太阳系早期的短寿期放射性核素

较详细地介绍全新的太阳系起源理论——X-wind模式,天体化学实验发现太阳系早期存在大量的短寿期放射性核素(半衰期小于100Ma),这些核素对太阳系的形成和演化有重要的影响,一种理论认为,这些核素是在恒星内部合成,并由星风注入原太阳分子云,星风产生的激波诱发分子云核的塌缩而形成原太阳,另一种理论认为,这些核素是高能粒子与原太阳分子云或太阳星云中的气体和尘埃相互作用的产物。     

准噶尔盆地中部1区块侏罗系三工河组油气输导特征分析

分析准噶尔盆地中部1区块侏罗系三工河组油藏输导格架构成及输导特征对油气分布的控制机制.研究区内砂岩输导层包括J1s12输导层及J1b1输导层,对2套输导层的分布及成因类型进行综合评价,认为J1s12砂体为区内主要输导层;将区内断裂体系划分为深层油源断裂与浅层层间断裂,前者是油气垂向输导的最主要通道,后者是油气向圈闭聚集的重要通道.结果表明:现今构造格局不是准中1区块岩性油气藏成藏控制因素,成藏期主要输导层J1s12古构造脊控制油气运移方向,油源断裂沟通的圈闭及输导层古构造脊上与层间断层沟通的圈闭是油气聚集的主要场所.     

The optical–infrared colour distribution of a statistically complete sample of faint field spheroidal galaxies

In hierarchical models, where spheroidal galaxies are primarily produced via a continuous merging of disc galaxies, the number of intrinsically red systems at faint limits will be substantially lower than in 'traditional' models where the bulk of star formation was completed at high redshifts. In this paper we analyse the optical–near-infrared colour distribution of a large flux-limited sample of field spheroidal galaxies identified morphologically from archival Hubble Space Telescope data. The I ₈₁₄− HK ' colour distribution for a sample jointly limited at I ₈₁₄<23 mag and HK '<19.5 mag is used to constrain their star formation history. We compare visual and automated methods for selecting spheroidals from our deep HST images and, in both cases, detect a significant deficit of intrinsically red spheroidals relative to the predictions of high-redshift monolithic-collapse models. However, the overall space density of spheroidals (irrespective of colour) is not substantially different from that seen locally. Spectral synthesis modelling of our results suggests that high-redshift spheroidals are dominated by evolved stellar populations polluted by some amount of subsidiary star formation. Despite its effect on the optical–infrared colour, this star formation probably makes only a modest contribution to the overall stellar mass. We briefly discuss the implications of our results in the context of earlier predictions based on models where spheroidals assemble hierarchically.     

Theoretical values for the [O iii] 5007/4959 line-intensity ratio and homologous cases

The magnetic-dipole probabilities for the ¹D₂–³P₂ and ¹D₂–³P₁ transitions in carbon-like and oxygen-like ions are calculated up to atomic number Z =12, including relativistic corrections to the magnetic dipole operator. The ratio of the probabilities for these two transitions is found to change by up to 5 per cent compared with previous theoretical work, none of which included these relativistic corrections, with the effect being largest for the near neutral ions. The transition probability ratio for the [O  iii ] 5007 and 4959 Å lines is found to be 3.01, implying an intensity ratio of 2.98, in significantly better agreement with the observed ratio than the earlier theoretical work.     

Three-dimensional calculations of high- and low-mass planets embedded in protoplanetary discs

We analyse the non-linear, three-dimensional response of a gaseous, viscous protoplanetary disc to the presence of a planet of mass ranging from 1 Earth mass (1 M_⊕) to 1 Jupiter mass (1 M_J) by using the zeus hydrodynamics code. We determine the gas flow pattern, and the accretion and migration rates of the planet. The planet is assumed to be in a fixed circular orbit about the central star. It is also assumed to be able to accrete gas without expansion on the scale of its Roche radius. Only planets with masses   M _p≳ 0.1 M_J  produce significant perturbations in the surface density of the disc. The flow within the Roche lobe of the planet is fully three-dimensional. Gas streams generally enter the Roche lobe close to the disc mid-plane, but produce much weaker shocks than the streams in two-dimensional models. The streams supply material to a circumplanetary disc that rotates in the same sense as the orbit of the planet. Much of the mass supply to the circumplanetary disc comes from non-coplanar flow. The accretion rate peaks with a planet mass of approximately 0.1 M_J and is highly efficient, occurring at the local viscous rate. The migration time-scales for planets of mass less than 0.1 M_J, based on torques from disc material outside the Roche lobes of the planets, are in excellent agreement with the linear theory of type I (non-gap) migration for three-dimensional discs. The transition from type I to type II (gap) migration is smooth, with changes in migration times of about a factor of 2. Starting with a core which can undergo runaway growth, a planet can gain up to a few M_J with little migration. Planets with final masses of the order of 10 M_J would undergo large migration, which makes formation and survival difficult.     

Amplification of primordial magnetic fields by anisotropic gravitational collapse

If a magnetic field is frozen into a plasma that undergoes spherical compression, then the magnetic field B varies with the plasma density ρ according to   B ∝ρ^2/3  . In the gravitational collapse of cosmological density perturbations, however, quasi-spherical evolution is very unlikely. In anisotropic collapses the magnetic field can be a much steeper function of gas density than in the isotropic case. We investigate the distribution of amplifications in realistic gravitational collapses from Gaussian initial fluctuations using the Zel'dovich approximation. Representing our results using a relation of the form   B ∝ρ^α  , we show that the median value of α can be much larger than the value  α= 2/3  resulting from spherical collapse, even if there is no initial correlation between magnetic field and principal collapse directions. These analytic arguments go some way towards understanding the results of numerical simulations.