Venus Atmospheric Thermal Structure and Radiative Balance

From the discovery that Venus has an atmosphere during the 1761 transit by M. Lomonosov to the current exploration of the planet by the Akatsuki orbiter, we continue to learn about the planet’s extreme climate and weather. This chapter attempts to provide a comprehensive but by no means exhaustive review of the results of the atmospheric thermal structure and radiative balance since the earlier works published in Venus and Venus II books from recent spacecraft and Earth based investigations and summarizes the gaps in our current knowledge. There have been no in-situ measurements of the deep Venus atmosphere since the flights of the two VeGa balloons and landers in 1985 (Sagdeev et al., Science 231:1411–1414, 1986). Thus, most of the new information about the atmospheric thermal structure has come from different remote sensing (Earth based and spacecraft) techniques using occultations (solar infrared, stellar ultraviolet and orbiter radio occultations), spectroscopy and microwave, short wave and thermal infrared emissions. The results are restricted to altitudes higher than about 40 km, except for one investigation of the near surface static stability inferred by Meadows and Crisp (J. Geophys. Res. 101:4595–4622, 1996) from 1 \(\upmu\)m observations from Earth. Little information about the lower atmospheric structure is possible below about 40 km altitude from radio occultations due to large bending angles. The gaps in our knowledge include spectral albedo variations over time, vertical variation of the bulk composition of the atmosphere (mean molecular weight), the identity, properties and abundances of absorbers of incident solar radiation in the clouds. The causes of opacity variations in the nightside cloud cover and vertical gradients in the deep atmosphere bulk composition and its impact on static stability are also in need of critical studies. The knowledge gaps and questions about Venus and its atmosphere provide the incentive for obtaining the necessary measurements to understand the planet, which can provide some clues to learn about terrestrial exoplanets.     

Accuracy of Star Occultation Measurements for Satellite Navigation

To determine the orbital parameters of a satellite using star occultations, it is necessary to measure the intensity of stars as they occult. The accuracy of the intensity measurements is reduced by interfering sources of light and internal noise, and is expressed in terms of the magnitude of various sources of interference. Subsequently, a specific system is analyzed in detail. Moonlit cloud tops introduce the largest systematic error. Photon noise from the star radiation, airglow, and moonlit cloud tops are the largest sources of random errors.     

The helium abundance on Jupiter

Methods of determining helium on Jupiter (and the Jovian planets) are critically surveyed. Current information is consistent with solar abundance, He/H₂ = 0.11 by number. The available lines of evidence are the mean density, spectral-line broadening, and stellar occultations. Methods usable from spacecraft flying by are discussed. Observation of far-infrared emission has great promise, but we may have to await the development of entry probes for the greatest assurance.This is one of the publications by the Science Advisory Group.     

The Cassini Ultraviolet Imaging Spectrograph Investigation

The Cassini Ultraviolet Imaging Spectrograph (UVIS) is part of the remote sensing payload of the Cassini orbiter spacecraft. UVIS has two spectrographic channels that provide images and spectra covering the ranges from 56 to 118 nm and 110 to 190 nm. A third optical path with a solar blind CsI photocathode is used for high signal-to-noise-ratio stellar occultations by rings and atmospheres. A separate Hydrogen Deuterium Absorption Cell measures the relative abundance of deuterium and hydrogen from their Lyman-α emission. The UVIS science objectives include investigation of the chemistry, aerosols, clouds, and energy balance of the Titan and Saturn atmospheres; neutrals in the Saturn magnetosphere; the deuterium-to-hydrogen (D/H) ratio for Titan and Saturn; icy satellite surface properties; and the structure and evolution of Saturn’s rings.This revised version was published online in July 2005 with a corrected cover date.     

The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) on the New Horizons Mission

The Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) comprises the hardware and accompanying science investigation on the New Horizons spacecraft to measure pick-up ions from Pluto’s outgassing atmosphere. To the extent that Pluto retains its characteristics similar to those of a “heavy comet” as detected in stellar occultations since the early 1980s, these measurements will characterize the neutral atmosphere of Pluto while providing a consistency check on the atmospheric escape rate at the encounter epoch with that deduced from the atmospheric structure at lower altitudes by the ALICE, REX, and SWAP experiments on New Horizons. In addition, PEPSSI will characterize any extended ionosphere and solar wind interaction while also characterizing the energetic particle environment of Pluto, Charon, and their associated system. First proposed for development for the Pluto Express mission in September 1993, what became the PEPSSI instrument went through a number of development stages to meet the requirements of such an instrument for a mission to Pluto while minimizing the required spacecraft resources. The PEPSSI instrument provides for measurements of ions (with compositional information) and electrons from 10 s of keV to ～1 MeV in a 160°×12° fan-shaped beam in six sectors for 1.5 kg and ～2.5 W.     

Self-similar neutrino heat waves

Transport of energy and lepton charge by neutrino radiation in a uniform medium is investigated within neutrino-thermoconductivity approximation — as a neutrino heat wave. The process is described by a self-similar solution. The problem applies primarily to the cooling of young neutron stars.     

The Medium Energy Instrument on Exosat

The Medium Energy Instrument on EXOSAT, although conceived as the main instrument for occultations, has been made sufficiently versatile to provide a significant advance over previous large area proportional counters when used for individual source studies of timing and spectra. The energy range is 1.2 to 50 keV, with E/E of 0.2 at 6 keV, sufficient to detect iron lines. The effective area of 1800 cm² and narrow field of view (3/4° × 3/4°) make it suitable for the detailed study of sources down to the 0.3 mCrab confusion limit. The unique facility provided by EXOSAT, allowing uninterrupted observations of X-ray sources for periods of up to 80 hours, backed up by a high capacity data link and on-board processing, enables timing studies to be performed over the range from milliseconds to days. Sophisticated background discrimination techniques giving a rejection efficiency of99% will control the background count rate to a suitably low value in the environment of the 200,000 km orbit.     

三体系统中引力拖车的偏置非开普勒轨道研究

为了研究太阳-小行星-引力拖车三体系统中引力拖车的轨道运动问题,采用柱坐标系下的Hill方程描述了三体系统中引力拖车的运动情况,应用平均化方法消除周期项的影响,得到平均偏置非开普勒轨道的表达式,并研究了轨道稳定性与引力拖车最大有效拉力等问题.研究表明:三体系统中,在小行星飞行方向（或反方向）上存在偏置非开普勒轨道;与二...     

Photometric effects of accretion disks in long-period eclipsing binaries

Summary A multi-year photometric program on long-period eclipsing binaries has begun to uncover some properties of accretion disks in these systems. Emission and transmission properties can sometimes be found from light curve features produced by partial eclipses of the disk by the cool star, and by partial occultations of the cool star by the disk. These disks do not have the classical alpha structure. They are optically thin normal to the orbital plane, but may be geometrically thicker than purely gravitationally-stratified disks. Disk gas may be contaminated by dust particles acquired from the outer layers of the cool loser. In some systems, high states, produced by elevated mass accretion by the hot star, occur, suggesting that the mass distribution in the disk is clumpy. However mass-transfer rates are found, they lie between 10^-7 and 10^-6 solar masses per year.While this binary sample is small at the moment, some of its properties are shared with other systems. The author has five-color observations of about a dozen additional systems, which may fill out this picture more fully.     

球形重力场下的视线动力学方程

以交会对接问题为背景,建立了球形重力场下的视线动力学方程,其简化形式可以描述平面重力场下的相对运动。该方程直接描述了视线参数和机动策略之间的关系,可广泛应用于相对运动问题的机动策略研究。     

某型飞机翼身主交点框下部疲劳寿命试验

介绍了某型飞机翼身主交点框下部疲劳寿命的试验方法及其结果, 还介绍了考虑预加高载对结构疲劳寿命影响的元件疲劳寿命试验。文章指出, 随着飞机使用范围的扩大, 环境影响引起的材料腐蚀损伤已成为飞机机体结构的致命杀手。在主交点框下部发生的环境腐蚀疲劳裂纹问题就是一个实例, 必须引起飞机总设计师和广大设计人员的重视。     

Orbital maneuver strategy design based on piecewise linear optimization for spacecraft soft landing on irregular asteroids

Recently, asteroid exploration becomes an important branch of human’s deep space activities. In this paper, a piecewise linear optimal orbital maneuver strategy is designed for a spacecraft soft landing on irregular-shaped asteroids. First, the space around an irregular asteroid is converted into several grid units, and the gravitational field of the asteroid is linearly fitted in each unit. Then, the soft-landing orbital maneuver strategy design problem is formulated as a piecewise linear optimal problem, and further transferred into a family of two-point boundary value problems, which can be solved using collocation method. Finally, a corresponding algorithm is developed to obtain the piecewise linear optimal maneuver strategy, which is proved to be able to achieve the soft-landing mission well. Simulation results show that the error of the model linearization is small enough, while the calculation efficiency is remarkably improved, and the robustness of maneuver strategy is also improved.     

后掠激波边界层干扰的有利影响

本文分析和对比了正激波和后掠激波/边界层干扰的机理,并用几个典型的算例说明了其差别.本文的结果指出,由于后掠的压力梯度方向垂直于激波,并且边界层内速度存在平行于激波的横向分量,会导致边界层内的速度分布形成空间"扭曲",可以阻止部分边界层进入激波后,并使穿过激波的部分边界层气流形成向两侧发散的趋势.这证明利用后掠激波/边界层干扰效应控制边界层是可行的.这也是实现近年来国内外兴起的"无隔道进气道"的关键机理之一.     

用螺桨-吊舱相关法设计和分析桨扇

本文用螺桨-吊舱相关分析法对桨扇进行设计和分析。用曲线升力线代表桨叶,并且考虑吊舱存在的影响;方法采用尾迹位于流面上的假定。对叶尖段进行跨音修正,对根部应用叶栅最佳损失攻角加以考虑。设计和分析的结果与文献〔2〕的计算和试验结果作部分比较,证明了本法的合理性和有效性,可以应用于桨扇的初步设计和性能分析中。     

基于改进引力搜索算法的认知无线网络频谱分配

为了提高认知无线网络频谱资源利用率,提出一种基于改进引力搜索算法的频谱分配方案。该方案 将质子位置信息映射为频谱分配变量,提出一种非线性引力衰减因子,以增强算法对于频谱分配可行解的搜索 能力。其次,为了保持算法对于频谱分配可行解的最优搜索方向,采用全局最优引导策略为质子增加记忆能力。 然后,提出动态高斯扰动策略,随着算法迭代自适应地调整扰动步长,避免算法陷入局部最优。最后,针对频 谱分配问题的离散化特性,引入Sigmoid 函数使质子的位置离散化。仿真实验结果表明,改进引力搜索算法能 够有效地实现频谱分配问题的优化求解,取得了相对较高的网络效益和用户公平度。     

航天领域蒸汽压缩热泵技术研究进展

蒸汽压缩热泵是未来大型航天器热控系统和制冷设备的新方案。介绍了国际上的研究情况,阐明了此技术的优越性和可行性。分析了航天用蒸汽压缩热泵的关键技术,包括微重力相变换热器及其研究方法、无润滑高转速压缩机等。在此基础上给出了中国开展航天领域蒸汽压缩热泵的研究方案。     

径向冷却通道截面特征长度对气冷稳定器性能影响

通过研究径向冷却通道截面特征长度的改变对气冷稳定器的冷态流场、冷却性能及流动损失的影响，为其进一步的优化设计提供参考依据。采用经过实验验证的CFD方法，对某气冷稳定器进行了数值模拟研究，在所研究的特征长度范围内，结果表明:特征长度的增加，减少了径向冷却通道下部的进气阻力，使得风兜引气率增加了667%；下部出气孔出流由于受到回流涡的影响，出流量明显低于上部出气孔，特征长度的改变对出流量分布的影响不大；特征长度的增加会加强径向稳定器近环形稳定器处的外壁面冷却效果，但是会减弱径向稳定器近中心锥处的外壁面冷却效果；特征长度的增加，使得出口总压恢复系数下降了0.086%，沿程总压恢复系数曲线向下移动。      

The interplanetary magnetic field. Solar origin and terrestrial effects

Many observations related to the large-scale structure of the interplanetary magnetic field, its solar origin and terrestrial effects are discussed. During the period observed by spacecraft the interplanetary field was dominated by a sector structure corotating with the sun in which the field is predominantly away from the sun (on the average in the Archimedes spiral direction) for several days (as observed near the earth), and then toward the sun for several days, etc. The average sector appears to be a coherent entity with internal structure such that its preceding portion is more active than its following portion. Cosmic rays corotate with the interplanetary field, and there are differential flows associated with the sector pattern. Profound effects on geomagnetic activity and the radiation belts are produced as the sector pattern rotates past the earth. The solar origin of the sector pattern is discussed. The solar source may be associated with the large-scale weak background photospheric fields observed with the solar magnetograph. It is suggested that there may be a rather continual relation between this solar structure and terrestrial responses, of which the recurring M-Region geomagnetic storms are just the most prominent example.     

Galileo probe Li-SO2 battery cell life testing

Several hundred D-sized, Li-SO₂ battery cells have been in a carefully controlled quiescent storage test for up to 14 years, starting at Honeywell but completing at the NASA Ames Research Center, in support of the Atmospheric Probe portion of the Galileo Mission to the planet Jupiter. This population of cells includes similar samples from 8 different manufacturing lots; the earliest from October 1981, the latest from October 1988. The baseline samples have been divided among several storage chambers, each having its own constant temperature, respectively, set between 0°C to 40°C. Non-invasive measurements have been made repeatedly of open circuit voltage and internal resistance (at 1000 Hz). At intervals, a small portion of the cells has been removed from storage and fully discharged under repetitive conditions, thus assessing any storage related loss of discharge capacity. The results show that for storage up to 20°C the cells have excellent stability. Above 20°C noticeable degradation occurs     

Adaptive Forward Error Control for Digital Satellite Systems

Two hybrid schemes of time-frequency resource sharing to increase the rain margin of Ku-and Ka-band satellite systems are proposed. Scheme 1 requires sharing a small pool of bandwidth for adaptive forward error control coding, sharing a small pool of time frame for rate reduction, and sharing a portion of low frequency time-division multiple access (TDMA) back-up frame for downlink transmission to the rain affected stations. Scheme 2 utilizes variable rate modulation and forward error correction, shares a small pool of time frame for rate reduction, and shares a portion of low frequency TDMA back-up frame. Effective usable capacities of the system using these schemes are calculated. Distribution of resources in order to maximize the effective usable capacity is also analyzed. The results obtained are compared with other adaptive schemes. Preliminary analysis shows that the utilized capacity of scheme 1 exceeds 99 percent of the effective usable capacity possible if it never rains for an outage of 0.05 percent and fade margin of 2.5 dB. For scheme 2 similar performance is achievable at a fade margin of 1.5 dB. For higher outage objectives the loss of effective utilized capacity is higher for scheme 2.