射电源AO 0235＋164不同波段之间的相关时延分析及谱指数演化

详细介绍了由Edelson和Krolik提出的离散相关分析方法，该方法比较适合于因天文观测的不规则性而引起的时间分布不均匀的不同波段之间流量的相关分析，取两种极端的情况（完全相关和完全不相关）对该方法进行了测试，结果表明这是一种比较切实可行的方法。利用它，对AO0235＋164在4个波段上流量变化作相关性分析，结果表明，AO 0235＋164在5GHz,8GHz,14.5GHz和光学BI皮段的辐射之间存在着明显的相关性，高频波段的流量变化早于低频波段的流量变化，表明这些波段的辐射（从射电到光学）可能来源于相同的辐射机制，或者辐射是相关的，另外发现，谱指数随着时间而发生变化，这种变化在5GHz 8GHz和14．5GHz之间多表现为逆谱的形式，种种迹象表明AO 0235 164的射电爆发可能是和激波的形成有关，多波段的频谱分析和频谱演化研究可能是揭示这种关系的有效途径。     

Light variations in the candidate for protoplanetary objects HD 179821=V1427 Aql in 1899–1999

We present photoelectric and photographic observations of the supergiant HD 179821 with a large infrared excess, a candidate for protoplanetary objects. Over, ten years of our UBV observations, the star exhibited semiregular light variations with amplitudes $\Delta V = 0\mathop .\limits^m 10$ , $\Delta B = 0\mathop .\limits^m 15$ , and $\Delta U = 0\mathop .\limits^m 25$ , as well as systematic color and light variations. From 1990 until 1996, the yearly mean U-B and B-V color indices decreased by 0.25 and 0.15, respectively. After 1996, the motion of the star in the two-color (B-V)-(U-B) diagram upward and to the left slowed down. The color excess that we derived from our observations, by assuming that the star’s spectral type was F3 I in the 1990s, is E(B-V)=1.0. The photographic observations of HD 179821 from 1899 until 1989 show that its brightness m _pg generally increased while significantly fluctuating. An analysis of the observational data suggests that HD 179821 is most likely a post-AGB star of intermediate or low mass.     

The Visual Light Curve Of C/1995 O1 (Hale-Bopp) From Discovery To Late 1997

We present a light curve of C/1995 O1 (Hale-Bopp) compiledfrom more than 3000 visual observations of the comet made by members of the The Astronomer Group world-wide. These observations cover the period from discovery through to the end of 1997. The light curve shows that the rate of brightening of the comet varied widely at different times, with rapid rates of brightening at high heliocentric distance pre-perhelion and a comparably rapid post-perihelion fade. There is no evidence that the comet was suffering a large photometric outburst when first discovered, although a small outburst can be identified at perihelion. At least five difficult brightening regimes can be identified in the light curve between discovery and perihelion. From 2.5 AU to perihelion the rate of brightening with decreasing heliocentric distance was typical for “fairly” new comets(n ∼ 3.5, where “n” is the power law exponent of the heliocentric distance), although this was preceded by a period of very slow brightening with n ∼ 1 from r ∼ 4.0 AU to r ∼ 2.8 AU and followed by an initially more rapid brightening which appears to be related to the on-set of rapid water sublimation activity. We derive the light curve parameters at different stages of the comet's apparition. This revised version was published online in July 2006 with corrections to the Cover Date.     

On the dynamic efficiency of internal shocks in magnetized relativistic outflows

We study the dynamic efficiency of conversion of kinetic-to-thermal/magnetic energy of internal shocks in relativistic magnetized outflows. We model internal shocks as being caused by collisions of shells of plasma with the same energy flux and a non-zero relative velocity. The contact surface, where the interaction between the shells takes place, can break up either into two oppositely moving shocks (in the frame where the contact surface is at rest), or into a reverse shock and a forward rarefaction. We find that for moderately magnetized shocks (magnetization  σ≃ 0.1  ), the dynamic efficiency in a single two-shell interaction can be as large as 40 per cent. Thus, the dynamic efficiency of moderately magnetized shocks is larger than in the corresponding unmagnetized two-shell interaction. If the slower shell propagates with a sufficiently large velocity, the efficiency is only weakly dependent on its Lorentz factor. Consequently, the dynamic efficiency of shell interactions in the magnetized flow of blazars and gamma-ray bursts is effectively the same. These results are quantitatively rather independent on the equation of state of the plasma. The radiative efficiency of the process is expected to be a fraction   f _r < 1  of the estimated dynamic one, the exact value of f _r depending on the particularities of the emission processes which radiate away the thermal or magnetic energy of the shocked states.     

Evolution of optical spectral index and variability properties of S5 0716+714

We analyze the spectral variability and spectral evolution in the optical energy region by using multiband (BVRI) optical observations of S5 0716+714 spanning 1994 to 2005. The spectrum hardens when the source becomes brighter, which is consistent with general BL Lac objects. The spectral evolution parameter implies that the spectral variability is small in optical bands over 10 years. A simple model representing the variability of a synchrotron component can explain the spectral changes. In addition, we em...     

Dust Activity in Comet Hale-Bopp

Earth, Moon, and Planets - Comet Hale-Bopp has shown an extremely elevated level of dust activity during its apparition. We examine the dust activity of the comet, particularly the dust jets which...     

面向全空间信息系统的多粒度时空对象数据模型描述框架

全空间信息系统是一种面向从微观到宏观的动态复杂世界的空间信息系统,其理论基础是多粒度时空对象数据模型。为了确定多粒度时空对象数据模型的具体内容,需要确定描述多粒度时空对象特征的基本框架;为了开展多粒度时空对象的实际建模,需要明确多粒度时空对象数据模型的建模过程。为此,本文首先从数据模型、数据管理、可视化、空间分析和实际应用5个方面,分析了全空间信息系统与传统GIS的联系与区别,从空间范畴、动态变化、复杂关系、认知与行为、可视化技术、时空大数据分析6个方面,分析了传统GIS空间数据模型存在的不足;在此基础上,提出了多粒度时空对象的多粒度、多类型、多形态、多参照系、多元关联、多维动态、多能自主7个特点,确定了由时空参照、空间位置、空间形态、组成结构、关联关系、认知能力、行为能力和属性特征8项内容构成的多粒度时空对象数据模型描述框架;最后在分析了传统GIS空间数据模型建模过程的基础上,提出了多粒度时空对象数据模型的建模过程和思路。     

全空间下并行矢量空间分析研究综述与展望

新一代并行空间分析将面临空间大数据分析和实时空间分析服务的挑战。矢量空间计算作为GIS系统中的重要组成部分,在并行化算法设计中存在负载不均,并行扩展性差,IO性能低等技术瓶颈。本文首先从应用需求和技术发展的演变历史回顾了矢量空间分析算法发展过程;然后,从研究现状的角度详细阐述了并行矢量空间分析计算的研究成果,总结了并行空间分析算法的算法特征和技术瓶颈,对不同并行编程模型进行了对比,并提出了并行空间分析算法的研发流程;最后,从发展前景的角度预测了全空间信息系统中基于多粒度时空对象的空间数据模型和计算方法的发展趋势,提出了以内存计算等技术实现存算一体化的新型空间数据模型和分析方法的技术趋势。     

A general relativistic effect in quasi-spherical objects as the possible origin of relativistic jets

Based on recently reported results, we present arguments indicating that sign changes in proper acceleration of test particles on the symmetry axis and close to the r=2M surface of quasi-spherical objects—related to the quadrupole moment of the source—might be at the origin of relativistic jets of quasars and micro-quasars.     

Properties of BL Lac Objects with Redshift≤0.2

1 INTRODUCTIONBlazars, including BL Lacertae objects and Optical Violently Variable (OVV) quasars,belong to a class of active ga1actic nuclei (AGNs), the spectrum of which is dominated bynontherma1 radiation from re1ativistic electrons in jets pointing at us (e.g. BlandfOrd & Rees1978; Urry & Padovani 1995). The entire electromagnetic spectraI energy distributions (SEDs)usually reveal two broad components, the low energy part, peaking in the IR to soft X-rayrange, and the high en…