Optical colors of 56 near-Earth objects: trends with size and orbit

We present the results of BVRIZ photometry of 56 near-Earth objects (NEOs) obtained with the 1-m Jacobus Kapteyn telescope on La Palma during 2000 and 2001. Our sample includes many NEOs with particularly deep 1-μm pyroxene/olivine absorption bands, similar to Q-type asteroids. We also classify three NEOs with particularly blue colors. No D-type asteroids were found, placing an upper limit of ∼2% on the fraction of the NEO population originating in the outer main belt or the Trojan clouds. The ratio of dark to bright objects in our sample was found to be 0.40, significantly higher than current theoretical predictions. As well as classifying the NEOs, we have investigated color trends with size and orbit. We see a general trend for larger silicate objects to have shallower absorption bands but find no significant difference in the distribution of taxonomic classes at small and large sizes. Our data clearly show that different taxonomic classes tend to occupy different regions of (a, e) space. By comparing our data with current model predictions for NEO dynamical evolution we see that Q-, R-, and V-type NEOs tend to have orbits associated with “fast track” delivery from the main belt, whereas S-type NEOs tend to have orbits associated with “slow track” delivery. This outcome would be expected if space weathering occurs on time scales of >10⁶ years.     

Probing the physics of interacting galaxies

The morphological and velocity structures in the gaseous (HI and CO) and stellar components of two interacting systems are examined. Both Arp 140 and Arp 104 reveal extended tidal tails in the HI. The Hα and FIR fluxes of Arp 140 yield similar SFR of ∼ 0.8 M_⊙ yr^-1. In contrast the Hα flux of Arp 104 yields a SFR of ∼ 0.05 M_⊙ yr^-1, ∼ 20 times smaller than that obtained from the FIR flux. Spectra were used to examine the changing velocity of atomic and molecular gas in NGC 5218 (Arp 104). The atomic and molecular gas were found to be dynamically similar with comparable velocities and velocity widths across the galaxy; consistent with the two phases responding similarly to the interaction, or enhanced HI to CO conversion in the centre of the galaxy. This revised version was published online in August 2006 with corrections to the Cover Date.     

Characterization of zonal winds in the stratosphere of Titan with UVES

Titan has been observed with UVES, the UV-Visual Echelle Spectrograph at the Very Large Telescope, with the aim of characterizing the zonal wind flow. We use a retrieval scheme originally developed for absolute stellar accelerometry [Connes, P., 1985. Astrophys. Space Sci., 110, 211-255] to extract the velocity signal by simultaneously taking into account all the lines present in the spectrum. The method allows to measure the Doppler shift induced at a given point by the zonal wind flow, with high precision. The short-wavelength channel (4200-5200 Å) probes one scale height higher than the long-wavelength one (5200-6200 Å), and we observe statistically significant evidence for stronger winds at higher altitudes. The results show a high dispersion. Globally, we detect prograde zonal winds, with lower limits of 62 and 50 m s⁻¹ at the regions centered at 200 and 170 km altitude, but approximately a quarter of the measurements indicates null or retrograde winds.     

Short-lived asteroids in the 7/3 Kirkwood gap and their relationship to the Koronis and Eos families

A population of 23 asteroids is currently observed in a very unstable region of the main belt, the 7/3 Kirkwood gap. The small size of these bodies—with the notable exception of (677) Aaltje (∼30 km)—as well as the computation of their dynamical lifetimes (3<T_D<172 Myr) shows that they cannot be on their primordial orbits, but were recently injected in the resonance. The distribution of inclinations appears to be bimodal, the two peaks being close to 2° and 10°. We argue that the resonant population is constantly being replenished by the slow leakage of asteroids from both the Koronis (I∼2°) and Eos (I∼10°) families, due to the drift of their semi-major axes, caused by the Yarkovsky effect. Assuming previously reported values for the Yarkovsky mean drift rate, we calculate the flux of family members needed to sustain the currently observed population in steady state. The number densities with respect to semi-major axis of the observed members of both families are in very good agreement with our calculations. The fact that (677) Aaltje is currently observed in the resonance is most likely an exceptional event. This asteroid should not be genetically related to any of the above families. Its size and the eccentricity of its orbit suggest that the Yarkovsky effect should have been less efficient in transporting this body to the resonance than close encounters with Ceres.     

拉萨地体东南缘的多期深熔作用及动力学

位于青藏高原班公湖-怒江蛇绿岩带与印度-雅鲁藏布江蛇绿岩带之间拉萨地体东南缘的前寒武纪结晶基底经历了角闪岩相-麻粒岩相区域变质作用和强烈的混合岩化.研究区可识别出两期深熔作用,第一期为斜长角闪岩部分熔融形成的花岗闪长岩脉体,其与围岩一起发生了变质与变形再造,转变成了黑云斜长片麻岩.第二期为含夕线石石榴石片麻岩部分熔融形成的含石榴石斜长石花岗岩脉体.岩石化学成分显示,第一期深熔脉体具有埃达克岩的典型地球化学特征,其SiO2=63.81%,Al2O3=16,92%,MgO=1.86%,Na2O=4.22%,K2O=1.81%,K2O/Na2O=0.43,并显示出LREE富集、无Eu异常的BEE配分模型,同时明显富Sr(366×10-6),贫Y(12×10-6)和Yb(0.4×10-6),Sr/Y=30.舍石榴石斜长石花岗岩主要由斜长石、石英和石榴石组成,含少量白云母和黑云母,其全岩SiO2=71.14%,Al2O3=14.26%,K2O=0.26%,Na2O=2.79%.CaO=2.94%.过铝指数A/CNK=1.40,为典型的过铝花岗岩.黑云斜长片麻岩脉体中的大多数锆石具有同心韵律状结晶环带和较高的Th//U比值(0.433～1.167),为典型的岩浆结晶锆石.锆石岩浆结晶域U-Pb原位定年给出了64.0±1.0Ma(MSWD=8.7)加权平均年龄;个别锆石变质交生边给出了27.9 Ma的谐和年龄,同时具有较低的Th/U比值(0.019),应代表后期叠加的变质热事件年龄.含石榴石斜长石花岗岩中的锆石均发育同心韵律状环带,而且具有较高的Th/U比值(0.196～1.212).所获得的谐和年龄在27.0～34.1Ma之间(加权平均年龄为29.3±0.9 Ma),应代表过铝花岗岩的结晶年龄.因此,我们认为拉萨地体东南缘变质基底在古近纪经历了两期深熔作用,第一期发生在约65Ma,在特提斯洋壳俯冲和印度板块与拉萨地体碰撞的动力学体制下,拉萨地体下地壳加厚和升温,发生了麻粒岩相变质和部分熔融,形成了埃达克岩质的花岗闪长岩浆;第二期混合岩化作用发生在约30Ma,在印度板块与拉萨地体碰撞后伸展的动力学体制下,高角闪岩相泥质变质岩中的含水矿物脱水熔融形成了过铝质花岗闪长岩浆.     

How tides and river flows determine estuarine bathymetries

For strongly tidal, funnel-shaped estuaries, we examine how tides and river flows determine size and shape. We also consider how long it takes for bathymetric adjustment, both to determine whether present-day bathymetry reflects prevailing forcing and how rapidly changes might occur under future forcing scenarios.Starting with the assumption of a 'synchronous' estuary (i.e., where the sea surface slope resulting from the axial gradient in phase of tidal elevation significantly exceeds the gradient in tidal amplitude ), an expression is derived for the slope of the sea bed. Thence, by integration we derive expressions for the axial depth profile and estuarine length, L, as a function of and D, the prescribed depth at the mouth. Calculated values of L are broadly consistent with observations. The synchronous estuary approach enables a number of dynamical parameters to be directly calculated and conveniently illustrated as functions of and D, namely: current amplitude Û, ratio of friction to inertia terms, estuarine length, stratification, saline intrusion length, flushing time, mean suspended sediment concentration and sediment in-fill times.Four separate derivations for the length of saline intrusion, L_I, all indicate a dependency on (U_o is the residual river flow velocity and f is the bed friction coefficient). Likely bathymetries for `mixed' estuaries can be delineated by mapping, against and D, the conditions L<sub>I</sub>/L<1,E<sub>X</sub>/L<1 (E<sub>X</sub> is the tidal excursion) alongside the Simpson-Hunter criteria D/U<sup>3</sup><50 m<sup>−2</sup> s<sup>3</sup>. This zone encompasses 24 out of 25 `randomly' selected UK estuaries.However, the length of saline intrusion in a funnel-shaped estuary is also sensitive to axial location. Observations suggest that this location corresponds to a minimum in landward intrusion of salt. By combining the derived expressions for L and L_I with this latter criterion, an expression is derived relating D_i, the depth at the centre of the intrusion, to the corresponding value of U_o. This expression indicates U_o is always close to 1 cm s⁻¹, as commonly observed. Converting from U_o to river flow, Q, provides a morphological expression linking estuarine depth to Q (with a small dependence on side slope gradients).These dynamical solutions are coupled with further generalised theory related to depth and time-mean, suspended sediment concentrations (as functions of and D). Then, by assuming the transport of fine marine sediments approximates that of a dissolved tracer, the rate of estuarine supply can be determined by combining these derived mean concentrations with estimates of flushing time, F_T, based on L_I. By further assuming that all such sediments are deposited, minimum times for these deposition rates to in-fill estuaries are determined. These times range from a decade for the shortest, shallowest estuaries to upwards of millennia in longer, deeper estuaries with smaller tidal ranges.     

上海潮滩沉积物重金属的动力学累积特征

１９９３年７－８月，在上海长江口南岸和杭州湾北岸淤泥质潮滩不同地貌部位，采集表层沉积物和柱状沉积物样品，采用筛析法，离心法、火焰原子吸收法，＾２１０Ｐｂ法等分别对沉积物粒度、重金属总量，不同粒级重金属含量以及沉积速率等进行了和测定。结果表明，潮滩沉积物重金属的空间分布格局并不受沿岸排污的直接影响，而与沉积动力作用密切相关。在水动力条件较弱的淤涨岸段和高潮滩部位，伴随着细颗粒起泥沙的大量堆积，Ｃｕ，     

地形摩擦对台风移动的影响

本文从动力学的角度研究了台风流场与台风运动的关系,在实际预报中考虑地形摩擦改变的流场对台风移动的影响取得了明显的效果。     

莱州湾海湾扇贝养殖区海水中悬浮颗粒的动态变化

1997年10月和1998年6月，在莱州湾两个主要海湾扇贝养殖区－芙蓉岛海区和金城海区，各定点进行了24h连续观测和取样，并在实验室内分析了总颗粒物（TPM）、颗粒有机物（POM）和叶绿素α的含量。结果表明，6月份金城海区的颗粒有机物和叶绿素α的含量均高于荚蓉岛海区；在10月份，芙蓉岛海区颗粒有机物的含量高于金城海区，但其叶绿素α的含量却低于金城海区，表明金城海区颗粒有机物的质量高于芙蓉岛海区。     

An integrable case of a rotational motion analogous to that of Lagrange and Poisson for a gyrostat in a Newtonian force field

The scope of the present paper is to provide analytic solutions to the problem of the attitude evolution of a symmetric gyrostat about a fixed point in a central Newtonian force field when the potential function isV ⁽²⁾.We assume that the center of mass and the gyrostatic moment are on the axis of symmetry and that the initial conditions are the following: (t ₀)=₀, (t ₀)=₀, (t ₀)=(t ₀)=₀, ₁(t ₀)=0, ₂(t ₀)=0 and ₃(t ₀)= ₃ ⁰ .The problem is integrated when the third component of the total angular momentum is different from zero (B ₁ 0). There now appear equilibrium solutions that did not exist in the caseB ₁=0, which can be determined in function of the value ofl ₃ ^r (the third component of the gyrostatic momentum).The possible types of solutions (elliptic, trigonometric, stationary) depend upon the nature of the roots of the functiong(u). The solutions for Euler angles are given in terms of functions of the timet. If we cancel the third component of the gyrostatic momentum (l ₃ ^r =0), the obtained solutions are valid for rigid bodies.