Weighing the cusp at the Galactic Centre

As stars close to the galactic centre have short orbital periods it has been possible to trace large fractions of their orbits in the recent years. Previously the data of the orbit of the star S2 have been fitted with Keplerian orbits corresponding to a massive black hole (MBH) with a mass of M_BH = 3–4 × 10⁶M_⊙ implying an insignificant cusp mass. However, it has also been shown that the central black hole resides in a ∼1″ diameter stellar cluster of a priori unknown mass. In a spherical potential which is neither Keplerian nor harmonic, orbits will precess resulting in inclined rosetta shaped trajectories on the sky. In this case, the assumption of non‐Keplerian orbits is a more physical approach. It is also the only approach through which cusp mass information can be obtained via stellar dynamics of the cusp members. This paper presents the first exemplary modelling efforts in this direction. Using positional and radial data of star S2, we find that there could exist an unobserved extended mass component of several 10⁵M_⊙ forming a so‐called ‘cusp’ centered on the black hole position. Considering only the fraction of the cusp mass Mequation/tex2gif-inf-4.gif within the apo‐center of the S2 orbit we find as an upper limit that Mequation/tex2gif-inf-6.gif/(M_BH + Mequation/tex2gif-inf-9.gif) ≤ 0.05. A large extended cusp mass, if present, is unlikely to be composed of sub‐solar mass constituents, but could be explained rather well by a cluster of high M/L stellar remnants, which we find to form a stable configuration. (© 2005 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

极隙区纬度Pc1-2波的统计分布特征

利用南极中山站和戴维斯站观测的感应式磁力计数据,运用互谱分析方法统计分析了2004年3、6、9、12月的Pc1-2波事件,研究了Pc1-2波出现频次、中心频率和振幅对季节和磁地方时的分布。结果共获得有效Pc1-2波事件2932件,其中,出现在3、9月较多,分别占51.4%和26.1%,12月次之,占18.6%,6月最少,占3.8%。两站的Pc1-2波事件有59.8%出现在磁中午(0800—1000 UT)附近,且在午后靠近磁中午的时候Pc1-2波的中心频率比在午前靠近磁中午的时候大,振幅则在0800 UT时出现最大值;此外,在6月,Pc1-2波的平均中心频率最大,而平均振幅则最小。这些结果表明,极隙区纬度Pc1-2波的传播在很大程度上受电离层电导率的影响。     

磁层顶日下点距离R0与磁暴Dst指数的相关性

利用2004—2006年ACE、WIND卫星观测的太阳风数据和相应时期反映磁暴大小的〖WTB1X〗D〖WTB1〗st指数,针对200个不同级别的磁暴事件,分析了磁层顶日下点距离〖WTB1X〗R0与磁暴D〖WTB1〗st指数的线性相关性。分析显示,在极端太阳风条件下,〖WTB1X〗D〖WTB1〗st指数时间序列比借助于Chao Model计算出的磁层顶日下点距离〖WTB1X〗R〖WTB1〗0的时间序列延迟了约3 h。经修正时间延迟后,对磁层顶日下点距离〖WTB1X〗R0与磁暴D〖WTB1〗st指数的线性相关性进行分析。结果表明:发生超级磁暴时,二者线性相关系数的均值为077;大磁暴时,线性相关系数的均值为074;中等磁暴时,线性相关系数的均值为047。此外,用最小二乘数据拟合得到了不同级别磁暴时的〖WTB1X〗R0 D〖WTB1〗st关系图。     

海滩近岸带中尺度地形动力过程研究进展

海滩近岸带中尺度地形动力过程是海岸海洋科学研究的重要研究内容之一.近20年来该领域发展较快,取得了一些重要的成果.对近岸带中尺度地形动力过程的碎波带地形与沙坝、冲流带地形与滩角、海滩风暴响应、观测技术手段等主要领域的进展进行了总结和评述,并对我国海滩研究提出要从加强观测手段和制定长期观测计划两方面来加强的建议.     

突变理论在地震资料解释异常地质体中的应用

阐述了尖点突变理论,建立了地震信号尖点突变模型并转化为尖点突变的标准形式,在时间域内提取突跳势、突跳时间;在频率域内提取突跳势、突跳次数等参数.运用突变理论对实际地震资料进行薄煤带的解释表明:突跳参数曲线上异常的位置与异常地质体边界的位置有关,为地震资料解释异常地质体提供了一种新的途径.     

基于监控量测数据的隧道失稳分析

利用监控量测数据,结合灰色理论建立隧道洞身位移变形系统。采用尖点突变分析方法,对开挖过程中初支结构的稳定性进行分析,建立隧道塌方预测模型。通过杜家山隧道发生的塌方事故与预测模型进行验证,得出塌方预测结果与实际情况相吻合;说明建立的隧道塌方预测模型是有效的,可以用来指导该类隧道的施工。     

岩体演化的非线性动力学模型与稳定性分析

以时间序列为基础,应用支持向量机建立岩体演化的非线性动力学模型,依据Lyapunov指数给出最长可预报时间,并通过函数拟合、变量代换将其化为标准的尖点突变模型,利用突变理论对其进行稳定性分析。结果表明,该模型预测效果理想,并具有良好的推广能力。     

Perturbations of the upper atmosphere in the cleft region

In the dayside polar region—loosely referred to as the cleft region—particle precipitation and Joule heating cause significant perturbations of the upper atmosphere. Here Dynamics Explorer-2 satellite data are used to present a synopsis of these disturbance effects. Documented are an increase in electron temperature and a decrease in electron density; increases in ion drift speed and ion temperature; an increase in the upward-directed ion velocity; increases in zonal wind speed and neutral gas temperature; and changes in the neutral gas composition and mass density. It is suggested that the increase in electron temperature is partly controlled by the decrease in electron density; that the ion upflow velocity mainly depends on the electron temperature, less frequently on the ion temperature; and that the observed decrease in thermospheric mass density is due to a decrease in the atomic oxygen density, which in turn is caused by diverging wind flows.     

The Auroral Station in Adventdalen, Svalbard

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Interplanetary Shocks, Magnetopause Boundary Layers and Dayside Auroras: The Importance of a Very Small Magnetospheric Region

Dayside near-polar auroral brightenings occur when interplanetary shocks impinge upon the Earth's magnetosphere. The aurora first brightens near local noon and then propagates toward dawn and dusk along the auroral oval. The propagation speed of this wave of auroral light is 10 km s^-1 in the ionosphere. This speed is comparable to the solar wind speed along the outer magnetosphere. The fundamental shock-magnetospheric interaction occurs at the magnetopause and its boundary layer. Several physical mechanisms transferring energy from the solar wind directly to the magnetosphere and from the magnetosphere to the ionosphere are reviewed. The same physical processes can occur at other solar system magnetospheres. We use the Haerendel (1994) formulation to estimate the acceleration of energetic electrons to 50 keV in the Jovian magnetosphere/ionosphere. Auroral brightenings by shocks could be used as technique to discover planets in other stellar systems.