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161.
The cardiovascular function is one of the main disturbed by weightlessness: it is particularly affected by the astronaut's return to Earth, where symptoms linked to the cardiovascular deconditioning syndrom appear in the following forms: (1) orthostatic intolerance with its risk of syncope: (2) higher submaximal oxygen consumption for an equivalent work load. Lower Body Negative Pressure (LBNP) is intended to stimulate the venous system of the lower limbs; however, the specific effects of periodical LBNP sessions on the orthostatic intolerance have never been studied. With this objective in mind, 5 volunteers took part in two recent antiorthostatic bedrest experiments for 30 days. In the first experiment 3 subjects were submitted to several sessions of LBNP experiment per day and 2 others were controls; in the second experiment the LBNP group of the 1st one became controls and vice-versa. Two orthostatic investigations were performed: (1) 5 days before the bedrest; (2) at the end of the 30 day bedrest period. The results showed: (1) when the subjects were control, a high orthostatic intolerance post bedrest with 3 syncopes and one presyncopal state during the first minutes of the tilt test; (2) when the subjects were submitted to LBNP sessions, no orthostatic intolerance. 相似文献
162.
163.
Cyanobacteria are capable of tolerating environmental extremes. To survive in extreme environments, cyanobacteria have developed the capability to adapt to a variety of stresses. For example, cyanobacteria have adopted a number of strategies with which to survive UV stress, including expression of UV-screening pigments and antioxidant systems. We have previously shown that several antioxidants are significantly expressed in Nostoc sp. by UVB irradiation. We report here that the content of UV-responsive biomarkers such as β-carotene and scytonemin can be easily detected by Fourier transform Raman spectroscopy with use of a small sample size and that the content of β-carotene is dependant on the UVB intensity and exposure time. Our results indicate that Raman spectroscopy may be a helpful tool to analyze UV-protective molecules of cyanobacterium in astrobiological studies without access to large sample sizes and complicated extractions, which are needed by other analytical techniques such as high-performance liquid chromatography and mass spectrometry. 相似文献
164.
目前修建的多数机场和公路的刚性道（路）面都铺设一个基层（subbaselayer);从而由双层基础（two-layer foundation)支承着道面板构成一个混凝土板块系统。本文利用双层基础体系上板块的计算推导出一个解析的回归计算、分析道（路）面参数的方法（closed-form procedure)。为了计算道（路）面的表面弯沉,已编制出一个称之为NUS－DEF3的计算机程序,用作回归计算分析的子程序。文中介绍了这个系统的回归算法。该算法是把一个有三个未知数的三元方程组简化为一个简单的非线性方程。它不同于通过最小二乘方迭代求最好的解的常规方法,而是在得出唯一解析解时,从一开始就不需要选择初始模量。该文还用数字范例对三个典型的双层基础上板块的问题做了演示。 相似文献
165.
166.
当美国西南航空公司进入其25周年之际,它仍保持着效率型典范的形象,这对于其大多数竞争对手来说是难以理解的.由于调整了航线的长度,西南航空公司在各大航空公司中营运成本最低,并且是过去22年中唯一每年都赢利的定期航班航空公司.西南航空公司自1971年成立起,每年就产生12.07%的投资回收率.对于许多观察家来说,西南航空公司一直是竞争或赶超的对手.它在美国超过50%的最大城市对航线上所占市场份额居首位,而且在全部城市对航线上保持着三分之二的市场份额. 相似文献
167.
本文研究了四点安装的 SC 切和 AT 切谐振器的加速度灵敏度和加热特性。加速度的灵敏度是根据振动引起的边带来确定的。每一个谐振器的测量结果均与振动方向和振动频率呈函数关系。所研究的谐振器的参数包括:切角(AT 和 SC)、固定方位、泛音次数、晶片的几何形状(平平的、平凸的、双凸的)、安装支架的刚度和晶片材料(天然石英、人造石英和经扫掠的人造石英)。预热特性的测量是,先把谐振器浸入冰水中,然后迅速将其浸入沸水中,等达到热均衡之后,用晶体阻抗表(CI-meter)监测谐振器频率。对不同的 AT 和 SC 切设计(基模和三次泛音)的预热时间作了比较。可以看出,四点安装的陶瓷扁平封装的 SC 切谐振器能够在20秒内从0℃预热到100℃,而频率在2×10~(-7)以内。 相似文献
168.
储存在射频四极陷阱(Trap)中的199Hg离子在4O.5GHz频率时的超精细谐振,证明具有极窄的相对线宽,因而被选作为高精密的频率标准。引起该类频标频率变化的主要因素是因储存离子运动产生的二阶多普勒频移,采用少量低压气体作为背景,使运动的离子被致冷至300K所形成的离子云的密度几乎完全决定于伪电势与空间电荷力的平衡。我们发现在这种情况下,根据陷阱参数、温度和储存离子的总数和质量可以准确地计算出二阶多普勒频移。用氦作为致冷气体所进行的大量实验表明,由射频脉冲宽度限制的谱线宽度为0.85Hz。根据所观测到的谱线形状可以预计自然线宽将小于0.1Hz。采用闭环稳定储存离子数的方法,已能使测得的二阶多普勒频移达n×10~(-13)量级。 相似文献
169.
Andre-Deshays C Haignere JP Guell A Marsal O Suchet L Kotovskaya A Gratchev V Noskin A Grigoriev A 《Acta Astronautica》1995,36(8-12):707-712
One year after the achievemant of the 2 weeks ANTARES french-russian mission in the MIR station in July 1992, a 22 days ALTAÏR mission with a french cosmonaut has been performed in July 1993, making use of the scientific payload remaining on board. Taking benefit of the analysis of the previous mission, the experimental protocols were adapted to refine scientific objectives and gave to the scientists the opportunity to enhance quantitatively and qualitatively their results. The french biomedical program, conducted in close scientific cooperation with IMBP and associated laboratories, was composed of 8 experiments out of which 2 were new with regards to the ANTARES program. In the field of cardio-vascular physiology and fluid regulation, the experiments: ORTHOSTATISME, DIURESE have been renewed and complemented by the TISSU experiment (proposed by a german scientist) and a real-time tele-assistance program using US echography technic and ground support from the french CADMOS support control center located in Toulouse. With respect to neurosciences objectives, to the experiments VIMINAL (cognitive processes) and ILLUSIONS (study of proprioceptives cues), was added the SYNERGIES experiment to analyse the postural adjustements during movement. The IMMUNOLOGIE experiment carried on and the radiobiological experiment BIODOSE ended.
Adding the results of the 2 missions ANTARES and ALTAÏR, and the data obtained in between onboard with russian cosmonauts, the scientists have received a wealth of physiological data and gained reproducibility and confidence in their results. 相似文献
170.
Scalo J Kaltenegger L Segura A Segura AG Fridlund M Ribas I Kulikov YN Grenfell JL Rauer H Odert P Leitzinger M Selsis F Khodachenko ML Eiroa C Kasting J Lammer H 《Astrobiology》2007,7(1):85-166
The changing view of planets orbiting low mass stars, M stars, as potentially hospitable worlds for life and its remote detection was motivated by several factors, including the demonstration of viable atmospheres and oceans on tidally locked planets, normal incidence of dust disks, including debris disks, detection of planets with masses in the 5-20 M() range, and predictions of unusually strong spectral biosignatures. We present a critical discussion of M star properties that are relevant for the long- and short-term thermal, dynamical, geological, and environmental stability of conventional liquid water habitable zone (HZ) M star planets, and the advantages and disadvantages of M stars as targets in searches for terrestrial HZ planets using various detection techniques. Biological viability seems supported by unmatched very long-term stability conferred by tidal locking, small HZ size, an apparent short-fall of gas giant planet perturbers, immunity to large astrosphere compressions, and several other factors, assuming incidence and evolutionary rate of life benefit from lack of variability. Tectonic regulation of climate and dynamo generation of a protective magnetic field, especially for a planet in synchronous rotation, are important unresolved questions that must await improved geodynamic models, though they both probably impose constraints on the planet mass. M star HZ terrestrial planets must survive a number of early trials in order to enjoy their many Gyr of stability. Their formation may be jeopardized by an insufficient initial disk supply of solids, resulting in the formation of objects too small and/or dry for habitability. The small empirical gas giant fraction for M stars reduces the risk of formation suppression or orbit disruption from either migrating or nonmigrating giant planets, but effects of perturbations from lower mass planets in these systems are uncertain. During the first approximately 1 Gyr, atmospheric retention is at peril because of intense and frequent stellar flares and sporadic energetic particle events, and impact erosion, both enhanced, the former dramatically, for M star HZ semimajor axes. Loss of atmosphere by interactions with energetic particles is likely unless the planetary magnetic moment is sufficiently large. For the smallest stellar masses a period of high planetary surface temperature, while the parent star approaches the main sequence, must be endured. The formation and retention of a thick atmosphere and a strong magnetic field as buffers for a sufficiently massive planet emerge as prerequisites for an M star planet to enter a long period of stability with its habitability intact. However, the star will then be subjected to short-term fluctuations with consequences including frequent unpredictable variation in atmospheric chemistry and surficial radiation field. After a review of evidence concerning disks and planets associated with M stars, we evaluate M stars as targets for future HZ planet search programs. Strong advantages of M stars for most approaches to HZ detection are offset by their faintness, leading to severe constraints due to accessible sample size, stellar crowding (transits), or angular size of the HZ (direct imaging). Gravitational lensing is unlikely to detect HZ M star planets because the HZ size decreases with mass faster than the Einstein ring size to which the method is sensitive. M star Earth-twin planets are predicted to exhibit surprisingly strong bands of nitrous oxide, methyl chloride, and methane, and work on signatures for other climate categories is summarized. The rest of the paper is devoted to an examination of evidence and implications of the unusual radiation and particle environments for atmospheric chemistry and surface radiation doses, and is summarized in the Synopsis. We conclude that attempts at remote sensing of biosignatures and nonbiological markers from M star planets are important, not as tests of any quantitative theories or rational arguments, but instead because they offer an inspection of the residues from a Gyr-long biochemistry experiment in the presence of extreme environmental fluctuations. A detection or repeated nondetections could provide a unique opportunity to partially answer a fundamental and recurrent question about the relation between stability and complexity, one that is not addressed by remote detection from a planet orbiting a solar-like star, and can only be studied on Earth using restricted microbial systems in serial evolution experiments or in artificial life simulations. This proposal requires a planet that has retained its atmosphere and a water supply. The discussion given here suggests that observations of M star exoplanets can decide this latter question with only slight modifications to plans already in place for direct imaging terrestrial exoplanet missions. 相似文献