The inner solar system cratering record and the evolution of impactor populations

We review previously published and newly obtained crater size-frequency distributions in the inner solar system. These data indicate that the Moon and the terrestrial planets have been bombarded by two populations of objects. Population 1,dominating at early times, had nearly the same size distribution as the present-day asteroid belt, and produced heavily cratered surfaces with a complex, multi-sloped crater size-frequency distribution. Population 2, dominating since about 3.8–3.7 Gyr,had the same size distribution as near-Earth objects(NEOs) and a much lower impact flux, and produced a crater size distribution characterized by a differential –3single-slope power law in the crater diameter range 0.02 km to 100 km. Taken together with the results from a large body of work on age-dating of lunar and meteorite samples and theoretical work in solar system dynamics, a plausible interpretation of these data is as follows. The NEO population is the source of Population 2 and it has been in near-steady state over the past ～ 3.7–3.8 Gyr; these objects are derived from the main asteroid belt by size-dependent non-gravitational effects that favor the ejection of smaller asteroids. However, Population 1 was composed of main belt asteroids ejected from their source region in a size-independent manner, possibly by means of gravitational resonance sweeping during orbit migration of giant planets;this caused the so-called Late Heavy Bombardment(LHB). The LHB began some time before ～3.9 Gyr, peaked and declined rapidly over the next ～ 100 to 300 Myr,and possibly more slowly from about 3.8–3.7 Gyr to ～2 Gyr. A third crater population(Population S) consisted of secondary impact craters that can dominate the cratering record at small diameters.     

SIMS Pb/Pb dating of Zr-rich minerals in lunar meteorites Miller Range 05035 and LaPaz Icefield 02224:Implications for the petrogenesis of mare basalt

Miller Range (MIL) 05035 and LaPaz Icefield (LAP) 02224 are unbrecciated lunar basalt meteorites. In this report, we studied their petrography and mineralogy and made in situ uranogenic Pb/Pb dating of Zr-rich minerals. Petrography and mineralogy of these two lunar meteorites are consistent with previous investigations. The zirconolite Pb/Pb age of MIL 05035 is 3851±8 Ma (2σ), in excellent agreement with previous reports. This age suggests that MIL 05035 could be paired with Asuka 881757, a low-Ti mare basalt meteorite. The magmatic event related to MIL 05035 was probably due to the late heavy impact bom- bardment on the moon around 3.9 Ga. One baddeleyite grain in LAP 02224 shows a large variation of Pb/Pb age, from 3109±29 to 3547±21 Ma (2σ), much older than the whole-rock age of the same meteorite (~3.02±0.03 Ga). The other baddeleyite grain in LAP 02224 has an age of 3005±17 Ma (2σ). The result indicates that the minimum crystallization age of LAP 02224 is ~3.55 Ga and the younger ages could reflect late thermal disturbance on U-Pb system.     

冀西北石榴角闪二辉麻粒岩早期高压变质矿物组合的确定及其形成的温压条件——来自锆石中矿物包裹体的信息

采用激光拉曼、阴极发光和电子探针技术,确认冀西北石榴角闪二辉麻粒岩锆石中保存早期高压变质包体矿物组合:石榴石(Grt)+单斜辉石(Cpx)+斜长石(Pl)+石英(Qtz)+金红石(Rt)、单斜辉石(Cpx)+斜长石(Pl)+石英(Qtz)和石榴石(Grt)+单斜辉石(Cpx)+斜长石(Pl)+石英(Qtz)。其中少量锆石具有继承性锆石的核,而多数锆石则形成于高压麻粒岩相变质阶段。利用TWQ方法限定石榴角闪二辉麻粒岩锆石中所保存的高压包体矿物组合的变质温度条件为750～820℃,压力为1.07～1.40 GPa。该项研究成果对于如何识别高压麻粒岩以及深入研究其成因机制均具有重要的科学意义。     

Ion Probe Study of Silicate Inclusions from Colomera (ⅡE) Iron Meteorite: the Rare Earth Element Perspective

Coupled with a petrographical study, I carried out an ion probe study of rare earth element microdistributions in mineral phases of silicate inclusions from the Colomera ⅡE iron meteorite. Most mineral grains have homogeneous REEs, but show considerable inter-grain variations by a factor of 2 to 100. The whole rock REE abundances for Colomera, estimated by combining REE data with modal abundances, are relatively LREE-enriched with REEs of -10'CI, which suggest that Colomera silicates were highly differentiated and might represent a low degree partial melt (-10%) of a chondritic source. REE geochemistry of Colomera silicate inclusions points to an origin that involves differentiation, dynamic mixing, remelting, reduction, recrystallization, and subsequent rapid cooling near the surface of a planetary body.     

Geological Characteristics and Model Ages of Marius Hills on the Moon

Marius Hills is a volcanic plateau on the nearside of the Moon.It is of great interest for its high concentration of volcanic features,including domes,cones,ridges,and rilles.However,the morphological and chronological characteristics of this plateau were not well studied due to the low resolution of early mission data.This study describes the detailed morphology of the volcanic features using the latest high spatial resolution images of the Terrain Camera(TC) onboard Selene-1(10 m/pix) and Narrow Angle Cam...     

Implementation of New OPAL Tables in Eggleton's Stellar Evolution Code

Based on previous works of OPAL, we construct a series of opacity tables for various metallicities Z=0, 0.000 01, 0.000 03, 0.000 1, 0.000 3, 0.001, 0.004, 0.01, 0.02, 0.03, 0.04, 0.05, 0.06, 0.08 and 0.1. These tables can be easily used in Eggleton's stellar evolution code in place of the old tables without changing the code. The OPAL tables are used for log10(T/K) > 3.95 and Alexander's for log10(T/K) < 3.95. At log10(T/K) = 3.95, the two groups' data fit well for all hydrogen mass fractions. Conductive opacities are included by reciprocal addition according to the formulae of Yakovlev and Urpin. A comparison of 1 and 5 M models constructed with the older OPAL tables of Iglesias and Rogers shows that the new opacities have most effect in the late stages of evolution, the extension of the blue loop during helium burning for intermediate-mass and massive stars.     

散射系数矩阵的计算及其应用

利用Gabor Daubechies（G? D）小波束域波场分解和传播在空间和方向上的双重局域性，提出了基于G? D小波束域叠前深度偏移进行角度域成像和计算局部散射系数矩阵的方法. 以简单分层模型为例，对不同探测系统的局部散射系数矩阵分布特征进行分析. 分析结果表明，在一定的探测系统几何布局下，由本文方法得到的局部散射系数矩阵能够较真实地反映局部结构的散射(或反射)特性. 通过局部散射系数矩阵进一步外推具有不同速度反差的水平界面随角度变化的反射系数，并估计界面的空间位置和倾角等说明局部散射系数矩阵的潜在应用.