellt quantities in the unpolarized case. Because one cannot generallyassign a single formation region to the whole line band in a real stellar atmosphere, e.g., the solaratmosphere, instead, the line formation region can be defined as the layers deviating farthestfrom t…  相似文献   

热带大气中30～60天低频振荡的CISK-Rossby波理论     

罗德海 《成都信息工程学院学报》1993,(4)

本文根据低纬热带大气中的风压场平衡关系对CISK-Rossby波进行了研究,指出对于弱对流加热,CISK-Rossby波既可以向东西方向传播,又可以向南北方向传播,并且这种弱对流加热所激发的CISK-Rossby波是一种稳定的减幅波;对于强对流加热,这种CISK-Rossby波减速并向东和向北传播,其传播特征与30～60天低频振荡的特征比较一致,并且这种CISK-Rossby波又是一种不稳定的增幅波,在10°N和17°N地区,经向波长为6000km的CISK-Rossby波的e倍增幅时间分别为6天和8天。因此,CISK-Rossby波可能是30～60天低频振荡的触发机制。  相似文献