美国“地球观测系统”卫星参数表

美国“地球观测系统”卫星参数见表１。表１　“地球观测系统”参数表卫星ＥＯＳ－ＡＭＥＯＳ－ＰＭＥＯＳ－ＣＯＬＯＲＥＯＳ－ＡＥＲＯＥＯＳ－ＡＬＴＥＯＳ－ＣＨＥＭ科学用途测量地表、云、气溶胶和辐射收支特性测量云、降水和辐射收支、地面雪和海冰、海面温度和海洋生产率研究海洋生物量和生产率观测大气和气溶胶测量海平面高度、洋流和冰层质量测量大气化学成分及其传输过程、海洋现象有效载荷ＡＳＴＥＲ，ＣＥＲＥＳ，ＭＯＤＩＳ，ＭＩＳＲ，ＭＯＰＩＴＴＡＩＲＳ／ＡＭＳＵ／ＭＨＳ，ＭＯＤＩＳ，ＣＥＲＥＳ，ＭＩＭＲＳｅａＷＩＦ…     

高层大气臭氧对于太阳紫外辐射27天波动的响应

本文利用Ｓｏｌａｒ Ｍｅｓｏｓｐｈｅｒｅ Ｅｘｐｌｏｒｅｒ（ＳＭＥ）卫星１９８２年和１９８３年太阳紫外辐射和赤道地区５０－９０ｋｍ臭氧分布的红外观测资料，对臭氧地太阳紫外辐射２７天振荡的响应进行了研究，并且利用大气光化波动模式对其进行了理论计算，计算结果与实测结果基本一致。     

空间扫描

印签订两项重要航天商业协议美《航空和空间技术周刊》２月１３日载文称，国际通信卫星组织（ＩＮＴＥＬＳＡＴ）已经与印度签订了第１个租借全部卫星转发器的协议。ＩＮＴＥＬＳＡＴ租下了印Ｉｎｓａｔ－ＺＥ卫星的１１个Ｃ波段转发器（该卫星将于１９９７年末搭乘俄质子号火箭进入东经８３的地球同步轨道）。印１０年内将收入１亿美元。印的另一项协议是和总部设在美国马里兰州拉纳姆的地球观测卫星公司（ＥＯＳＡＴ）签订的，印原则上已同意由ＥＯＳＡＴ在市场上销售１０颗印度遥感卫星拍摄的图像和收集的数据（印预计这１０颗遥感卫星将…     

新型星用导电型Kapton基热控材料

介绍了一种新型导电型Ｋａｐｔｏｎ基热控材料,其导电层采用了ＴＯ（氧化锡）膜。这种ＴＯ膜具有很高的光学透明度,方阻在１０＾４Ω￣１０＾６Ω范围内,可有效地抑制卫星表面的充放电现象。经过８２００ｈ太阳当量紫外辐照后,ＴＯ／Ｋａｐｔｏｎ／Ａｌ热控材料的αｓ相对变化率Δα３／α５仅为６．７％。在ＴＯ／Ｋａｐｔｏｎ与Ｋａｐｔｏｎ试样的８０００ｈ的紫外辐照对照实验中,表明ＴＯ膜具有明显的紫外辐射防护功能。在－     

综合信息

美国ＴＲＷ公司获得制造３颗国防支援计划（ＤＳＰ）卫星的合同这项与空军签订的合同价值７．２亿美元。ＤＳＰ卫星是装有红外遥感器的早期预警卫星，休斯公司与马来西亚签订制造马来西亚东亚卫星合同这颗ＭＩＳＡＴ（ＭａｌａｙｓｉａＥａｓｔＡｓｉａＳａｔｅｌｌｉｔｅ）卫星有１２台转发器，选用自旋型ＨＳ—３７６型公用舱或是用于巴西卫星的宽体型ＨＳ－３７６Ｗ型公用舱。制造和发射ＭＩＳＡＴ卫星的费用约为２．８亿美元（共制造２颗，１颗为备份星）。马来西亚已和阿里安空间公司签订了该卫星的发射合同。目前休斯公司正在生产３７…     

太阳紫外辐射对星上光学膜层的影响

光学遥感是当前卫星遥感的重要手段, 而卫星温控和能源系统也广泛采 用光学膜层, 它们在空间环境条件下的性能对卫星应用任务的完成, 乃至卫星寿命、安全将起着非常重要的作用. 本文给出了太阳紫外辐射对星上光学膜层影响的主要机制, 分析了这一影响的主要规律和原子氧剥蚀、高能粒子和静电场的作用, 综述了太阳紫外辐射对星上光学系统表面膜层影响的测量结果, 最后提出了星上光学膜层污染防护中应重点关注的几个方面.      

以太阳为射电源直接测量天线G／T

介绍以太阳为射电源,直接测量扩充后中国陆地卫星地面接收站,３个数据通道天线的Ｇ／Ｔ性能．对固定通道,测量了Ｌａｎｄｓａｔ—５下行频率的Ｇ／Ｔ～α（天线俯仰角）性能曲线;对可变通道,在α＝５°、３０°时,测量了Ｌａｎｄｓａｔ—６、ＪＥＲＳ—１、ＥＲＳ—１、ＳＰＯＴ卫星、ＺＹ—１卫星下行频率的Ｇ／Ｔ性能,以及可变通道的Ｇ／Ｔ～ｆ性能曲线,最后进行了误差分析．     

GOES—9将使美国天气预报能力进一步加强

１９９５年５月２３日，美国在卡纳维拉尔角发射了一颗新的静止气象卫星，这是美国为进一步加强其天气预报能力的又一新举措。这颗静止气象卫星是ＮＯＡＡ新一代地球静止环境业务气象卫星（ＧＯＥＳ－ＮＥＸＴ）系列中的第二颗，卫星入轨前叫ＧＯＥＳ－Ｊ，入轨后则按习惯改称ＧＯＥＳ－９。随着它的发射，美国将拥有一个具有先进技术的双星观测系统，从而大大增强了美国气象部门在追踪和预报美国本土及附近区域灾害性天气系统的能力。ＧＯＥＳ－ＮＥＸＴ系列由５颗共耗资１０亿美元的卫星组成，其中ＧＯＥＳ－９的造价为２．２亿美元。该系…     

欧空局环月观测器方案

为了填补欧洲在月球探测领域的空白，欧空局于今年１０月向其部长级会议提出了研制欧洲第一个月球探测器的建议。现将该探测器的方案简介如下。欧洲第一个月球探测器取名为“环月观测器”（ＭＯＲＯ——ＭｏｏｎＯｒｂｉｔｉｎｇＯｂｓｅｒ－ｖａｔｏｒｙ）。它实际上是一个月球极轨卫星，其任务是对月面进行遥感观测，对全月球进行月貌和重力场测量，为研究月球的形成、演化和未来提供科学数据。ＭＯＲＯ将携带４种科学探测仪器和１颗微型子卫星。４种仪器是：·月球立体相机（ＬＵＳＴＥＣ）·月球紫外／可见光／红外绘图光谱计（ＬＵＶＩ…     

日环境观测技术卫星搭载用的探测器

日本环境观测技术卫星（ＡＰＥＯＳ－２），是对其地球观测平台技术卫星（ＡＤＥＯＳ）大面积观测技术的进一步发展，作为人类共同关心的地球环境问题，日本拟从弄清全球规模的水、能量循环的机理入手，通过ＡＤＥＯＳ－２卫星获得大量珍贵的地球科学数据。该卫星拟于１９９８年用Ｈ－２火箭发射。为达到上述目标，ＡＤＥＯＳ－２卫星上应该搭载能提供下列数据集的探测器，其中最为核心的探测器有高性能微波扫描辐射计（ＡＭＳＲ）和全球成像器（ＧＬＩ），此外，还搭载其它机构的探测器，如环境厅的改进型大气边缘红外分光计（ＩＬＡＳ－２…     

Active region properties and irradiance variations

Total Solar Irradiance (TSI) has been measured for more than three decades. These observations demonstrate that total irradiance changes on time scales ranging from minutes to years and decades. Considerable efforts have been made to understand the physical origin of irradiance variations and to model the observed changes using measures of sunspots and faculae. In this paper, we study the short-term variations in TSI during the declining portion and minimum of solar cycle 22 and the rising portion of cycle 23 (1993–1998). This time interval of low solar activity allows us to study the effect of individual sunspot groups on TSI in detail. In this paper, we indicate that the effect of sunspot groups on total irradiance may depend on their type in the Zürich classification system and/or their evolution, and on their magnetic configuration. Some uncertainties in the data and other effects are also discussed.     

Two successive partial mini-filament confined ejections

Active region (AR) NOAA 11476 produced a series of confined plasma ejections, mostly accompanied by flares of X-ray class M, from 08 to 10 May 2012. The structure and evolution of the confined ejections resemble that of EUV surges; however, their origin is associated to the destabilization and eruption of a mini-filament, which lay along the photospheric inversion line (PIL) of a large rotating bipole. Our analysis indicate that the bipole rotation and flux cancellation along the PIL have a main role in destabilizing the structure and triggering the ejections. The observed bipole emerged within the main following AR polarity. Previous studies have analyzed and discussed in detail two events of this series in which the mini-filament erupted as a whole, one at 12:23 UT on 09 May and the other at 04:18 UT on 10 May. In this article we present the observations of the confined eruption and M4.1 flare on 09 May 2012 at 21:01 UT (SOL2012-05-09T21:01:00) and the previous activity in which the mini-filament was involved. For the analysis we use data in multiple wavelengths (UV, EUV, X-rays, and magnetograms) from space instruments. In this particular case, the mini-filament is seen to erupt in two different sections. The northern section erupted accompanied by a C1.6 flare and the southern section did it in association with the M4.1 flare. The global structure and direction of both confined ejections and the location of a far flare kernel, to where the plasma is seen to flow, suggest that both ejections and flares follow a similar underlying mechanism.     

Chromospheric dynamics

This review focuses on dynamics of the solar chromosphere, which serves as a good proxy for understanding processes in stellar chromospheres as well. In the quiet chromosphere it is useful to distinguish between the magnetic network on the boundaries of supergranulation cells, where strong magnetic fields are organized in mainly vertical magnetic flux tubes, and internetwork regions in the cell interior, where magnetic fields are weaker and dynamically less important. Recently, some progress has been made in understanding the physics of the non-magnetic chromosphere. On the other hand, the physical processes that heat the magnetic network have not been fully identified. Is the network heated by wave dissipation and if so, what are their physical characteristics? These and other aspects relating to the dynamics and energy transport mechanisms will be discussed in detail. In addition, some of the outstanding problems in the field such the driving mechanism for spicules and the nature of internetwork magnetic fields will also be highlighted. Furthermore, a critical assessment will be made on the challenges facing theory and the direction for future investigations, particularly in the light of the new space experiments, will be highlighted.     

Results of solar observations by the CORONAS-F payload

The CORONAS-F mission experiments and results have been reviewed. The observations with the DIFOS multi-channel photometer in a broad spectral range from 350 to 1500 nm have revealed the dependence of the relative amplitudes of p-modes of the global solar oscillations on the wavelength that agrees perfectly well with the earlier data obtained in a narrower spectral ranges. The SPIRIT EUV observations have enabled the study of various manifestations of solar activity and high-temperature events on the Sun. The data from the X-ray spectrometer RESIK, gamma spectrometer HELICON, flare spectrometer IRIS, amplitude–temporal spectrometer AVS-F, and X-ray spectrometer RPS-1 have been used to analyze the X- and gamma-ray emission from solar flares and for diagnostics of the flaring plasma. The absolute and relative content of various elements (such as potassium, argon, and sulfur) of solar plasma in flares has been determined for the first time with the X-ray spectrometer RESIK. The Solar Cosmic Ray Complex monitored the solar flare effects in the Earth’s environment. The UV emission variations recorded during solar flares in the vicinity of the 120-nm wavelength have been analyzed and the amplitude of relative variations has been determined.     

A spectroscopic measurement of high velocity spray plasma from an M-class flare and coronal mass ejection

The M1.5-class flare and associated coronal mass ejection (CME) of 16 February 2011 was observed with the Extreme ultraviolet Imaging Spectrometer on board the Hinode spacecraft. Spray plasma associated with the CME is found to exhibit a Doppler blue-shift of 850 km s^?1 – one of the largest values reported from spectroscopy of the solar disk and inner corona. The observation is unusual in that the emission line (Fe xii 193.51 Å) is not observed directly, but the Doppler shift is so large that the blue-shifted component appears in a wavelength window at 192.82 Å, intended to observe lines of O v, Fe xi and Ca xvii. The Fe xii 195.12 Å emission line is used as a proxy for the rest component of 193.51 Å. The observation highlights the risks of using narrow wavelength windows for spectrometer observations when observing highly-dynamic solar phenomena. The consequences of large Doppler shifts for ultraviolet solar spectrometers, including the upcoming Multi-slit Solar Explorer (MUSE) mission, are discussed.     

一个基于观测的太阳风背景模型

建立由太阳光球磁场和日冕偏振亮度等观测约束的单流体太阳风模型,包括日冕和太阳风的等离子体密度、速度和磁场,温度还有待于以后处理.这里采用高山观测台(HAO)MKⅢ的日冕偏振亮度(pB)在1.36Rs上的观测概图,根据Guhathakurta在1996年发展的日冕电子密度反演模型确定日冕的电子密度分布.同时采用Wilcox太阳观测台(WSO)的光球磁场视向分量的观测概图作为底部边界,根据Zhao等在1994年发展的水平电流-电流片(HCCS)模型得到全球磁场.Phillips在1995年及McComas在2003年分别用Ulysses第一次和第二次跨极飞行的观测发现,归一化到1 AU的太阳风动量流密度除了在10°～30°的纬度范围内略低以外几乎不变.根据这一结论,结合已经得到的密度数据,就可以得到日冕和太阳风的速度.将上面的模型应用于1918卡林顿自转周稳态太阳风的研究,结果与太阳活动极小期的观测基本相符,但是与观测相比较低速高密度区偏大,因此密度模型还有待改进.      

Coronal spectroscopy: Probing sources of slow solar wind in active regions,and the early phases of solar flares

Coronal spectroscopy has pushed forward the understanding of physical processes in all phenomena on the Sun. In this review we concentrate specifically on plasma parameters measured in sources of the slow solar wind in active regions and the early phases of solar flares. These topics are a key part of the science goals of the Solar Orbiter mission (Müller et al., 2020) which has been designed to probe what drives the solar wind and solar transients that fill the heliosphere.Active regions, outside of flaring, have general characteristics that include closed loops showing red-shifted (down-flowing plasma), and the edges of the active regions showing blue-shifted (upflowing plasma). Constraining and understanding the evolution, behaviour and cause of the flows has been developed in the past years and are summarised. Of particular importance is the upflowing plasma which, in some cases, can contribute to the slow solar wind, and this review concentrates on recent results on this topic.The early phases of solar flares and their energy sources are not yet fully understood. For decades, there has been a huge interest in pin-pointing the trigger of a solar flare. Coronal spectroscopy has revealed small-scale dynamics that occurs tens of minutes before the flare begins. The understanding of the trigger is key to improving flare predictions in the future, as well as understanding the physical processes.Finally we look to the future of coronal spectroscopy, with new instruments and methodologies being developed that build on the current knowledge, and will improve significantly our physical understanding of processes at all scales on the Sun.