低燃速的端羧基聚丁二烯丙烯腈(CTBN)推进剂

对端羧基聚丁二烯丙烯睛(CTBN)液体共聚物为粘合剂的极低燃速的复合固定推进剂进行了论证。本计划的目的是,研制一种用于燃气发生器的(StarterCartridge)、压力在70公斤/厘米~2(100磅/英寸~2)下,燃速指标为1.78毫米/秒(0.070英寸/秒)的推进剂。选择了双环氧交链系统的低丙烯睛 CTBN 粘合剂,因为它的老化性能和工艺性能较之一般的粘合剂材料优越。在改进的 MK6气体发生器装置中,用浇注单孔圆柱形的、端面包复和外圆柱面包复的推进剂药柱进行弹道性能评定。用50%双级配的过氯酸胺、30%CTBN 粘合剂和20%装填密度高的硝基胍组成的推进剂配方成功地满足了设计要求,在要求的压力与温度25℃(77°F)下,达到了1.70毫米/秒(0.067英寸/秒)的燃速指标。当压力在35公斤/厘米~2(500磅/英寸~2)到70公斤/厘米~2(1000磅/英寸~2)范围内,温度在-54℃和74℃之间时,所测得的温度敏感系数π=0.36%/℃(0.20%/°F)。通过初步的力学性能和物理性能试验表明,此种类型的药柱设计在工作条件下,是合格的。因此,这种推进剂用于各种低燃速的场合似乎是有吸引力的。     

M stars as targets for terrestrial exoplanet searches and biosignature detection

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.     

Interplanetary transfer of photosynthesis: an experimental demonstration of a selective dispersal filter in planetary island biogeography

We launched a cryptoendolithic habitat, made of a gneissic impactite inoculated with Chroococcidiopsis sp., into Earth orbit. After orbiting the Earth for 16 days, the rock entered the Earth's atmosphere and was recovered in Kazakhstan. The heat of entry ablated and heated the rock to a temperature well above the upper temperature limit for life to below the depth at which light levels are insufficient for photosynthetic organisms ( approximately 5 mm), thus killing all of its photosynthetic inhabitants. This experiment shows that atmospheric transit acts as a strong biogeographical dispersal filter to the interplanetary transfer of photosynthesis. Following atmospheric entry we found that a transparent, glassy fusion crust had formed on the outside of the rock. Re-inoculated Chroococcidiopsis grew preferentially under the fusion crust in the relatively unaltered gneiss beneath. Organisms under the fusion grew approximately twice as fast as the organisms on the control rock. Thus, the biologically destructive effects of atmospheric transit can generate entirely novel and improved endolithic habitats for organisms on the destination planetary body that survive the dispersal filter. The experiment advances our understanding of how island biogeography works on the interplanetary scale.     

Biomarker response to galactic cosmic ray-induced NOx and the methane greenhouse effect in the atmosphere of an Earth-like planet orbiting an M dwarf star

Planets orbiting in the habitable zone of M dwarf stars are subject to high levels of galactic cosmic rays (GCRs), which produce nitrogen oxides (NOx) in Earth-like atmospheres. We investigate to what extent these NO(Mx) species may modify biomarker compounds such as ozone (O3) and nitrous oxide (N2O), as well as related compounds such as water (H2O) (essential for life) and methane (CH4) (which has both abiotic and biotic sources). Our model results suggest that such signals are robust, changing in the M star world atmospheric column due to GCR NOx effects by up to 20% compared to an M star run without GCR effects, and can therefore survive at least the effects of GCRs. We have not, however, investigated stellar cosmic rays here. CH4 levels are about 10 times higher on M star worlds than on Earth because of a lowering in hydroxyl (OH) in response to changes in the ultraviolet. The higher levels of CH4 are less than reported in previous studies. This difference arose partly because we used different biogenic input. For example, we employed 23% lower CH4 fluxes compared to those studies. Unlike on Earth, relatively modest changes in these fluxes can lead to larger changes in the concentrations of biomarker and related species on the M star world. We calculate a CH4 greenhouse heating effect of up to 4K. O3 photochemistry in terms of the smog mechanism and the catalytic loss cycles on the M star world differs considerably compared with that of Earth.     

THREE ASPECTS OF ISAR SIGNAL PROCESSING

ＴＨＲＥＥＡＳＰＥＣＴＳＯＦＩＳＡＲＳＩＧＮＡＬＰＲＯＣＥＳＳＩＮＧＳｈｅＺｈｉｓｈｕｎ；ＺｈｕＺｈａｏｄａ（ＤｅｐａｒｔｍｅｎｔｏｆＥｌｅｃｔｒｏｎｉｃＥｎｇｉｎｅｅｒｉｎｇ，ＮＵＡＡ２９ＹｕｄａｏＳｔｒｅｅｔ，Ｎａｎｊｉｎｇ２１００１６Ｐ．Ｒ．Ｃ...     

A NEW APPROACH FOR ISAR TRANSLATIONAL MOTION COMPENSATION

ＡＮＥＷＡＰＰＲＯＡＣＨＦＯＲＩＳＡＲＴＲＡＮＳＬＡＴＩＯＮＡＬＭＯＴＩＯＮＣＯＭＰＥＮＳＡＴＩＯＮＹｉｎＪｕｎ；ＺｈｕＺｈａｏｄａ（ＤｅｐａｒｔｍｅｎｔｏｆｅｌｅｃｔｒｏｎｉｃＥｎｇｉｎｅｅｒｉｎｇ，ＮＵＡＡ２９ＹｕｄａｏＳｔｒｅｅｔ，Ｎａｎｊｉｎ...     

AN OPTICAL FIBRE SENSOR BASED CUTTING FORCE MEASURING DEVICE

ＡＮＯＰＴＩＣＡＬＦＩＢＲＥＳＥＮＳＯＲＢＡＳＥＤＣＵＴＴＩＮＧＦＯＲＣＥＭＥＡＳＵＲＩＮＧＤＥＶＩＣＥＪｉｎＷｅｎｌｉｎｇ；ＷａｎｇＸｉｎ（ＤｅｐａｒｔｍｅｎｔｏｆＭｄｃｈａｎｉｃａｌＥｎｇｉｎｅｅｒｉｎｇ，ＮＵＡＡ２９ＹｕｄａｏＳｔｒｅｅｔ，Ｎａ...     

LORENTZ TIME-SPACE TRANSFORMATION IS A APPROXIMATE CALCULATION METHOD IN AERODYNAMICS FOR COMPRESSIBILITY

1　 LORENZ TRANSFORMATIONEXISTED IN AERODYNAMICANALYSISIn earlier paper a relation between magnetand fluid is deduced.Naturally we can think thedeep meaning of it.And man asks:does theaerodynamic system also has the character ofmagnet field?To answer this question,relativityspace- time wave equation are analyzed.It de-scribes the same phenomena of the wave equationof compress fluid in normal space and time.It isamazement.In normal compressible fluid thenon- dimensional simp…     

稀土Y对低膨胀高温合金显微组织和界面的影响

运用分析电子显微术、高分辨电子显微术、化学相分析和 X-射线衍射等方法分析研究了Fe-Ni-Co-Nb-Ti-Si低膨胀高温合金的相组成和相结构 ,以及稀土对合金的组织和性能的影响规律。结果显示 ,微量的稀土主要存在于合金的片状相中 ,并使其晶体结构发生变化。加入适量的稀土 Y后 ,合金片状相变得更加细密、均匀。和不含稀土的低膨胀高温合金相比 ,含 Y的低膨胀高温合金中片状相与基体的晶格错配由 0 .7%下降到 0 .0 7% ,表明界面应力明显下降