2010年的欧洲航天活动

欧洲在2010年开展了较多的航天活动,其中有不少技术先进的新型航天器,例如,冷卫星-2（CryoSa-2）、“陆地合成孔径雷达-X附加数字高程测量”（TanDEM—X）雷达成像卫星、宁静号节点舱-3（Tranquility Node3）、隙望塔号（Cupola）观测舱和“欧洲机械臂”（ERA）等重要航天器都顺利上天,只有新发射的欧洲通信卫星公司的W3B通信卫星因故障而失效,令人遗憾。     

宇宙神-3运载火箭首射成功

20 0 0年 5月 2 4日 ,采用俄罗斯发动机的美国新型运载火箭宇宙神 - 3A首次发射获得了成功 ,并把 1颗名叫 W4的欧洲通信卫星送入轨道 ,因而引起广泛关注。1　宇宙神 - 3系列运载火箭1995年 ,洛马公司宣布研制宇宙神 - 3新型运载火箭 (原来称为宇宙神 - 2 AR,R代表重新设计 )。宇宙神 - 3运载火箭采用了成熟的技术 ,具有可靠性高、成本低的特点。它是洛马公司改进现有运载火箭 ,以形成采用公共模块 (包括公共助推级 )建造新型火箭系列的重要的一步。这次发射的是宇宙神 - 3A,此后 ,洛马公司还将推出宇宙神 - 3B运载火箭。宇宙神 - 3B将采…     

TIMED/SABER与AURA/MLS临近空间探测温度数据比较

利用AURA/MLS数据（V4.2）和TIMED/SABER数据（V2.0）对20~92km高度的大气温度进行比较分析,计算AURA/MLS数据与TIMED/SABER数据的温度绝对偏差,并分析平均温度偏差在不同季节中随经度、纬度和高度的变化特征.结果表明:20~80km高度的平均温度偏差在±6K以内,相对偏差在3%以内;80~90km高度平均温度偏差减小至-10K以下,相对偏差在9%以内.中低纬度地区平均温度偏差廓线的变化趋势一致,从20km高度的-3K左右的负偏差逐渐增加,在45~50km高度的平流层顶处有较明显的3K左右的正偏差峰值.平均温度偏差随纬度变化明显,随经度变化很小.研究结果可为卫星数据的应用提供参考依据.      

单向电永磁作动器结构优化与动态特性分析

针对电磁作动器的使用要求,设计出一种具有能耗低、吸力大及响应快等特点的新型单向电永磁作动器。结合有限元仿真软件,利用有限元法研究作动器的结构参数如铁芯齿形结构、平面结构、无永磁结构、铁芯的倾斜角度及衔铁位移（气隙厚度）等因素对作动器电磁吸力和响应速度的影响。结果表明,电磁吸力随着作动衔铁位移的增加而大幅度减小;倾角结构的铁芯设计能使作动器性能达到最佳,且铁芯的倾斜角度为50°时,电磁吸力有最大值3071N。     

2011年世界航天活动计划

1月20日,天顶-3F火箭发射了俄罗斯的电子-1（Elektro—L1）气象卫星。该卫星的质量约为1620kg（其中有效载荷质量为435kg）,设计寿命为10年。     

50MHz低噪声压控温补晶振的研制

介绍50 MHz低噪声压控温补晶振的研制,它采用基频25 MHz AT切基频石英谐振器,二次倍频实现50 MHz双路隔离输出;压控范围达±11?0-6;桥式温补网络,在-40℃～70℃范围内可达到±1.4?0-6的频率稳定性;静态相位噪声可达到(1 kHz)-145 dBc,σy(0.1 s)的频率稳定性优于3?0-11;50 mm?0 mm?0 mm的小型结构,双路输出隔离良好;只有12 mA功耗;年老化可达1.2?0-6;在总均方根加速度6 g随机振动下,频率稳定性可达σy(0.1 s)5?0-10。并给出晶振电气性能测试数据。     

铜颗粒污染物对变压器油运动黏度的影响

变压器油中铜颗粒污染物的存在极易影响油液的理化性能,甚至导致重大生产事故,因而根据ISO4406:1999标准,配制了24组不同污染度的含铜颗粒油样并通过实验测试了变压器油样的运动黏度性能（40℃）,获得了实验范围内铜颗粒污染度对油液运动黏度的影响规律;然后根据测试数据采用偏最小二乘（PLS）法和支持向量机（SVM）法建立了油样中不同粒径、含量的铜颗粒与油液运动黏度的数学模型,探讨了不同粒径、含量的铜颗粒污染物对油液运动黏度的影响规律。结果表明:随着铜颗粒污染度的增加,油液的运动黏度减小;铜颗粒污染物粒径在15～25 μm范围内对油液运动黏度的影响较大,且粒径越大,油液运动黏度也越大;所建立SVM模型对验证集进行预测的相关系数和均方根误差（RMSE）分别是0.962 6、4.597×10-5。为消除实验误差,减少人为因素的影响比较准确地掌握铜颗粒污染物对油液运动黏度的影响提供了新的途径。      

1MΩ～100GΩ高值电阻器高精度的校准方法CSCD

高阻计、数字源表等仪器在半导体行业有着广泛的应用. 但目前市场上1MΩ-100GΩ高值电阻器准确度（±1. 0x10-3 -±1. 0x10-2）无法满足高阻计、数字源表等仪器电阻参数的溯源需求. 本文提出了一种高精度的高值电阻器的校准方法,该方法由两个多功能校准源和指零仪组成的比较电桥实现. 根据校准方法组建了1MΩ-100GΩ测量系统,测量结果的不确定度为3. 0x10-5 -8. 0x10-4,可满足市场上绝大部分高阻测量仪器的校准需求.     

子午工程首次火箭探空数据准单色惯性重力波特性分析

利用2010年6月3日子午工程首次气象火箭探测的温度和风场数据,采用矢端曲线法分别从平流层（20~50km）和对流层（0~15km）廓线提取了海南火箭发射场上空准单色惯性重力波参数.火箭探测的平流层和对流层两个准单色惯性重力波分别向上和向下逆风传播,固有周期为20.1h和22.4h,垂直波长为9.5km和4.0km,水平波长为2900km和753km,垂直群速度c_gz为0.0887m·-1和0.0298m·-1,水平群速度c_gh为12.7m·-1和3.65m·-1,λ_h/λ_z为305:1和188:1,c_gh/c_gz为143:1和122:1.      

Preliminary evaluation of soil moisture probe for use with Arcillite.

There is a need for reliable methods of measuring the level and distribution of water in the solid substrates that are used for growing plants in space. In a microgravity environment, water distribution is governed generally by capillary forces. Arcillite is the solid substrate used in the ASTROCULTURE (TM) system which was developed for growing plants in space. The goal of this study is to evaluate the applicability of heat pulse moisture sensors for measuring moisture levels in Arcillite. The ASTROCULTURE system uses suction as a means of controlling the moisture level in Arcillite, but the spatial distribution of the moisture is left unknown. Studies of the moisture content in a cell experiment were conducted to calibrate a heat pulse moisture sensor and then the sensor was used in a suction experiment to verify moisture content and distribution. Results of the studies demonstrate that head pulse moisture sensors can be used to monitor moisture content and distribution within the root module of the ASTROCULTURE system.     

Study of the 28 October 2003 and 20 January 2005 solar flares by means of 2.223 MeV gamma-emission line

By the data on intensity-time profiles of the neutron capture line of 2.223 MeV we have studied some characteristics of two solar flares, 28 October 2003 and 20 January 2005 (INTEGRAL and CORONAS-F observations, respectively). The SINP code was applied making allowance for the main processes of neutron interactions and deceleration in the solar plasma, character of neutron source, losses of neutrons and density model of the solar atmosphere. Comparison of the computed time profiles of 2.223 MeV line with observed ones for the flare of 28 October 2003 confirms the results obtained earlier for three other flares. Namely, the effect of density enhancement (EDE) in the sub-flare region, as well as the variations (hardening) of accelerated particle spectrum in the course of the event have been confirmed. The usual modeling procedure by the SINP code, however, seems to be inapplicable to the event of 20 January 2005. Possible causes of density enhancements during some flares and peculiarities of the 20 January 2005 flare are discussed.     

Ozone trends in the mid-latitude stratopause region based on microwave measurements at Lindau (51.66° N, 10.13° E), the ozone reference model,and model calculations

We compared 8 years of ozone measurements taken at Lindau (51.66° N, 10.13° E) at altitudes between 40 and 60 km using the microwave technique with the CIRA ozone reference model that was established 20 years ago (Keating et al., 1990). We observed a remarkable decrease in ozone density in the stratopause region (i.e., an altitude of 50 km), but the decrease in ozone density in the middle mesosphere (i.e., up to 60 km in altitude) is slight. Likewise, we observed only a moderate decrease in the atmospheric region below the stratopause. Other studies have found the strongest ozone decrease at 40 km and a more moderate decrease at 50 km, which is somewhat in contradiction to our results. This decrease in ozone density also strongly depends on the season. Similar results showed model calculations using the GCM COMMA-IAP when considering the increase in methane. In the lower mesosphere/stratopause region, the strongest impact on the concentration of odd oxygen (i.e., O₃ and O) was observed due to a catalytic cycle that destroys odd oxygen, including atomic oxygen and hydrogen radicals. The hydrogen radicals mainly result from an increase in water vapor with the growing anthropogenic release of methane. The finding suggesting that the stratopause region is apparently attacked more strongly by the water vapor increase has been interpreted in terms of the action of this catalytic cycle, which is most effective near the stratopause and amplified by a positive feedback between the ozone column density and the ozone dissociation rate, thereby chemically influencing the ozone density. However, the rising carbon dioxide concentration cools the middle atmosphere, thereby damping the ozone decline by hydrogen radicals.     

Modeling of the very high velocity impact process with respect to in-situ ionization measurements

This overview deals with very high impact velocities, where complete vaporization of an impacting cosmic dust particle is to be expected upon expansion from the high pressure high temperature state behind the stopping shock (v > 15 km/s). The topics discussed are the mechanics and thermodynamics of compression, adiabatic release, equation of state and nonequilibrium states upon expansion. The case of very high particle porosity (ρ 1 g/cm³) and the case of very small dust masses (m < 10⁻¹⁷ g) are discussed from what one presently knows. The possibility of three body collisions in the expanding gas phase is discussed briefly. The effect of oblique impact is discussed with respect to its relevance to the ionization process. The numbers communicated are up to the highest “experimental” impact velocities (80 km/s, Halley mission). As one goes to lower impact velocities (20 < v < 30 km/s) there is still complete vaporization of the dust particle but ionization out of the bulk of the particle becomes low. Other than thermal processes may become important. Ideas are outlined to understand their physical nature.     

Midday bottomside electron density profiles during moderate solar activity and comparison with IRI-2001

Bottomside electron density (Ne-h) profiles during midday (10–14 h) are analyzed using modern digital ionosonde observations at a low-middle latitude station, New Delhi (28.6N, 77.2E, dip 42.4N), for the period from January 2003 to December 2003, pertaining to moderate solar activity (MSA). Each individual profile is normalized with respect to the peak height and density (hmF2, NmF2) of the F2-region. These profiles are compared with those obtained from the International Reference Ionosphere (IRI-2001) model. Bilitza [Bilitza, D. International Reference Ionosphere 2000. Radio Sci. 36 (2), 261–275, 2001] using both the options namely: Gulyaeva’s model [Gulyaeva, T.L. Progress in ionospheric informatics based on electron density profile analysis of ionograms. Adv. Space Res. 7 (6) 39–48, 1987] and B0 Tab. option [Bilitza, D., Radicella, S.M., Reinisch, B.W., Adeniyi, J.O., Mosert Gonzalez, M.E., Zhang, S.R., Obrou, O. New B0 and B1 models for IRI. Adv. Space Res. 25 (1), 89–95, 2000]. The study reveals that during summer and equinox, the IRI model with B0 Tab. option in general, produces better agreement with the observed median profiles, while the IRI predictions using Gulyaeva’s option, overestimate the electron density distribution at all the heights below the F2-peak. However, during winter, in general, the IRI model, using both the options, reveals shows fairly good agreement with the observations.     

RAMAN SPECTRA OF SEVEN INTERPLANETARY DUST PARTICLES

The Raman Shift Spectra of seven interplanetary dust particles,U2034 (F10),U2034(F8),U2022(B1),W7074 18,W7074 C15,W7074 C3 and W7074 A7,were measured with a Spex-1403 Raman Spectrograph.The exciting radiations were the 488 nm and 514 nm line of a 5W argon ion laser.All seven spectra exhibit the 1350 and 1600 Acm-1 arbon bands,implying that the IDPS were coated with hydrocarbon and incompletely crystallized carbon,the part of which may be the residue of hydro-carbon contents in the particles after water loss by the heating during their entry into the earth's atmosphere.A weak band structure in the 520-610 cm-1 range could be caused by cyclosilicates,and a weak band at 2900 cm-1 is tentatively identified as due to hydrocarbon molicules.     

在片校准标准件基底边界条件影响

通过分析国内外校准标准件物理边界条件,研究不同校准基底的物理边界条件对共面波导（CPW）传输线特性和校准准确度的影响。研制了W波段砷化镓衬底的多线TRL在片校准标准件,将在片校准标准件分别放置在金属卡盘、玻璃片、吸波材料三种校准基底上。用三种不同校准基底的校准标准件对试验装置校准后,分别提取了CPW传输线的衰减常数、相对介电常数和特征阻抗,并对商用校准标准件104-783A的短路标准和传输线标准进行了测试,验证了结果的合理性。     

强磁暴、能量粒子暴与热层大气密度涨落之间的相关关系

利用1997-2007年由GOES8, GOES11和GOES12星载高能粒子探测器在地球同步轨道高度上所探测到的高能质子和高能电子通量探测数据以及高度560km左右星载大气密度探测器所得的热层大气密度探测数据, 统计分析了强地磁扰动、高能粒子通量跃变和热层大气密度涨落之间的相关关系, 初步获得强地磁扰动期间, 地球同步轨道(外辐射带外环)均出现了增幅大于三个数量级的高能质子通量(尤其是E>1MeV)强增强现象, 随后热 层大气密度强烈上涨, 表明三者之间是正相关关系. 在时间上地球同步轨道高能质子通量强增强现象先于日均Ap值(地磁活动程度)上涨约一天左右, 而热层大气密度强涨落现象又明显滞后于强地磁扰动事件.      

Penetration testing for the Optical Probe for Regolith Analysis (OPRA)

The Optical Probe for Regolith Analysis (OPRA) is a spike-shaped subsurface analytical probe that will be delivered to a planet, asteroid, or cometary body by a lander and/or rover. OPRA will be pushed down into the subsurface to record near infrared spectra as a function of depth down to maximum of 50 cm. Therefore, knowledge of the required penetration force to specific depths can be helpful in estimating the length of the probe. Test probes covering the anticipated diameter (2.5, 1.9, 1.2 and 0.9 cm diameter) and tip angle (T.A. = 30°, 60°, 90° and 120°) of OPRA were inserted mechanically into dry playground sand. The results showed that tip angle does not have a major effect, while probe diameter and density of the regolith are the most important parameters. Increasing probe diameter from 0.9 to 1.9 cm (i.e. a factor of 2) leads to an increase in penetration force from 200 to 1000 N (i.e. a factor of 5) at 20 cm depth. An increase in bulk density (B.D.) from 1550 to 1700 kg m⁻³ leads to an increase in penetration force from 10 to 200 N at 20 cm depth. Bearing capacity theory was used to explain the downward movement of the penetrometer through regolith and showed good agreement with the experimental results. This model was then used to take into account the effect of gravity on other planetary bodies. We observed a good agreement between the theoretical model and results from penetration testings on the Moon by the Apollo missions. Since the maximum allowed force for penetration is the weight of the lander/rover on their targeted planetary surface, our results put a strong constraint on the maximum reachable depth without endangering the whole mission.     

以太阳风为源水分子在月球空间环境中的分布特征

近年来,越来越多的观测结果均显示月球上存在水.本文通过运用Monte-Carlo方法及基于能量守恒的有心力场中粒子轨道算法对水分子在近月表的输运过程进行建模,得到了水分子在近月表分布随时间演化的图像.模拟结果显示,分布在高纬地区的水分子较同经度的中低纬地区要多,这与目前探测得到的结论是一致的.同时,对最终进入永久阴影区的水分子的百分比进行了统计,在光解离常数为6.4×104s的情况下,有大约4.12%的水分子会被永久阴影区存储下来,这个比例与前人估算结果相吻合.