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51.
Panagiotis K. Marhavilas 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2012
The analysis of energetic particles and magnetic field measurements from the Ulysses spacecraft has shown that in a series of events, the energy density contained in the suprathermal tail particle distribution is comparable to or larger than that of the magnetic field, creating conditions of high-beta plasma. In this work we analyze periods of high-beta suprathermal plasma occurrences (βep > 1) in interplanetary space, using the ratio (βep) of the energetic particle (20 keV to ∼5 MeV) and magnetic field energy densities from measurements covering the entire Ulysses mission lifetime (1990–2009) in order to reveal new or to reconfirm some recently defined interesting characteristics. The main key-results of the work are summarized as follows: (i) we verify that high-beta events are detected within well identified regions corresponding mainly to the vicinity of shock surfaces and magnetic structures, and associated with energetic particle intensity enhancements due to (a) reacceleration at shock-fronts and (b) unusually large magnetic field depressions. (ii) We define three considerable features for the high-beta events, concentrated on the next points: (a) there is an appreciable solar-activity influence on the high-beta events, during the maximum and middle solar-cycle phase, (b) the annual peak magnitude and the number of occurrences of high events are well correlated with the sunspot number, (c) the high-beta suprathermal plasma events present a spatial distribution in heliographic latitudes (HL) up to ∼±80°, and a specific important concentration on the low (−25° ? HL < −6°, 6° < HL ? 25°) and median (−45° ? HL < −25°, 25° < HL ? 45°) latitudes. We also reconfirm by a statistical analysis the results of Marhavilas and Sarris (2011), that the high-beta suprathermal plasma (βep > 1) events are characterized by a very large parameter βep (up to 1732.5), a great total duration (406 days) and a large percentage of the Ulysses-mission lifetime (which is equal to 6.34% of the total duration with usable measurements, and 11.3% of the duration in presence of suprathermal particles events). 相似文献
52.
在分析了几种传统的电机制动方案基础上,提出了一种适合陀螺马达的能耗制动方案,该方案依据马达逐渐停转时自身产生的微弱电信号,再经放大处理后作为能耗制动的控制信号,实现陀螺马达准确、可靠、平稳的停止,避免了不及时切断电源而烧坏定子绕组的情况. 相似文献
53.
We have obtained the first UV high resolution spectra of hot luminous stars in M31 with the FOS onHubble Space Telescope. The spectra, combined with optical spectroscopic and photometric observations, enable us to study their stellar winds and photospheric parameters. We derive mass-loss rates and velocity laws from the wind line profiles, with the SEI method, as well as information on abundances. The wind lines and photospheric spectra are compared with galactic stars of the same spectral type.The spectra analyzed so far indicate that the stars have mass-loss rates comparable or slightly lower than galactic stars of the same spectral type, but possibly different velocity laws in their winds. The spectra of two stars are discussed here. 相似文献
54.
Chung-Ming Ko Min-Hsu Chu 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2005,35(12):2115-2118
A two-fluid model is used to study the time evolution of stellar winds including the dynamical effect of cosmic rays. Neglecting the diffusion of cosmic rays, we seek self-similar solutions to spherically symmetric winds with a termination shock. The velocity upstream of the shock is taken to be zero. Physical solutions are those that can connect the shock to the star with the velocity approaching zero at the star. Two parameters govern the behaviour of the solutions, namely, the ratio of the upstream sound speed to the shock speed (in an inertial frame) and the gravitation potential of the central star. In some parameter regimes, no physical solution is possible. 相似文献
55.
T. Hirayama 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008,41(6):914-925
In this paper we present a new mechanism of the main energy conversion of the solar flare. Since a flare inducing prominence (flux tube) rises Vz ? 300 km s−1, the plasmas below it cannot continuously eject with Alfvén speeds of VA = 3000 km s−1 but probably with Vz ≈ ±100 km s−1. Plasma up and downflows with VA will within a short duration be blocked between the chromosphere where reconnected flux tubes are piling up, and the slowly rising flux rope. Hence the Petschek slow shock mechanism is difficult to be realized as a major energy converting mechanism. 相似文献
56.
57.
A. Galli P. Wurz S. Barabash A. Grigoriev H. Gunell R. Lundin M. Holmström A. Fedorov 《Space Science Reviews》2006,126(1-4):267-297
We present measurements of energetic hydrogen and oxygen atoms (ENAs) on the nightside of Mars detected by the neutral particle
detector (NPD) of ASPERA-3 on Mars Express. We focus on the observations for which the field-of-view of NPD was directed at
the nightside of Mars or at the region around the limb, thus monitoring the flow of ENAs towards the nightside of the planet.
We derive energy spectra and total fluxes, and have compiled maps of hydrogen ENA outflow. The hydrogen ENA intensities reach
105 cm−2 sr−1 s−1, but no oxygen ENA signals above the detection threshold of 104 cm−2 sr−1 s−1 are observed. These intensities are considerably lower than most theoretical predictions. We explain the discrepancy as due
to an overestimation of the charge-exchange processes in the models for which too high an exospheric density was assumed.
Recent UV limb emission measurements (Galli et al., this issue) point to a hydrogen exobase density of 1010 m−3 and a very hot hydrogen component, whereas the models were based on a hydrogen exobase density of 1012 m−3 and a temperature of 200 K predicted by Krasnopolsky and Gladstone (1996). Finally, we estimate the global atmospheric loss
rate of hydrogen and oxygen due to the production of ENAs. 相似文献
58.
在铁路无线列调通信中存在弱场区和盲区,通信质量难以控制。设计了完整的方案,提高了原无线列调中存在的弱场区的场强,并增大场强覆盖率,使通话距离得到扩展,改善了话音质量。 相似文献
59.
以能量为核心,建立太阳能飞行器的获能模型;通过对太阳能飞行器飞行剖面特点的分析,设计飞行过程中各个阶段的飞行方案,并建立相应的耗能模型;考虑目前储能电池技术水平,根据产能和耗能模型,建立储能模型,完成了能源闭环模型的设计;参照Zephyr 7太阳能无人机的结构参数对论文建立的模型进行了仿真分析,获取了飞行过程中能量变化规律,同时对飞行姿态进行优化。结果表明:通过对太阳能飞行器昼夜飞行高度的不同设置以及飞行姿态角的优化,太阳能飞行器可以实现跨昼夜持久飞行。 相似文献
60.
Astronauts are often on a voluntarily reduced energy intake during space missions, possibly caused by a metabolic or emotional stress response with involvement of the central serotonergic system (SES). We investigated 24 h urinary excretion (24 h-E) of serotonin (5-HT) and 5-hydroxyindol acidic acid as indicators of the SES in healthy males under two different normocaloric conditions: normal physical activity (NPA) and -6 degree head-down-tilt (HDT). HDT or NPA were randomly arranged with a recovery period of 6 months in between. 24 h-E of hormones varied widely among individuals. Values were higher in HDT compared to NPA. Assuming that the 24 h-E values are, beside being indicators for alterations in the number and metabolism of platelets. Also indicators of central SES, HDT condition seems to activate central SES in a higher degree compared to NPA. Therefore, changes in central SES might be involved in the mechanisms associated with space flight or microgravity, including possible maladaptations such as voluntary undernutrition. 相似文献