Numerical study on the impacts of heterogeneous reactions on ozone formation in the Beijing urban area   总被引：2，自引：0，他引：2  

徐峻  张远航  王玮 《大气科学进展》2006,23(4):605-614

The air quality model CMAQ-MADRID （Community Multiscale Air Quality-Model of Aerosol Dynamics, Reaction, Ionization and Dissolution） was employed to simulate summer O3 formation in Beijing China, in order to explore the impacts of four heterogeneous reactions on O3 formation in an urban area. The results showed that the impacts were obvious and exhibited the characteristics of a typical response of a VOC-limited regime in the urban area. For the four heterogeneous reactions considered, the NO2 and HO2 heterogeneous reactions have the most severe impacts on O3 formation. During the O3 formation period, the NO2 heterogeneous reaction increased new radical creation by 30%, raising the atmospheric activity as more NO→NO2 conversion occurred, thus causing the O3 to rise. The increase of O3 peak concentration reached a maximum value of 67 ppb in the urban area. In the morning hours, high NO titration reduced the effect of the photolysis of HONO, which was produced heterogeneously at night in the surface layer. The NO2 heterogeneous reaction in the daytime is likely one of the major reasons causing the O3 increase in the Beijing urban area. The HO2 heterogeneous reaction accelerated radical termination, resulting in a decrease of the radical concentration by 44% at the most. O3 peak concentration decreased by a maximum amount of 24 ppb in the urban area. The simulation results were improved when the heterogeneous reactions were included, with the O3 and HONO model results close to the observations.  相似文献   

大别山双河长英质片麻岩在1.0～4.5GPa下的结晶实验及其地质意义     

刘晓春  杨农  曲玮 《地球学报》1999,20(2):113-120

在７５０～１２００℃、１．０～４．５ＧＰａ条件下对取自于大别山双河的长英质片麻岩进行了重结晶实验。在７５０℃时,随压力增加矿物生成顺序为：角闪石在１．７５ＧＰａ时出现,２．５ＧＰａ时消失;黑云母在１．７５ＧＰａ时通过水化反应生成多硅白云母;绿帘石可以稳定到＞３．５ＧＰａ,在４ＧＰａ时转变成硬柱石;石榴石和绿辉石在１．５ＧＰａ时开始出现,而斜长石在１．７５ＧＰａ时消失;石英在３ＧＰａ时转变为柯石英。这表明角闪岩相与榴辉岩相的转变发生在１．５～１．７５ＧＰａ,并且,榴辉岩相可进一步划分出角闪榴辉岩相、柯石英榴辉岩相和硬柱石榴辉岩相等,它们分别指示不同的压力区间。多硅白云母是长英质岩石在高压－超高压条件下的主要共生矿物,其水化反应特性及结构水的保存致使陆壳在深俯冲过程中未发生明显的脱水作用,这是大别山碰撞带未能形成钙碱性岩浆弧的主要原因。  相似文献   

Variation in mantle lithology and composition beneath the Ngao Bilta volcano,Adamawa Massif,Cameroon volcanic line,West-central Africa     

Robert Temdjim  Merlin Patrick Njombie Wagsong  Arnold Julien Nzakou Tsepeng  Stephen Foley 《地学前缘(英文版)》2020,(2):665-677

Mantle peridotites entrained as xenoliths in the lavas of Ngao Bilta in the eastern branch of the continental Cameroon Line were examined to constrain mantle processes and the origin and nature of melts that have modified the upper mantle beneath the Cameroon Line.The xenoliths consist mainly of lherzolite with subordinate harzburgite and dunite.They commonly contain olivine,orthopyroxene,clinopyroxene and spinel although the dunite is spinel-free.Amphibole is an essential constituent in the lherzolites.Mineral chemistry differs between the three types of peridotite:olivines have usual mantle-like Mg#of around 90 in lherzolites,but follow a trend of decreasing Mg#(to 82)and NiO(to 0.06 wt.%)that is continuous in the dunites.Lherzolites also contain orthopyroxenes and/or clinopyroxenes with low-Mg#,indicating a reaction that removes Opx and introduces Cpx,olivine,amphibole and spinel.This is attributed to reaction with a silica-undersaturated silicate melt such as nephelinite or basanite,which originated as a low-degree melt from a depleted source as indicated by low Al2O3 and Na2O in Cpx and high Na2O/K2O in amphibole.Thermobarometric estimates place the xenoliths at pressures of 11–15 kbar(35–50 km)and temperatures of 863–957
C,along a dynamic rift geotherm and shallower than the region where carbonate melts may occur.The melt/rock reactions exhibited by the Ngao Bilta xenoliths are consistent with their peripheral position in the eastern branch of the Cameroon Volcanic Line in an area of thinned crust and lithosphere beneath the Adamawa Uplift.  相似文献   

The effect of the ¹⁹F(α, p)²²Ne reaction rate uncertainty on the yield of fluorine from Wolf–Rayet stars     

Richard J. Stancliffe  Maria Lugaro  Claudio Ugalde  Christopher A. Tout  Joachim Görres  Michael Wiescher 《Monthly notices of the Royal Astronomical Society》2005,360(1):375-379

In the light of recent recalculations of the  ¹⁹F(α, p)²²Ne  reaction rate, we present results of the expected yield of ¹⁹F from Wolf–Rayet (WR) stars. In addition to using the recommended rate, we have computed models using the upper and lower limits for the rate, and hence we constrain the uncertainty in the yield with respect to this reaction. We find a yield of  3.1 × 10⁻⁴ M_⊙  of ¹⁹F with our recommended rate, and a difference of a factor of 2 between the yields computed with the upper and lower limits. In comparison with previous work we find a difference in the yield of a factor of approximately 4, connected with a different choice of mass loss. Model uncertainties must be carefully evaluated in order to obtain a reliable estimate of the yield, together with its uncertainties, of fluorine from WR stars.  相似文献   

Time of explosive decay of a daemon-containing nucleus     

E. M. Drobyshevski 《Monthly notices of the Royal Astronomical Society》2000,311(3):L1-L3

We start from the hypothesis that the dark matter of the Galactic disc contains Planckian particles carrying a negative electric charge of up to Z =10, which we call dark electric matter objects (daemons). Daemons are capable of catalysing proton-fusion reactions, which may account for the observed solar neutrino deficiency. The inevitable poisoning of the catalytic property of daemons as they capture heavy nuclei ( A 20) in the interior of the Sun is used to estimate the decay time of a daemon-containing nucleus (nucleon) in quantum-relativistic processes, which remain largely unknown. This time is τ _ex∼10⁻⁷ s. This may mean that the lower limit on the mass of an intranucleonic particle interacting with a daemon is ∼10⁸–10¹⁰ GeV and, possibly, even ∼10¹⁴–10¹⁵ GeV. The desirability of a search for multiple events occurring with an interval ∼ τ _ex along the 'slow' daemon trajectories on operating installations dedicated to detection of the proton decay is pointed out.  相似文献   

Reaction‐induced nucleation and growth v. grain coarsening in contact metamorphic,impure carbonates     

A. BERGER  S. H. BRODHAG  M. HERWEGH 《Journal of Metamorphic Geology》2010,28(8):809-824

The understanding of the evolution of microstructures in a metamorphic rock requires insights into the nucleation and growth history of individual grains, as well as the coarsening processes of the entire aggregate. These two processes are compared in impure carbonates from the contact metamorphic aureole of the Adamello pluton (N‐Italy). As a function of increasing distance from the pluton contact, the investigated samples have peak metamorphic temperatures ranging from the stability field of diopside/tremolite down to diagenetic conditions. All samples consist of calcite as the dominant matrix phase, but additionally contain variable amounts of other minerals, the so‐called second phases. These second phases are mostly silicate minerals and can be described in a KCMASHC system (K₂O, CaO, MgO, Al₂O₃, SiO₂, H₂O, CO₂), but with variable K/Mg ratios. The modelled and observed metamorphic evolution of these samples are combined with the quantification of the microstructures, i.e. mean grain sizes and crystal size distributions. Growth of the matrix phase and second phases strongly depends on each other owing to coupled grain coarsening. The matrix phase is controlled by the interparticle distances between the second phases, while the second phases need the matrix grain boundary network for mass transfer processes during both grain coarsening and mineral reactions. Interestingly, similar final mean grain sizes of primary second phase and second phases newly formed by nucleation are observed, although the latter formed later but at higher temperatures. Moreover, different kinetic processes, attributed to different driving forces for growth of the newly nucleated grains in comparison with coarsening processes of the pre‐existing phases, must have been involved. Chemically induced driving forces of grain growth during reactions are orders of magnitudes larger compared to surface energy, allowing new reaction products subjected to fast growth rates to attain similar grain sizes as phases which underwent long‐term grain coarsening. In contrast, observed variations in grain size of the same mineral in samples with a similar T–t history indicate that transport properties depend not only on the growth and coarsening kinetics of the second phases but also on the microstructure of the dominant matrix phase during coupled grain coarsening. Resulting microstructural phenomena such as overgrowth and therefore preservation of former stable minerals by the matrix phase may provide new constraints on the temporal variation of microstructures and provide a unique source for the interpretation of the evolution of metamorphic microstructures.  相似文献   

Time-variable emission from transiently accreting neutron stars in quiescence due to deep crustal heating     

Greg Ushomirsky  Robert E. Rutledge 《Monthly notices of the Royal Astronomical Society》2001,325(3):1157-1166

Transiently accreting neutron stars in quiescence ( L _X ≲10³⁴ erg s⁻¹) have been observed to vary in intensity by factors of few, over time-scales of days to years. If the quiescent luminosity is powered by a hot neutron star core, the core cooling time-scale is much longer than the recurrence time, and cannot explain the observed, more rapid variability. However, the non-equilibrium reactions which occur in the crust during outbursts deposit energy in isodensity shells, from which the thermal diffusion time-scale to the photosphere is days to years. The predicted magnitude of variability is too low to explain the observed variability unless – as is widely believed – the neutrons beyond the neutron-drip density are superfluid. Even then, the variability due to this mechanism in models with standard core neutrino cooling processes is less than 50 per cent – still too low to explain the reported variability. However, models with rapid core neutrino cooling can produce a variability by a factor as great as 20, on time-scales of days to years following an outburst. Thus, the factors of ∼ few intensity variability observed from transiently accreting neutron stars can be accounted for by this mechanism only if rapid core cooling processes are active.  相似文献   

Intermediate-metallicity, high-velocity stars and Galactic chemical evolution   总被引：2，自引：0，他引：2  

S. G. Ryan  I. M. Smith 《Monthly notices of the Royal Astronomical Society》2003,341(1):199-212

High signal-to-noise ratio spectra were obtained of 10 high-proper-motion stars having  −1 ≲[Fe/H] < 0  , and a comparable number of disc stars. All but two of the high-proper-motion stars were confirmed to have  [Fe/H] > −1.0  , some approaching solar metallicity, but, even so, earlier measurements overestimated the metallicities and velocities of some of these stars. Models of stellar populations were used to assign membership probabilities to the Galactic components to which the high-velocity stars might belong. Many were found to be more probably thick-disc than halo objects, despite their large space motions, and two might be associated with the inner Galaxy. It may be necessary to reassess contamination of previous halo samples, such as those used to define the metallicity distribution, to account for contamination by high-velocity thick-disc stars, and to consider possible subcomponents of the halo.
The change in [α/Fe] ratios at  [Fe/H]≃−1.0  is often used to constrain the degree and timing of Type Ia supernova nucleosynthesis in Galactic chemical-evolution models. [Ti/Fe] values were measured for eight of the high-velocity stars. Both high- and low-[Ti/Fe] halo stars exist; likewise high- and low-[Ti/Fe] thick-disc stars exist. We conclude that the [Ti/Fe]'break' is not well defined for a given population; nor is there a simple, continuous evolutionary sequence through the break. Implications for the interpretation of the [α/Fe] break in terms of SN Ia time-scales and progenitors are discussed. The range of [Ti/Fe] found for high -velocity (low rotation) thick-disc stars contrasts with that for the low -velocity (high rotation) thick-disc sample studied by Prochaska et al.  相似文献   

Oxygen isotopic ratios in first dredge-up red giant stars and nuclear reaction rate uncertainties revisited     

Jeffrey A. Stoesz  Falk Herwig 《Monthly notices of the Royal Astronomical Society》2003,340(3):763-770

  相似文献   

恒星尘埃的实验室研究--实验天体物理学   总被引：1，自引：0，他引：1  

徐伟彪 《天文学报》2006,47(1):1-8

原始球粒陨石含有来自恒星的微小固体颗粒(微米级),这些尘埃的同位素组成与太阳系物质截然不同,它们是目前唯一能直接获得的恒星固体样品．已发现的恒星尘埃有金刚石、石墨、碳化硅、刚玉、尖晶石、氮化物、和硅酸盐等,它们的母体恒星包括红巨星,AGB恒星、新星和超新星．对恒星尘埃的研究,使得更深入地了解星系的化学演化历史、恒星内部的核反应和湍流机制、恒星大气中尘埃的形成、星际介质物理现象等．恒星尘埃把天体物理领域延伸到了微观世界,它有机地结合了地球化学实验技术和天体物理理论,开辟了一门崭新的天文学分支实验天体物理学．  相似文献