Emergence of a Habitable Planet

We address the first several hundred million years of Earth’s history. The Moon-forming impact left Earth enveloped in a hot silicate atmosphere that cooled and condensed over ∼1,000 yrs. As it cooled the Earth degassed its volatiles into the atmosphere. It took another ∼2 Myrs for the magma ocean to freeze at the surface. The cooling rate was determined by atmospheric thermal blanketing. Tidal heating by the new Moon was a major energy source to the magma ocean. After the mantle solidified geothermal heat became climatologically insignificant, which allowed the steam atmosphere to condense, and left behind a ∼100 bar, ∼500 K CO₂ atmosphere. Thereafter cooling was governed by how quickly CO₂ was removed from the atmosphere. If subduction were efficient this could have taken as little as 10 million years. In this case the faint young Sun suggests that a lifeless Earth should have been cold and its oceans white with ice. But if carbonate subduction were inefficient the CO₂ would have mostly stayed in the atmosphere, which would have kept the surface near ∼500 K for many tens of millions of years. Hydrous minerals are harder to subduct than carbonates and there is a good chance that the Hadean mantle was dry. Hadean heat flow was locally high enough to ensure that any ice cover would have been thin (<5 m) in places. Moreover hundreds or thousands of asteroid impacts would have been big enough to melt the ice triggering brief impact summers. We suggest that plate tectonics as it works now was inadequate to handle typical Hadean heat flows of 0.2–0.5 W/m². In its place we hypothesize a convecting mantle capped by a ∼100 km deep basaltic mush that was relatively permeable to heat flow. Recycling and distillation of hydrous basalts produced granitic rocks very early, which is consistent with preserved >4 Ga detrital zircons. If carbonates in oceanic crust subducted as quickly as they formed, Earth could have been habitable as early as 10–20 Myrs after the Moon-forming impact.     

硼酸盐玻璃中稀土离子的发光研究

应用荧光光谱、红外振动光谱等研究了在可见光区发光的Ｐｒ（３＋），Ｓｍ（３＋），Ｅｕ（３＋），Ｔｂ（３＋），Ｄｙ（３＋），Ｅｒ（３＋）和Ｔｍ（３＋）等镧系稀土离子在硼酸盐玻璃中的发光行为，系统地分析了稀土离子在硼酸盐玻璃基质中的激发谱和发光谱特性。     

对流层特大暴雨天气对电离层变化的影响

研究气象活动对电离层变化的影响．利用时序叠加方法，通过对1958-1998年期间发生在武汉的5次特大暴雨天气事件对武汉上空电离层变化的影响进行分析，发现：(1)特大暴雨能够引起低电离层，fbEs和，f0Es参量较明显地减小；(2)特大暴雨对电离层F区寻常波描迹的最低虚高h′F和电离层等效峰高hpF的参量也有一定影响，且随着雨量的增大这种影响作用也会增加；(3)特大暴雨对电离层其他参量影响甚弱或没有影响．本文认为，特大暴雨天气事件对电离层的影响主要来自于动力过程，特别是特大暴雨激发的或相伴的大气重力波、潮汐波和行星波等长周期大尺度过程的作用．     

Magnetosphere Imaging Instrument (MIMI) on the Cassini Mission to Saturn/Titan

The magnetospheric imaging instrument (MIMI) is a neutral and charged particle detection system on the Cassini orbiter spacecraft designed to perform both global imaging and in-situ measurements to study the overall configuration and dynamics of Saturn’s magnetosphere and its interactions with the solar wind, Saturn’s atmosphere, Titan, and the icy satellites. The processes responsible for Saturn’s aurora will be investigated; a search will be performed for substorms at Saturn; and the origins of magnetospheric hot plasmas will be determined. Further, the Jovian magnetosphere and Io torus will be imaged during Jupiter flyby. The investigative approach is twofold. (1) Perform remote sensing of the magnetospheric energetic (E > 7 keV) ion plasmas by detecting and imaging charge-exchange neutrals, created when magnetospheric ions capture electrons from ambient neutral gas. Such escaping neutrals were detected by the Voyager l spacecraft outside Saturn’s magnetosphere and can be used like photons to form images of the emitting regions, as has been demonstrated at Earth. (2) Determine through in-situ measurements the 3-D particle distribution functions including ion composition and charge states (E > 3 keV/e). The combination of in-situ measurements with global images, together with analysis and interpretation techniques that include direct “forward modeling’’ and deconvolution by tomography, is expected to yield a global assessment of magnetospheric structure and dynamics, including (a) magnetospheric ring currents and hot plasma populations, (b) magnetic field distortions, (c) electric field configuration, (d) particle injection boundaries associated with magnetic storms and substorms, and (e) the connection of the magnetosphere to ionospheric altitudes. Titan and its torus will stand out in energetic neutral images throughout the Cassini orbit, and thus serve as a continuous remote probe of ion flux variations near 20R _S (e.g., magnetopause crossings and substorm plasma injections). The Titan exosphere and its cometary interaction with magnetospheric plasmas will be imaged in detail on each flyby. The three principal sensors of MIMI consists of an ion and neutral camera (INCA), a charge–energy–mass-spectrometer (CHEMS) essentially identical to our instrument flown on the ISTP/Geotail spacecraft, and the low energy magnetospheric measurements system (LEMMS), an advanced design of one of our sensors flown on the Galileo spacecraft. The INCA head is a large geometry factor (G ∼ 2.4 cm² sr) foil time-of-flight (TOF) camera that separately registers the incident direction of either energetic neutral atoms (ENA) or ion species (≥5^∘ full width half maximum) over the range 7 keV/nuc < E < 3 MeV/nuc. CHEMS uses electrostatic deflection, TOF, and energy measurement to determine ion energy, charge state, mass, and 3-D anisotropy in the range 3 ≤ E ≤ 220 keV/e with good (∼0.05 cm² sr) sensitivity. LEMMS is a two-ended telescope that measures ions in the range 0.03 ≤ E ≤ 18 MeV and electrons 0.015 ≤ E≤ 0.884 MeV in the forward direction (G ∼ 0.02 cm² sr), while high energy electrons (0.1–5 MeV) and ions (1.6–160 MeV) are measured from the back direction (G ∼ 0.4 cm² sr). The latter are relevant to inner magnetosphere studies of diffusion processes and satellite microsignatures as well as cosmic ray albedo neutron decay (CRAND). Our analyses of Voyager energetic neutral particle and Lyman-α measurements show that INCA will provide statistically significant global magnetospheric images from a distance of ∼60 R _S every 2–3 h (every ∼10 min from ∼20 R _S). Moreover, during Titan flybys, INCA will provide images of the interaction of the Titan exosphere with the Saturn magnetosphere every 1.5 min. Time resolution for charged particle measurements can be < 0.1 s, which is more than adequate for microsignature studies. Data obtained during Venus-2 flyby and Earth swingby in June and August 1999, respectively, and Jupiter flyby in December 2000 to January 2001 show that the instrument is performing well, has made important and heretofore unobtainable measurements in interplanetary space at Jupiter, and will likely obtain high-quality data throughout each orbit of the Cassini mission at Saturn. Sample data from each of the three sensors during the August 18 Earth swingby are shown, including the first ENA image of part of the ring current obtained by an instrument specifically designed for this purpose. Similarily, measurements in cis-Jovian space include the first detailed charge state determination of Iogenic ions and several ENA images of that planet’s magnetosphere.This revised version was published online in July 2005 with a corrected cover date.     

Acceleration of interplanetary pick-up ions and anomalous cosmic rays

It may not be doubted anymore that anomalous cosmic rays (ACRs) are produced in the heliosphere from interplanetary pick-up ions through their acceleration at the solar wind termination shock. However, there is no general agreement in the community of heliospheric researchers concerning the mechanism of injection of the pick-up ions into the shock acceleration. We discuss here three possible ways for pick-up ions to be involved into the acceleration process at the termination shock: (1) preacceleration of pick-up ions in the whole region from the Sun up to the termination shock by solar wind turbulences and interplanetary shock waves, (2) local preacceleration of pick-up ions in a vicinity of the termination shock by shock surfing, and (3) formation of high-velocity tails in pick-up ion spectra consisting of secondary pick-up ions which are produced in the supersonic solar wind due to ionization of energetic neutral atoms entering from the inner heliosheath.     

Avoid online radiation risk: Theoretical simulation of chromosome breaks in cells exposed to heavy ions

In this study, we report an easy and quick method on simulating chromosome breaks in cells exposed to heavy charged particles. The theoretical value of chromosome break was calculated, and validated comparison with experimental value by using premature chromosome condensation technique. A good consistency was found between theoretical and experimental value. This suggested that higher relative biological effectiveness of heavy ions was closely correlated with its physical characteristics. Also, a safe approach on predicting chromosome breaks in cells exposed to heavy ions at off-line environment can be considered. Furthermore, three key factors influencing the theoretical simulation was investigated and discussed.     

新型内突扩加力燃烧室方案可行性分析

介绍了一种新型内突扩加力燃烧室方案,具有质量轻、尺寸小、红外隐身功能突出等优点;在分析当前高推重比发动机需求的基础上,结合目前国内外加力燃烧室的技术水平,根据新一代军用发动机的加力燃烧室进气参数,论证了该方案所具有的现实可行性。     

二冲程点燃式直喷重油发动机小负荷试验

利用燃用轻柴油的二冲程点燃式空气辅助缸内直喷发动机,进行了转速为3000r/min、节气门开度为10%与20%下的小负荷试验,研究了点火及喷油参数对发动机性能的影响。试验结果表明:当节气门开度较小时,采用上止点前30°~40°点火提前角,饱和点火能量,稀混合气（过量空气系数大于1.1）及适度提前混合物喷射结束时刻的策略能够充分改善发动机动力性和经济性。随着负荷增大,点火能量影响程度减小,采用适度推迟点火提前角,偏浓混合气（过量空气系数小于1.0）及提前喷射结束时刻策略,增加燃油蒸发时间来充分发挥发动机动力性能,而采用饱和点火能量,偏稀混合气（过量空气系数大于1.15）能够大幅度改善发动机经济性及HC/CO排放。      

不同钝体宽度下的驻涡燃烧室排放试验

为了研究空气流量分配对驻涡燃烧室对排放特性的影响,了解对驻涡燃烧室内污染物生成的过程及其影响因素,设计了一个能够改变中心钝体宽度、仅凹腔供油的驻涡燃烧室.在常压下对该驻涡燃烧室进行了排放特性试验,进口温度保持200℃.试验中,燃烧室进口马赫数为0.15~0.3.影响排放的因素主要包括雾化质量、凹腔当量比以及与进口马赫数相关的驻留时间等.总体来说雾化质量、凹腔当量比的提高对降低CO和HC的排放是有利的,但是这会使NOx排放增加.在低凹腔当量比时,CO排放曲线变化下降比较平缓,甚至出现上升趋势,而HC排放曲线比较陡峭.这是由于HC的消耗速度比CO消耗速度快,随着凹腔当量比的增加,供油压力提高,燃油雾化粒径变小,燃油蒸发时间缩短,使HC排放快速减少,中间产物CO大量产生而来不及消耗.凹腔当量比进一步上升时,由于燃烧温度的提高,使得CO排放快速减少.在燃烧室内燃烧过程中,NOx的形成和消耗是非常复杂的过程,目前只能作一些定性的分析,而CO和HC的反应过程相对简单.通过对不同钝体槽宽下,具有相似凹腔前壁流量的工况的比较,发现CO和HC的形成主要受凹腔内工作状况影响,而NOx的形成过程更复杂,主流也对其产生着重要的影响.      

Low-dose carbon ion irradiation effects on DNA damage and oxidative stress in the mouse testis

To investigate the effects of low-dose carbon ion irradiation on reproductive system of mice, the testes of outbred Kunming strain mice were whole-body irradiated with 0, 0.05, 0.1, 0.5 and 1 Gy, respectively. We measured DNA double-strand breaks (DNA DSBs) and oxidative stress parameters including malondialdehyde (MDA) content, superoxide dismutase (SOD) activity, and testis weight and sperm count at 12 h, 21 d and 35 d after irradiation in mouse testis. At 12 h postirradiation, a significant increase in DNA DSB level but no pronounced alterations in MDA content or SOD activity were observed in 0.5 and 1 Gy groups compared with the control group. At 21 d postirradiation, there was a significant reduction in sperm count and distinct enhancements of DSB level and MDA content in 0.5 and 1 Gy groups in comparison with control. At 35 d postirradiation, the levels of DNA DSBs and MDA, and SOD activity returned to the baseline except for the MDA content in 1 Gy (P < 0.05), while extreme falls of sperm count were still observed in 0.5 (P < 0.01) and 1 Gy (P < 0.01) groups. For the 0.05 or 0.1 Gy group, no differences were found in DNA DSB level and MDA content between control and at 12 h, 21 d and 35 d after irradiation, indicating that lower doses of carbon ion irradiation have no significant influence on spermatogenesis processes. In this study, male germ cells irradiated with over 0.5 Gy of carbon ions are difficult to repair completely marked by the sperm count. Furthermore, these data suggest that the deleterious effects may be chronic or delayed in reproductive system after whole-body exposure to acute high-dose carbon ions.