Formation of Giant Planets– An Attempt in Matching Observational Constraints

We present models of giant planet formation, taking into account migration and disk viscous evolution. We show that migration can significantly reduce the formation timescale bringing it in good agreement with typical observed disk lifetimes. We then present a model that produces a planet whose current location, core mass and total mass are comparable with the one of Jupiter. For this model, we calculate the enrichments in volatiles and compare them with the one measured by the Galileo probe. We show that our models can reproduce both the measured atmosphere enrichments and the constraints derived by Guillot et al. (2004), if we assume the accretion of planetesimals with ices/rocks ratio equal to 4, and that a substantial amount of CO₂ was present in vapor phase in the solar nebula, in agreement with ISM measurements.     

Energisation of O+ and O+ 2 Ions at Mars: An Analysis of a 3-D Quasi-Neutral Hybrid Model Simulation

We have studied the loss of O⁺ and O⁺ ₂ ions at Mars with a numerical model. In our quasi-neutral hybrid model ions (H⁺, He⁺⁺, O⁺, O⁺ ₂) are treated as particles while electrons form a massless charge-neutralising fluid. The employed model version does not include the Martian magnetic field resulting from the crustal magnetic anomalies. In this study we focus the Martian nightside where the ASPERA instrument on the Phobos-2 spacecraft and recently the ASPERA-3 instruments on the Mars Express spacecraft have measured the proprieties of escaping atomic and molecular ions, in particular O⁺ and O⁺ ₂ ions. We study the ion velocity distribution and how the escaping planetary ions are distributed in the tail. We also create similar types of energy-spectrograms from the simulation as were obtained from ASPERA-3 ion measurements. We found that the properties of the simulated escaping planetary ions have many qualitative and quantitative similarities with the observations made by ASPERA instruments. The general agreement with the observations suggest that acceleration of the planetary ions by the convective electric field associated with the flowing plasma is the key acceleration mechanism for the escaping ions observed at Mars.     

Satellite Measurements of Middle Atmospheric Impacts by Solar Proton Events in Solar Cycle 23

Solar cycle 23 was extremely active with seven of the largest twelve solar proton events (SPEs) in the past forty years recorded. These events caused significant polar middle atmospheric changes that were observed by a number of satellites. The highly energetic protons produced ionizations, excitations, dissociations, and dissociative ionizations of the background constituents in the polar cap regions (>60 degrees geomagnetic latitude), which led to the production of HO_x (H, OH, HO₂) and NO_y (N, NO, NO₂, NO₃, N₂O₅, HNO₃, HO₂NO₂, BrONO₂, ClONO₂). The HO_x increases led to short-lived ozone decreases in the polar mesosphere and upper stratosphere due to the short lifetimes of the HO_x constituents. Polar middle mesospheric ozone decreases greater than 50 % were observed and computed to last for hours to days due to the enhanced HO_x. The NO_y increases led to long-lived polar stratospheric ozone changes because of the long lifetime of the NO_y family in this region. Upper stratospheric ozone decreases of >10 % were computed to last for several months past the solar events in the winter polar regions because of the enhanced NO_y.     

Microstructure and high-temperature oxidation behavior of plasma-sprayed Si/Yb2SiO5 environmental barrier coatings

An environmental barrier coating (EBC) consisting of a silicon bond coat and an Yb₂SiO₅ top-coat was sprayed on a carbon fibers reinforced SiC ceramic matrix composite (CMC) by atmospheric plasma spray (APS). The microstructure of the coating annealed at 1300 °C and its high-temperature oxidation behavior at 1350 °C were investigated. The significant mass loss of silica during the plasma spray process led to the formation of Yb₂SiO₅ and Yb₂O₃ binary phases in the top-coat. Eutectics of Yb₂SiO₅ and Yb₂O₃ were precipitated in the top-coat, and channel cracks were formed in the top-coat after 20 h annealing because of the mismatch between the coefficients of thermal expansion (CTEs) of Yb₂SiO₅ and the SiC substrate. The EBC effectively improved the oxidation resistance of the CMC substrate. The channel cracks in the Yb₂SiO₅ top-coat provided inward diffusion channels for oxygen and led to the formation of oxidation delamination cracks in the bond coat, finally resulting in spallation failure of the coating after 80 h oxidation.     

等离子喷涂LaTi2Al9O19热障涂层的微观组织结构及热物理性能

 第一代热障涂层(TBCs)由氧化钇部分稳定的氧化锆(YSZ)陶瓷隔热层和金属粘结层组成,该涂层长期使用温度低于1 200℃。随着先进航空发动机向着高推重比发展,迫切要求发展新一代超高温、高隔热热障涂层材料。LaTi₂Al₉O₁₉(LTA)在1 500℃长期保持相稳定,是一种非常有前景的超高温热障涂层候选材料。本文采用大气等离子喷涂(APS)制备了LTA涂层,研究了喷涂工艺对涂层微观组织结构和热物理性能的影响。结果表明沉积态涂层中含少量的非晶态,在860℃和1 130℃出现晶化峰。等离子喷涂过程中La₂O₃挥发量较多,导致沉积态涂层中La元素与原始粉末相比含量偏低,而其他组分的化学成分随喷涂功率变化不大。LTA涂层的热扩散系数在1 400℃下为0.3~0.4 mm²·s^-1,热导率为1.1~1.6 W·m^-1·K^-1。1 050℃经过20小时热处理后,得到晶化的涂层在晶化温度范围内的热扩散系数和热导率值均增大。随着喷涂功率减小,涂层孔隙率增加,热导率减小。     

催化剂对HMX/AP/HTPB推进剂热分解特性的影响

热分析实验是使用国产CDR-1型差动热分析仪。热分解活化能用Ozawa法和Kissinger法计算[1],其它动力学参数均用Kissinger法求得。全部热分析实验均在氮气气氛中进行。推进剂燃速用靶线法燃速仪测定。HMX和各种催化剂在使用前均经过烘干处理。催化剂过100目筛。      

Origin of Molecular Oxygen in Comets: Current Knowledge and Perspectives

The Rosetta Orbiter Spectrometer for Ion and Neutral Analysis (ROSINA) instrument onboard the Rosetta spacecraft has measured molecular oxygen (O₂) in the coma of comet 67P/Churyumov-Gerasimenko (67P/C-G) in surprisingly high abundances. These measurements mark the first unequivocal detection of O₂ in a cometary environment. The large relative abundance of O₂ in 67P/C-G despite its high reactivity and low interstellar abundance poses a puzzle for its origin in comet 67P/C-G, and potentially other comets. Since its detection, there have been a number of hypotheses put forward to explain the production and origin of O₂ in the comet. These hypotheses cover a wide range of possibilities from various in situ production mechanisms to protosolar nebula and primordial origins. Here, we review the O₂ formation mechanisms from the literature, and provide a comprehensive summary of the current state of knowledge of the sources and origin of cometary O₂.     

Microstructure and Mechanical Properties of In-situ Synthesized Al2O3/TiAl Composites

Al2O3 particle-reinforced TiAl composites are successfully reaction-synthesized from the powder mixture of Ti, Al, TiO2, and Nb2O5, using the hot pressing reaction synthesis technique. The microstructure and mechanical properties of the as-sintered products are investigated. It is found that in the as-sintered products consisting of γ-TiAl, α2-Ti3Al, Al2O3, and NbAl3 phases, the fine Al2O3 particles tend to disperse on the grain boundaries. With the Nb2O5 content increasing, the grains are remarkably refined and the Al2O3 particles are dispersing more uniformly in the TiAl matrix, forming a partial lamellar structure containing α and lamellar phases. The hardness of the in-situ composites increases gradually, and the bending strength and the fracture toughness of the as-sintered products reach the maximum value of 398.5 MPa and 6.99 MPa·m^1/2, respectively, as the Nb2O5 content increases to 6 wt%.     

Experimental comparison between aircraft fuel tank inerting processes using NEA and MIG

Fuel tank inerting technologies are able to reduce the fire risk by injection of inert gas into the ullage or fuel, the former called ullage washing and the latter fuel scrubbing. The Green On-Board Inert Gas Generation System (GOBIGGS) is a novel technology based on flameless catalytic combustion, and owning to its simple structure and high inerting efficiency, it has received a lot of attentions. The inert gas in the GOBIGGS is mainly comprised of CO₂, N₂, and O₂ (hereinafter, Mixed Inert Gas (MIG)), while that in the On-Board Inert Gas Generation System (OBIGGS), which is one of the most widely used fuel tank inerting technologies, is Nitrogen-Enriched Air (NEA). The solubility of CO₂ is nearly 20 times higher than that of N₂ in jet fuels, so the inerting capability and performance are definitely disparate if the inert gas is selected as NEA or MIG. An inerting test bench was constructed to compare the inerting capabilities between NEA and MIG. Experimental results reveal that, if ullage washing is adopted, the variations of oxygen concentrations on the ullage and in the fuel are nearly identical no matter the inert gas is NEA or MIG. However, the ullage and dissolved oxygen concentrations of MIG scrubbing are always higher than those of NEA scrubbing.     

Numerical analysis of hypersonic thermochemical non-equilibrium environment for an entry configuration in ionized flow

A theoretical methodology for thermochemical non-equilibrium flow combing with the HLLC (Harten-Lax-van Leer Contact) scheme was applied to study the hypersonic thermochemical non-equilibrium environment of an entry configuration in ionized flow. A two-temperature controlling model was utilized and the Gupta’s 11 species (N₂, O₂, NO, O, N, NO⁺, N₂⁺, O₂⁺, N⁺, O⁺, e^?) thermochemical non-equilibrium model was taken. Firstly, numerical calculations of hypersonic thermochemical non-equilibrium environments for different aerodynamic shapes were carried out to verify the reliability of the method above. Then, the method was used to research the effects of ionization and wall catalysis on the hypersonic thermochemical non-equilibrium environment of the entry configuration in ionized flow. The shock stand-off distance can be reduced by thermochemical reactions but doesn’t continue to decrease significantly when ionization occurs. The shock stand-off distance calculated by the 11 species model is 4.2% smaller than that calculated by the 5 species (N₂, O₂, NO, O, N) thermochemical non-equilibrium model without considering ionization. Ionization reduces wall heat flux but increases wall pressure a little. The effect of ionization on aerothermal loads is greater than that of aerodynamic loads. The thermochemical reactions of electrons and ions catalyzed at the wall increase wall heat flux significantly but make a small change in wall pressure. The maximum wall heat flux obtained by only considering the electrons and ions catalyzed at the partially catalytic wall condition is 11.8% less than that calculated at the super-catalytic wall condition.     

SCC evaluation of a 2297 Al-Li alloy rolled plate using the slow-strain rate technique

The stress corrosion cracking (SCC) susceptibility of 2297 Al-Li alloy in 1 M NaCl + 0.01 M H₂O₂ solution (CP solution) and 1 M NaCl + 0.01 M H₂O₂ + 0.6 M Na₂SO₄ solution (CPS solution) was investigated by slow-strain rate tests at various strain rates ranging from 10⁻⁵ s⁻¹ to 10⁻⁷ s⁻¹. The roles of H₂O₂ and SO₄²⁻ in the corrosion process were estimated by potentiodynamic polarization and electrochemical impedance spectroscopy. 2297 Al-Li alloy does not fracture ascribed to SCC in CP solution, while it undergoes SCC in CPS solution. In CPS solution, with a decreasing strain rate from 10⁻⁵ s⁻¹ to 10⁻⁷ s⁻¹, the SCC susceptibility firstly rises and then declines exhibiting a peak value at a strain rate of 10⁻⁶ s⁻¹. H₂O₂ promotes the active dissolution while SO₄²⁻ lowers the corrosion rate. The SCC fracture is associated with a decline in the dissolution rate of the crack tip by SO₄²⁻, which leads to stress concentration. In CPS solution, a reduction in the local dissolution rate of the crack tip leads to stress concentration, resulting in SCC fracture. As the preferred initiation site for a crack, pits also show a noteworthy effect on SCC of 2297 Al-Li alloy.     

Pollution of the upper atmosphere by rockets

This report estimates the amounts of various constituents that would have to be continually injected by rockets into the upper atmosphere in order to double the worldwide natural concentrations there. Involved in the calculations are: (a) the natural atmospheric abundances of constituents such as H₂O, CO₂, NO, Na, K, Li, H, etc.; (b) the residence times in various regions of the atmosphere, since these determine how rapidly a constituent will be removed; and (c) the chemical or photochemical stability of a substance exposed to the upper atmosphere environment. It is concluded that a doubling of the CO₂, H₂O, or NO content would require per year on the order of 10³ to 10⁵ Saturn-type rockets, each injecting 100 tons of exhaust above 100 km. On the other hand, a few hundred small rockets per year, each containing 10 kg of the chemical, would probably double the Na content; similarly, less than two such rockets per year would be expected to double the Li content. These last conclusions have implications for future tracer experiments using these substances.The author is now an Associate Director of the National Center for Atmospheric Research (NCAR) in Boulder, Colorado. The work reported here was supported by the United States Air Force under Contract AF 49(638)-700 with the RAND Corporation. The views or conclusions contained in this paper should not, however, be interpreted as representing the official opinion of the United States Air Force.     

Stratosphere NO y Species Measured by MIPAS and GOMOS Onboard ENVISAT During 2002–2010: Influence of Plasma Processes onto the Observed Distribution and Variability

We present observations of stratosphere NO _y species from 2002 to 2010 taken by the Michelson Interferometer for Passive Atmospheric Sounding (MIPAS) and by the Global Ozone Monitoring by Occultation of Stars (GOMOS) instruments on board ENVISAT. We jointly used observations of MIPAS NO₂, HNO₃, N₂O₅, ClONO₂ and N₂O, and GOMOS NO₂ and NO₃. MIPAS results are part of the MIPAS2D database retrieved adopting a full 2D tomographic approach. We describe the mean distribution and variability of NO _y species in the stratosphere, identifying changes induced by plasma processes. Beside enhancements due to sporadic solar proton events, we show that winter polar NO₂ has an almost linear relationship with the geomagnetic activity index Ap down to about 10?hPa. This indicates a dominant role of energetic precipitating particles in the production of upper atmosphere NO _y . The correlation has clear signatures extending to mid latitudes. Partitioning of the NO _y reservoir species are also traced, with HNO₃ and N₂O₅ showing a correlation with Ap extending to lower altitude within the polar regions. We found no large signatures of an impact of thunderstorm-induced plasma processes onto monthly means of NO _y species in the stratosphere.     

Skylab measurements of low energy cosmic rays

In this review the present state of our knowledge on the properties of heavy ions in low energy cosmic rays measured in the Skylab mission and in other spacecrafts is summarised and the possible mechanisms of their origin are discussed. A brief review of the general features of the galactic and solar cosmic rays is given in order to understand the special features of the low energy heavy ions of cosmic rays. The results of the cosmic ray experiment in the Skylab show that in the low energy interval of 8–30 MeV/N, the abundances of oxygen, nitrogen, and neon ions, relative to carbon are enhanced by a factor of 5 to 2 as compared to high energy cosmic rays; while Mg, Si, S, and A are depleted. In 50–150 MeV/N energy interval the abundance of nuclei of Ca-Cr relative to iron-group (Z = 25–28) is found to be highly enhanced, as compared to high energy cosmic rays. Furthermore the observations of the energy spectra of O, N, and Ne ions and their fairly large fluences in the energy interval of 8–30 MeV/N below the geomagnetic cut off energy of 50 MeV/N for fully stripped nuclei at the Skylab orbit indicate that these heavy ions are probably in partly ionised states. Thus, it is found that the Skylab results represent a new type of heavy ion population of low energy cosmic rays below 50 MeV/N, in the near Earth space and their properties are distinctly different from those of high energy cosmic rays and are similar to those of the anomalous component in the interplanetary space. The available data from the Skylab can be understood at present on the hypothesis that low energy interplanetary cosmic ray ions of oxygen etc. occur in partly ionised state such as O⁺¹,O⁺², etc. and these reach the inner magnetosphere at high latitudes where stripping process occurs near mirror points and this leads to temporarily trapped ions such as O⁺³, O⁺⁴, etc. It is noted that the origin of these low energy heavy cosmic ray ions in the magnetosphere and in interplanetary space is not yet fully understood and new type of sources or processes are responsible for their origin and these need further studies.     

RP-3航空煤油替代燃料简化机理及其验证

选定正癸烷作为RP-3航空煤油单组分替代燃料,建立了一种包含36组分62步基元反应的简化机理.并设计了本生灯预混预蒸发试验系统对RP-3航空煤油的火焰进行了试验研究.同时,采用两种已被验证的煤油简化机理（分别为23步和38步）及62步简化机理对本生灯预混预蒸发燃烧火焰进行数值模拟,并将计算结果和试验数据相对比.结果表明：在轴向,温度和CO₂体积分数呈先上升后下降的趋势,并且温度在距喷口轴向距离为0.020m时达到最大值;而O₂体积分数呈现下降后上升的趋势,并且距喷口轴向距离为0.025m时达到最小值.与38步简化机理和23步简化机理所获得的数据相比,在各工况下,62步简化机理计算所获得的火焰温度分布和O₂体积分数分布与试验数据能很好地吻合;同时,62步简化机理计算的CO₂体积分数分布与试验数据变化规律基本一致,而23步和38步机理的计算结果只能保持和试验数据变化趋势的一致性.因此,选定的正癸烷可作为RP-3航空煤油的单组分替代燃料,并且所获得的62步简化机理能在较大范围内反映RP-3航空煤油的燃烧性能.     

The Planets and Titan Observed by ISO

Infrared spectroscopic observations of planets and Saturn's satellite Titan with the Infrared Space Observatory led to many significant discoveries that improved our understanding on the formation, physics and chemistry of these objects. The prime results achieved by ISO are: (1) a new and consistent determination of the D/H ratios on the giant planets and Titan; (2) the first precise measurement of the ¹⁵N/¹⁴N ratio in Jupiter, a valuable indicator of the protosolar nitrogen isotopic ratio; (3) the first detection of an external oxygen flux for all giant planets and Titan; (4) the first detection of some stratospheric hydrocarbons (CH₃, C₂H₄, CH₃C₂H, C₄H₂, C₆H₆); (5) the first detection of tropospheric water in Saturn; (6) the tentative detection of carbonate minerals on Mars; (7) the first thermal lightcurve of Pluto. Based on observations with ISO, an ESA project with instruments funded by ESA Member States (especially the PI countries: France, Germany, The Netherlands, and the United Kingdom), and with the participation of ISAS and NASA.     

Estimate of the climate impact of cryoplanes

The climate impact of cryoplanes (i.e. hydrogen-powered aircraft) is estimated in terms of radiative forcing (RF). We compare two scenarios: the conventional (i.e. kerosene-powered aircraft) scenario assumes a growth of the fleet until 2015 and a constant fleet thereafter. In the cryoplane scenario, the whole conventional fleet is instantaneously replaced by cryoplanes in 2015 and does not change thereafter. The resulting direct and indirect effects of aircraft emissions of H₂O (direct RF and RF due to contrails) and NO_x (RF due to O₃ production and CH₄ destruction), as well as aviation-induced atmospheric CO₂ are investigated for both scenarios.Whereas in case of conventional air traffic the components CO₂, O₃, CH₄ and contrails cause a similar RF, in case of cryoplanes, contrails are by far the most climatic relevant component. In 2015, total RF due to the cyoplane scenario is larger than total RF due to the conventional scenario. This changes with time and in 2100 the climate impact due to the cryoplane scenario is smaller. Due to large uncertainties regarding the optical properties of cryoplane contrails, the RF of contrails, and the impact of aviation on `natural' cirrus, our present knowledge is not sufficient to decide whether a substitution of the conventional fleet by a fleet of cryoplanes is of environmental benefit. Further research is necessary in order to faciliate a more precise approach to this question.     

HF-W Chronometry and Inner Solar System Accretion Rates

Models for the mechanisms of accretion of the terrestrial planets are re-examined using the experimental technique of high-precision isotope ratio mass spectrometry of tungsten (W). The decay of ¹⁸²Hf to ¹⁸²W (via ¹⁸²Ta) provides a new kind of radiometric chronometer of planet formation processes. Hafnium and W, the parent and daughter trace elements, are highly refractory; however, Hf is lithophile and strongly partitioned into the silicate portion of a planet, whereas W is moderately siderophile and preferentially partitioned into a coexisting metallic phase. More than 90% of terrestrial W has gone into the Earth's core during its formation. The residual silicate portion, the Earth's primitive mantle, has a Hf/W ratio in the range 10−40, an order of magnitude higher than chondritic (∼1.3). Tungsten isotopic data for the Earth and the Moon suggest that we can date a major event of planet formation: The Moon formed about 50 Myrs after the start of the solar system, providing strong support for the Giant Impact Theory of lunar origin. Recent simulations of this event imply that the Earth was probably only half formed at the time. From this we can deduce the planetary accretion rate. Tungsten isotope data for Mars provide evidence of a much shorter accretion interval, perhaps as little as 10 Myrs, but the rates for the Earth over the same time interval could have been comparable. The large W isotopic heterogeneities on Mars could only have been produced within the first 30 Myrs of the solar system. Large-scale mixing, e.g. from convective overturn, as is thought to drive the Earth's plates, must be absent from Mars. Limitations of the method such as 1) cosmogenic ¹⁸²Ta effects on lunar samples, 2) incomplete mixing of debris to cause W isotope heterogeneity on the Moon, and 3) initial ¹⁸²Hf/¹⁸⁰Hf heterogeneities of the early solar system are critically discussed. This revised version was published online in June 2006 with corrections to the Cover Date.     

Deuterium Fractionation in Interstellar Clouds

This paper reviews the chemical processes responsible for fractionating deuterium in interstellar molecules. I show that this process is intrinsically a low temperature phenomenon and discuss how the degree of enhancement of the deuterium content of molecules is related to the physical conditions, particularly abundances, in molecular clouds. If significant amounts of abundant species, such as CO, are frozen out on to interstellar dust grains, the resulting enhancement in H₂D⁺ can result in its abundance being greater than that of H ₃ ⁺ at 10K. Transfer of the deuteron from H₂D⁺ can then lead to the efficient formation of multiply deuterated species, such as NHD₂ and ND₃. Fractionation can also occur in grain surface reactions and some simple models are discussed. This revised version was published online in August 2006 with corrections to the Cover Date.     

Nucleation processes and aerosol chemistry

As the result of many observable optical phenomena, the occasional existence of upper atmospheric aerosols has been known since the beginning of the Century. Nevertheless, it is only during the last two decades that their persistent nature and extent of global distribution have become recognized. This review is addressed to the chemistry of upper atmospheric aerosols with particular attention to the chemical reactions and nucleation mechanisms responsible for their formation.Considering the stratosphere, it is now generally agreed that sulfate, mainly in the form of sulfuric acid, represents the single most abundant constituent of stratospheric aerosols. There is now strong evidence that these aerosols are formed in situ from sulfur bearing gases oxidized by free radicals. The various nucleation processes of atmospheric importance are reviewed, and it is shown that heteromolecular nucleation processes are almost certainly responsible for new particle formation in the stratosphere.The nature, and even existence, of aerosol layers above the stratosphere is less certain. The influx of extraterrestrial materials into the Earth atmosphere is estimated to be in the order of 50 to 500 tons per day. Considerations are given to the possible mechanisms which convert these materials to aerosol size particles. Although these particles provide one possible explanation for the appeareance of noctilucent clouds, nucleation about ions, most probably H₃O⁺ hydrates, is a strong contender as a more plausible formation mechanism. Considerable attention is given to this important atmospheric process, where it is shown that chemical forces contribute to the stability of the prenucleation clusters and the overall height of the energy barrier to nucleation. Finally, the role of aerosols in the sodium and other cycles of trace upper atmospheric constituents, is discussed.This research was performed under the auspices of the U.S. Atomic Energy Commission and partially financed by the Department of Transportation and the National Science Foundation under interagency agreements.