Extreme oxygen isotope ratios in the early Solar System

The origins of the building blocks of the Solar System can be studied using the isotopic composition of early planetary and meteoritic material. Oxygen isotopes in planetary materials show variations at the per cent level that are not related to the mass of the isotopes; rather, they result from the mixture of components having different nucleosynthetic or chemical origins. Isotopic variations reaching orders of magnitude in minute meteoritic grains are usually attributed to stellar nucleosynthesis before the birth of the Solar System, whereby different grains were contributed by different stars. Here we report the discovery of abundant silica-rich grains embedded in meteoritic organic matter, having the most extreme 18O/16O and 17O/16O ratios observed (both approximately 10(-1)) together with a solar silicon isotopic composition. Both O and Si isotopes indicate a single nucleosynthetic process. These compositions can be accounted for by one of two processes: a single exotic evolved star seeding the young Solar System, or irradiation of the circumsolar gas by high energy particles accelerated during an active phase of the young Sun. We favour the latter interpretation, because the observed compositions are usually not expected from nucleosynthetic processes in evolved stars, whereas they are predicted by the selective trapping of irradiation products.     

Possible in situ formation of meteoritic nanodiamonds in the early Solar System

Grains of dust that pre-date the Sun provide insights into their formation around other stars and into the early evolution of the Solar System. Nanodiamonds recovered from meteorites, which originate in asteroids, have been thought to be the most abundant type of presolar grain. If that is true, then nanodiamonds should be at least as abundant in comets, because they are thought to have formed further out in the early Solar System than the asteroid parent bodies, and because they should be more pristine. Here we report that nanodiamonds are absent or very depleted in fragile, carbon-rich interplanetary dust particles, some of which enter the atmosphere at speeds within the range of cometary meteors. One interpretation of the results is that some (perhaps most) nanodiamonds formed within the inner Solar System and are not presolar at all, consistent with the recent detection of nanodiamonds within the accretion discs of other young stars. An alternative explanation is that all meteoritic nanodiamonds are indeed presolar, but that their abundance decreases with heliocentric distance, in which case our understanding of large-scale transport and circulation within the early Solar System is incomplete.     

Chronology of the early Solar System from chondrule-bearing calcium-aluminium-rich inclusions

Chondrules and Ca-Al-rich inclusions (CAIs) are high-temperature components of meteorites that formed during transient heating events in the early Solar System. A major unresolved issue is the relative timing of CAI and chondrule formation. From the presence of chondrule fragments in an igneous CAI, it was concluded that some chondrules formed before CAIs (ref. 5). This conclusion is contrary to the presence of relict CAIs inside chondrules, as well as to the higher abundance of 26Al in CAIs; both observations indicate that CAIs pre-date chondrules by 1-3 million years (Myr). Here we report that relict chondrule material in the Allende meteorite, composed of olivine and low-calcium pyroxene, occurs in the outer portions of two CAIs and is 16O-poor (Delta17O approximately -1 per thousand to -5 per thousand). Spinel and diopside in the CAI cores are 16O-rich (Delta17O up to -20 per thousand), whereas diopside in their outer zones, as well as melilite and anorthite, are 16O-depleted (Delta17O = -8 per thousand to 2 per thousand). Both chondrule-bearing CAIs are 26Al-poor with initial 26Al/27Al ratios of (4.7 +/- 1.4) x 10(-6) and <1.2 x 10(-6). We conclude that these CAIs had chondrule material added to them during a re-melting episode approximately 2 Myr after formation of CAIs with the canonical 26Al/27Al ratio of 5 x 10(-5).     

Widespread magma oceans on asteroidal bodies in the early Solar System

Immediately following the formation of the Solar System, small planetary bodies accreted, some of which melted to produce igneous rocks. Over a longer timescale (15-33 Myr), the inner planets grew by incorporation of these smaller objects through collisions. Processes operating on such asteroids strongly influenced the final composition of these planets, including Earth. Currently there is little agreement about the nature of asteroidal igneous activity: proposals range from small-scale melting, to near total fusion and the formation of deep magma oceans. Here we report a study of oxygen isotopes in two basaltic meteorite suites, the HEDs (howardites, eucrites and diogenites, which are thought to sample the asteroid 4 Vesta) and the angrites (from an unidentified asteroidal source). Our results demonstrate that these meteorite suites formed during early, global-scale melting (> or = 50 per cent) events. We show that magma oceans were present on all the differentiated Solar System bodies so far sampled. Magma oceans produced compositionally layered planetesimals; the modification of such bodies before incorporation into larger objects can explain some anomalous planetary features, such as Earth's high Mg/Si ratio.     

Contemporaneous formation of chondrules and refractory inclusions in the early Solar System

Chondrules and calcium-aluminium-rich inclusions (CAIs) are preserved materials from the early history of the Solar System, where they resulted from thermal processing of pre-existing solids during various flash heating episodes which lasted for several million years. CAIs are believed to have formed about two million years before the chondrules. Here we report the discovery of a chondrule fragment embedded in a CAI. The chondrule's composition is poor in 16O, while the CAI has a 16O-poor melilite (Ca, Mg, Al-Silicate) core surrounded by a 16O-rich igneous mantle. These observations, when combined with the previously reported CAI-bearing chondrules, strongly suggest that the formation of chondrules and CAIs overlapped in time and space, and that there were large fluctuations in the oxygen isotopic compositions in the solar nebula probably synchronizing astrophysical pulses.     

Origin of the obliquities of the giant planets in mutual interactions in the early Solar System

The origin of the spin-axis orientations (obliquities) of the giant planets is a fundamental issue because if the obliquities resulted from tangential collisions with primordial Earth-sized protoplanets, then they are related to the masses of the largest planetesimals out of which the planets form. A problem with this mechanism, however, is that the orbital planes of regular satellites would probably be uncorrelated with the obliquities, contrary to observations. Alternatively, they could have come from an external twist that affected the orientation of the Solar System plane; but in this model, the outer planets must have formed too rapidly, before the event that produced the twist. Moreover, the model cannot be quantitatively tested. Here I show that the present obliquities of the giant planets were probably achieved when Jupiter and Saturn crossed the 1:2 orbital resonance during a specific migration process: different migration scenarios cannot account for the large observed obliquities. The existence of the regular satellites of the giant planets does not represent a problem in this model because, although they formed soon after the planetary formation, they can follow the slow evolution of the equatorial plane it produces.     

Elwakil混沌系统的混沌控制与同步

根据Hurwitz稳定性判据,提出了Elwakil混沌系统的一种控制方案,实现了Elwakil系统对任意给定的光滑参考信号的追踪,并且实现了该混沌系统的自同步以及与Rssler混沌系统的异结构同步.该方法中采用的控制器只需要知道受控系统的部分状态变量的信息,因此形式简单,容易实现.Matlab的数值仿真表明该方法的有效性.     

Young chondrules in CB chondrites from a giant impact in the early Solar System

Chondrules, which are the major constituent of chondritic meteorites, are believed to have formed during brief, localized, repetitive melting of dust (probably caused by shock waves) in the protoplanetary disk around the early Sun. The ages of primitive chondrules in chondritic meteorites indicate that their formation started shortly after that of the calcium-aluminium-rich inclusions (4,567.2 +/- 0.7 Myr ago) and lasted for about 3 Myr, which is consistent with the dissipation timescale for protoplanetary disks around young solar-mass stars. Here we report the 207Pb-206Pb ages of chondrules in the metal-rich CB (Bencubbin-like) carbonaceous chondrites Gujba (4,562.7 +/- 0.5 Myr) and Hammadah al Hamra 237 (4,562.8 +/- 0.9 Myr), which formed during a single-stage, highly energetic event. Both the relatively young ages and the single-stage formation of the CB chondrules are inconsistent with formation during a nebular shock wave. We conclude that chondrules and metal grains in the CB chondrites formed from a vapour-melt plume produced by a giant impact between planetary embryos after dust in the protoplanetary disk had largely dissipated. These findings therefore provide evidence for planet-sized objects in the earliest asteroid belt, as required by current numerical simulations of planet formation in the inner Solar System.     

混沌系统混沌同步态的分岔行为

研究了耦合混沌系统中混沌同步态的分岔行为．随着振子数的增加分岔点将提前，在自治系统中混沌同步态比非自治系统有更强的稳定性。     

一个新自治系统的混沌控制和同步

针对一个新三维混沌自治系统,研究了该混沌系统的控制和同步问题．利用线性负反馈法和Routh-Hurwitz稳定性条件,获得达到控制目标时负反馈系数所满足的条件,并借助Matlab对受控系统进行数值模拟,仿真结果验证了该方法的有效性;设计了实现其同步的一种非线性控制器．利用李雅普诺夫稳定性定理,证明了同步误差系统是全局渐近稳定的．Matlab数值仿真结果表明所设计的非线性控制器能有效地实现混沌同步．     

一类分数阶混沌系统的耦合同步

基于稳定性理论,选取合适的初值,以三维分数阶Rssler系统和三维分数阶Lü混沌系统为例,实现了分数阶混沌系统的耦合同步,将整数阶同步理论扩展到分数阶混沌系统,利用整数阶同步条件结合仿真方法确定耦合系数,为分数阶混沌系统的应用奠定了基础.     

一个新混沌系统的混沌分析及混沌控制

研究了一种新混沌系统的基本动力学行为及混沌控制的问题,给出了相图、功率谱、Poincaré映射以及Lyapunov指数,基于Lyapunov指数谱和全局分岔图分析了系统参数对新系统的影响,最后运用线性反馈法对新混沌系统进行控制,将其控制到周期轨道上,并给出了数值仿真结果证实了所设计的线性反馈控制器的有效性.     

Lorenz混沌系统的追踪控制

基于Lyapunov稳定性定理,设计了一个控制器,对Lorenz混沌系统进行控制,使之能追踪任意的输入信号.利用Lyapunov函数和Barbalat定理,证明了该控制器的有效性.同时,以正弦信号、Lorenz混沌驱动系统和Rossler混沌驱动系统为例进行了数值仿真,其结果与理论推导相一致.     

Sprott-F系统的混沌反控制

混沌反控制是指使一个非混沌系统混沌化或增强一个现有的混沌系统的混沌行为,基于时滞和外力反馈法的基本原理,结合理论分析与仿真实验,实现了改进的Sprott-F系统的混沌反控制.     

基于混沌同步的混沌加密系统安全性

在Kerckhoff准则下,从选择密文攻击出发,探讨了基于混沌同步的混沌加密系统的安全性,并指出在选择密文攻击下可以获得加密系统的密钥．了基于超混沌的混沌加密系统和基于混沌的混合加密系统．结果表明,基于混沌同步的混沌加密系统不具有很高的安全性．     

太阳系边缘天体

最近,美国天文学家新近在太阳系边缘地带观测到一个除冥王星之外个头最大的天体.发现者是加利福尼亚理工学院的迈克·布朗及其同事.新发现的这一天体的临时国际代号为"2002LM60",它绕太阳公转的周期为288年,直径约1 290 km,相当于冥王星的一半,位于太阳系边缘的"柯伊伯带".这一发现引起世人的普遍关注.太阳系有九大行星,距太阳最远的是冥王星.这是常识大家都知道.     

一类三阶混沌系统的分支分析与混沌控制

从稳定性与混沌控制的角度,研究了时滞对具反馈控制的三阶混沌系统动力学性质的影响.首先,研究时滞对系统平衡点稳定性的影响以及Hopf分支的存在性.其次,应用中心流形理论和规范型方法,得到了决定分支周期解的稳定性和方向的详细计算公式.通过设计合适的反馈增益和时滞,混沌振荡转变为稳定的不动点或稳定的周期轨.最后,用数值模拟验证了理论结果的有效性.