空间碎片与空间环境

空间碎片起源于人类的航天活动,目前空间碎片的空间密度已经对航天器的安全造成威胁,且其数量仍在高速增长,已成为一个引人瞩目的环境问题,航天器受空间碎片撞击的事件时有发生。大空间碎片的撞击会使航天器姿态和轨道发生改变,更严重的是会导致航天器破损甚至完全解体;小空间碎片的撞击会使航天器表面性能改变,部分器件损伤或失效,使航天器丧失功能。目前地基设备只能对厘米级及更大的碎片进行观测、跟踪和编目,航天器可以根据空间碎片的轨道参数进行规避和机动飞行,以避免撞毁;小空间碎片(<1cm)数量众多,但无法进行轨道测量,只能通过天基直接探测和样品回收获得数据,数值建模和超高速撞击模拟实验是进行小空间碎片风险评估和撞击效应研究的有效方法。对小空间碎片只能采取被动防护的方法,在航天器总体设计、防护结构和材料方面着手,降低空间碎片的威胁。改善空间环境,减少空间碎片的最根本方法是对航天器采取钝化措施,减少空间碎片的产生,理论上还可以采取措施,清扫、清除或回收空间碎片。     

Chemical Classification of Space Debris

Space debris, here referring to all non-operating orbital objects, has steadily increased in number so that it has become a potential barrier to the exploration of space. The ever-increasing number of space debris pieces in space has created an increasingly threatening hazard to all on-the-orbit spacecraft, and all future space exploration activities have to be designed and operated with respect to the increasing threat posed by space debris. Generally, space debris is classified as large, medium and small debris pieces based on their sizes. The large debris piece is easily catalogued, but medium to small debris pieces are very difficult to track and also quite different in damage mechanisms from the large ones. In this paper, a scheme of chemical classification of space debris is developed. In our scheme, the first-order classification is employed to divide space debris into two groups: natural     

Analyzing the brightness distributions of the components of eclipsing variables using precise photometric data

We present the results of numerical simulations aimed at studying ways to analyze the brightness distributions of eclipsing-binary components from the high-precision photometric data that will be provided by the planned specialized orbital COROT and Kepler missions. We consider a simple model of an eclipsing binary with spherical components in circular orbits, with a linear limb-darkening law. We fit the light curves using a non-linear model with limb-darkening coefficients, as well as without placing stringent constraints on the shapes of the distributions. Our estimates demonstrate that, if the uncertainties in the measured light curves become as low as 10^?4 (a factor of ten better than the precision of ground-based photometry), the limb-darkening coefficients can be found with a relative uncertainty of 0.01. The uncertainties of the restored brightness distributions across the stellar disks are approximately the same.     

An ontological architecture for orbital debris data

The orbital debris problem presents an opportunity for international cooperation toward the mutually beneficial goals of orbital debris prevention, mitigation, remediation, and improved space situational awareness (SSA). Achieving these goals requires sharing orbital debris and other SSA data. Toward this, I present an ontological architecture for the orbital debris and related domains, taking steps in the creation of an orbital debris ontology. The purpose of the ontology is to capture general scientific domain knowledge; formally represent the entities within the domain; form, structure, and standardize (where needed) orbital and SSA terminology; and foster semantic interoperability and data-exchange. In doing so I hope to offer a scientifically accurate ontological representation of the orbital domain; contribute to research in astroinformatics, space ontology, and space data management; and improve spaceflight safety by providing a means to capture and communicate informaiton associated with space debris.     

Multifactorial Method of Search for Small Bodies in Close Orbits

The results of the search for Apollo, Amor, and Aten asteroids with the orbits close to those of meteoroids of the δ-Cancrids meteor complex (code DCA), which consists of the northern (code NCC) and southern (code SCC) branches, are presented. The search for small bodies in close orbits was performed on the basis of a multifactorial method of combining several criteria: Drummond orbital similarity criterion, Kholshevnikov metric, and parameters of the dynamic evolution of the orbits using two catalogs of meteor orbits (Japan Meteor Society, SonatoCo, and CAMS Meteoroid Orbit Database v2.0, CAMS) obtained from television observations. Asteroids in close orbits with the meteoroid orbits of the northern NCC and southern SCC branches of the δ-Cancrids are identified only in the Apollo group. The following asteroids are common for the NCC and SCC branches: 2015 PU228, 2014 YQ34, 2017 YO4 (according to the CAMS orbit catalog); Hephaistos 1978 SB, 2003 RW11, 2006 BF56, 2011 SR12, 2014 RS17, 2001 YB5 (SonatoCo catalog). The asteroid 85182 (1991 AQ) is identified only with the northern NCC branch but in two catalogs of meteor orbits.     

Sub-parsec structure of binary supermassive black holes in active galactic nuclei

Long-term, multi-frequency monitoring of the radio fluxes of the four BL Lac objects 3C 120, OJ 287, 1308+326, and BL Lac is considered. Harmonic components of the flux variability on scales from one year to decades are determined. The observational data used were obtained at the Radio Astronomy Laboratory of the Crimean Astrophysical Observatory (Ukraine) and the University of Michigan Radio Astronomy Observatory (USA). These data are used to construct kinematic models for active galactic nuclei using values for the orbital and precessional periods of binary systems consisting of supermassive black holes. The derived speeds of the companions in their orbits lie in the narrow range 3000–4000 km/s. The orbital radii for the binary supermassive black holes also lie in a narrow range, 10¹⁷–10¹⁸ cm, providing evidence that observed prominent examples of active galactic nuclei are fairly close binary systems. The parameters of the mediumin which the components of the binary systems are moving are estimated, as well as the rates at which the systems are losing orbital angular momentum and their lifetimes to coalescence.     

Interpretation of light curves of the cataclysmic variable OY Car in a model with shockless interaction between a gaseous stream and the disk

To determine the parameters of the accretion disk and shock-wave region responsible for the formation of the orbital peak in the light curve of the binary system OY Car (an SU UMa-type variable), we have analyzed its U BV R and JK light curves using two gas-dynamical models with different regions of shock interaction: one with a hot line along the stream from the Lagrange point L1 and one with a hot spot on the accretion disk. The hot-line model can better describe the quiescent state of the system: the maximum X² for the optical light curves does not exceed 207, whereas the minimum residual for the hot-spot model is X²>290. The shape of the eclipse is almost identical in both models; the main differences are in interpreting out-of-eclipse portions of the light curves, whose shape can varyin the transition from one orbital cycle to another. The hot-spot model is not able to describe variations of the system’s brightness at orbital phases ?～0.1–0.6. The rather complex behavior of the observed flux in this phase interval can be explained in the hot-line model as being due to variations of the temperature and size of the system. Based on the analysis of a sequence of 20 B curves of OY Car, we conclude that the flux variations in the primary minimum are due to variations of the luminosity of the accretion disk, whereas the flux variability in the vicinity of the orbital peak is due to the combined effect of the radiation of the disk and hot line. The JK light curves of OY Car in the quiescent state and during a small flare also indicate preference for the hot-line model, since the primaryminimum and the flux near quadratures calculated using the hot-spot model are not consistent with the observations.     

Orbits of four visual binaries determined from observations along short arcs

The orbits of the four visual binaries ADS 246 (GL 15), ADS 7724 (γ Leo), ADS 10386 (GJ 659), and ADS 14909 (1 Peg) have been determined using the apparent motion parameters (AMP) method. The orbital periods of these stars are 1200, 550, 7500, and 18 000 yr, respectively. The orbits were calculated based on observations along short arcs obtained with the 26-inch refractor of the Pulkovo Observatory and Hipparcos parallaxes, supplemented with radial-velocity measurements for the components of these pairs taken from the literature. All visual and photographic observations of these stars after 1830 from the WDS catalog have been taken into consideration. The new orbits of ADS 246 and ADS 7724 are compared with the orbits computed in other studies. The orbits of ADS 10386 and ADS 14909 have been determined for the first time. The orientation of the planes of the computed orbits in Galactic coordinates have also been calculated.     

Observable effects during gravitational microlensing of stars by NUT objects

We consider observable effects during the gravitational microlensing of stars of finite angular size with a given brightness distribution across their disks by exotic objects whose space-time environment is described with the NUT metric. We demonstrate that, under certain conditions, the microlensing light curves and chromatic effects due to the wavelength dependence of the disk brightness distributions can differ considerably from those observed for a Schwarzschild gravitational lens, so that their analysis can facilitate the identification of such objects.     

Subsystems of RR Lyrae variable stars in our Galaxy

We have used published, high-accuracy, ground-based and satellite proper-motion measurements, a compilation of radial velocities, and photometric distances to compute the spatial velocities and Galactic orbital elements for 174 RR Lyrae (ab) variable stars in the solar neighborhood. The computed orbital elements and published heavy-element abundances are used to study relationships between the chemical, spatial, and kinematic characteristics of nearby RR Lyrae variables. We observe abrupt changes of the spatial and kinematic characteristics at the metallicity [Fe/H]≈?0.95 and also when the residual spatial velocities relative to the LSR cross the critical value V _res≈290 km/s. This provides evidence that the general population of RR Lyrae stars is not uniform and includes at least three subsystems occupying different volumes in the Galaxy. Based on the agreement between typical parameters for corresponding subsystems of RR Lyrae stars and globular clusters, we conclude that metal-rich stars and globular clusters belong to a rapidly rotating and fairly flat, thick-disk subsystem with a large negative vertical metallicity gradient. Objects with larger metal deficiencies can, in turn, be subdivided into two populations, but using different criteria for stars and clusters. We suggest that field stars with velocities below the critical value and clusters with extremely blue horizontal branches form a spherical, slowly rotating subsystem of the protodisk halo, which has a common origin with the thick disk; this subsystem has small but nonzero radial and vertical metallicity gradients. The dimensions of this subsystem, estimated from the apogalactic radii of orbits of field stars, are approximately the same. Field stars displaying more rapid motion and clusters with redder horizontal branches constitute the spheroidal subsystem of the accreted outer halo, which is approximately a factor of three larger in size than the first two subsystems. It has no metallicity gradients; most of its stars have eccentric orbits, many display retrograde motion in the Galaxy, and their ages are comparatively low, supporting the hypothesis that the objects in this subsystem had an extragalactic origin.     

Rotations of elongate rigid particles in slow non-Newtonian flows

In Jeffery's well-known theoretical model each end of the symmetry axis of an isolated rigid prolate ellipsoid embedded in a Newtonian matrix undergoing simple shear flow describes one of an infinite family of accurately closed periodic orbits. The usefulness of this model in relating particle orientation distributions to bulk finite strain is reassessed in the light of recent theoretical and experimental work. This work shows that Jeffery's analysis is readily extended to include any axisymmetric particle shape (with a centre of symmetry), and that small surface irregularities may be neglected. In nonNewtonian media (both power-law and elasticoviscous) particle motions, although still periodic, show a progressive drift through the family of Jeffery orbits. In a secondorder Rivlin—Ericksen fluid the orbital drift estimated for the strain magnitudes and particle axis ratios likely in most tectonites is slight, and leads to negligibly small departures from the predictions of Jeffery's model. More orbital drift is anticipated in powerlaw fluids although Jeffery's model is still likely to yield an acceptable approximation except for very high strains.     

Observations of Near-Earth Optical Transients with the Lomonosov Space Observatory

The results of observations with the MASTER-SHOK robotic wide-field optical cameras onboard the Lomonosov Space Observatory carried out in 2016 are presented. In all, the automated transient detection system transmitted 22 181 images of moving objects with signal-to-noise ratios greater than 5 to the Earth. Approximately 84% of these images are identified with well-known artificial Earth satellites (including repeated images of the same satellite) and fragments of such satellites (space debris), according to databases of known satellites. The remaining 16% of the images are relate to uncatalogued objects. This first experience in optical space-based monitoring of near-Earth space demonstrates the high efficiency and great potential of using large-aperture cameras in space, based on the software and technology of the MASTER robotic optical complexes (the Mobile Astronomical System of TElescope- Robots (MASTER) global network of robotic telescopes of Lomonosov Moscow State University).     

A dynamical study of the wide hierarchic triple star ADS 10288

We have performed the first dynamical study of the relative motions of the components of the wide hierarchic triple star system ADS 10288 (GL 649.1 = WDS 16579+4722), based on a 15-year series of photographic observations with the 26″ Pulkovo refractor, supplemented with data from the WDS catalog, HIPPARCOS parallaxes, and radial velocities of the components. The radial velocities were measured in Simeiz using the ILS stellar radial-velocity correlation spectrometer designed by A.A. Tokovinin. We applied the parameters of the apparent motion technique, which makes it possible to derive a binary’s orbit and mass from observations of a short arc, about 5°–10° in length. We derived preliminary orbits for the pairs AB and (AB)-C, whose orbital periods are 340 and 64 000 years, respectively. Mass estimates derived from the mass-luminosity relation are consistent with our dynamical estimates. We determined the orientation of the orbits in Galactic coordinates. The orbital planes are not coplanar, and are steeply inclined to the Galactic plane, as was the case in our earlier studies for most wide visual pairs we have studied.     

Orbits of the visual binaries ADS 8814 and ADS 8065 from observations along a short arc

The orbits of the visual binaries ADS 8814 and ADS 8065 are determined for the first time. The orbits were calculated using the parameters of the apparent motion, based on position observations along short arcs obtained on the 26-inch refrector of the Pulkovo Observatory, supplemented with radial-velocity observations for the stellar components in both pairs obtained on the 1-m telescope of the Simeiz Section of the Crimean Astrophysical Observatory. All previous visual and photographic observations of these stars after 1832 were also taken into account. The orbit of ADS 8814 was refined using the differential-correction method. The orbital periods of these two stars are about 800 and 6000 years, respectively. The mass estimates derived for the known parallaxes from the Hipparcos catalog correspond to the spectral types of these stars. The polar vectors of the obtained orbits in Galactic coordinates are also given.     

泥石流阵流序列的整体性

泥石流往往以阵流群的形式出现,不同阵流参数具有统一的统计分布,意味着阵流序列隐含着深层的系统信息。文中根据蒋家沟泥石流观测数据,揭示阵流序列的自相关性和时空变化特征,进而确立其整体性。Hurst指数是刻画序列相关性的指标。阵流的流量、速度和时间间歇序列的Hurst指数值均大于05,从而证明序列具有长程相关性;另一方面,将阵流作为其运动参数(如流速、流量、间歇时间)组所确定的点,则一个泥石流事件为参数空间的一个点集,且集中在一个狭小区域,直观表现了阵流在时空的聚集特征,这是序列整体性的又一特征。阵流序列的这些基本特征,意味着不同泥石流事件背后隐藏着同一个动力学机制,即泥石流作为流域行为(而不是流体运动)的系统动力学。     

Analysis of the Sky Scanning Efficiency in the Lyra-B Space Experiment

The Lyra-B space experiment (SE) is a high-precision multicolor multiple all-sky photometric survey of stars and star-like objects. The experiment will be conducted from the Russian segment of the International Space Station (ISS). For this purpose, a 0.5-m telescope will be installed onboard (or, more precisely, outboard) the ISS, which will observe stars in a scanning mode. The Lyra-B SE was included in the program of scientific experiments at the ISS fairly long ago. At the beginning of the SE design it was thought that the ISS would exist “eternally” and the time needed for the full-fledged implementation of the experiment would be allocated. Today, however, the situation has changed. In 2025 the ISS will possibly cease to exist either as the space station as a whole or in the form in which it exists now. Hence there arises the problem to perform the entire volume of observations in a maximally short time, i.e., to find an optimal sky scanning strategy that would ensure a maximum duration of observations. In addition, we consider two related questions: with what density will the observations be distributed over the sky and how many times will a point in the sky fallen within the field of view of the Lyra-B telescope be observed in successive orbital revolutions? This question is important for investigating variable stars, determining the orbits and axial rotation periods of asteroids, and ensuring a specified photometric accuracy over the entire sky.     

The intermediate-age pre-cataclysmic variables SDSS J172406+562003 and RE J2013+4002

We have analyzed the physical status of the pre-cataclysmic variables SDSSJ172406+562003 and RE J2013+4002, which have evolved after their common-envelope stage a time t = 10⁶?10⁷ years. Spectroscopy and photometry of these systems were performed with the 6-m and 1-m telescopes of the Special Astrophysical Observatory. We demonstrate that emission lines in the spectra were formed solely by the reflection of radiation emitted by the white dwarfs on the surfaces of their cool companions, under conditions close to local thermodynamic equilibrium. These effects are also responsible for most of the objects?? photometric variability amplitude. However, comparing the light curves of SDSS 172406 from different epochs, we find aperiodic brightness variations, probably due to spottedness of the surface of the secondary. Jointly analyzing the spectra, radial-velocity curves, and light curves of the pre-cataclysmic variables and modeling the reflection effects, we have derived their fundamental parameters. We demonstrate that the secondaries in these systems are consistent with evolutionary models for main-sequence stars and do not have the luminosity excesses characteristic of cool stars in young pre-cataclysmic variables.     

四川盆地西缘早三叠世早期碳酸盐重力流沉积与环境

四川竹园坝?梨园里地区下三叠统飞仙关组地层中,碳酸盐砾屑沉积类型有:碎屑流和浊流;根据岩性组合可分三种组合层序:Ⅰ.碎屑流与半深水泥晶灰岩沉积组合层序;Ⅱ.碎屑流与浊流沉积组合层序;Ⅲ.复合层序?据重力流形成环境,计算了古斜坡坡度,测定了古流向,结合重力流形成及古构造?古地理演化,提出了区内碳酸盐重力流的演化及沉积模式?     

Structure of the circumbinary envelope around a young binary system

The structure of a circumstellar envelope around a young binary T Tauri star is considered. The supersonic orbital motion of the system components in the envelope gas leads to the formation of bow shocks around the star. Two- and three-dimensional numerical modeling indicates an important role of these shocks in the formation of the structure of the circumbinary envelope. In particular, for systems with circular orbits, the size of the central region of the envelope that is not filled with matter (the “gap”) is essentially determined by the parameters of the bow shocks. These modeling results are supported by comparisons of the obtained estimates for the gap parameters with observations.     

鄂尔多斯盆地西缘砾质冲积扇沉积学特征

晚三叠世鄂尔多斯西缘冲积扇沉积主要由碎屑流、颗粒流、片流及河道砾岩等组成。文中讨论了各类砾岩的沉积学特征,同时指出,不同成因的砾岩,其粒度分布曲线形态及某些粒度参数亦不同.据此本文提出了根据-系列新的粒度分布曲线形态和粒度参数Mdf,Rgs和Mdf/Rgs等甄别冲积扇中不同类型砾岩的设想。