The Role of Magnetic Reconnection in CME Acceleration

Observations carried out from the coronagraphs on board space missions (LASCO/SOHO, Solar Maximum and Skylab) and ground-based facilities (HAO/Mauna Loa Observatory) show that coronal mass ejections (CMEs) can be classified into two classes based on their kinematics evolution. These two classes of CMEs are so-called fast and slow CMEs. The fast CME starts with a high initial speed that remains more or less constant; it is also called the constant-speed CME. On the other hand, the slow CME starts with a low initial speed, but shows a gradual acceleration; it is also called the accelerated and slow CME. Low and Zhang [Astrophys. J. 564, L53–L56, 2002] suggested that these two classes of CMEs could be a result of a difference in the initial topology of the magnetic fields associated with the underlying quiescent prominences. A normal prominence magnetic field topology will lead to a fast CME, while an inverse quiescent prominence results in a slow CME, because of the nature of the magnetic reconnection processes. In a recent study given by Wu et al. [Solar Phys. 225, 157–175, 2004], it was shown that an inverse quiescent prominence magnetic topology also could produce a fast CME. In this study, we perform a numerical MHD simulation for CMEs occurring in both normal and inverse quiescent prominence magnetic topology. This study demonstrates three major physical processes responsible for destabilization of these two types of prominence magnetic field topologies that can launch CMEs. These three initiation processes are identical to those used by Wu et al. [Solar Phys. 225, 157–175, 2004]. The simulations show that both fast and slow CMEs can be initiated from these two different types of magnetic topologies. However, the normal quiescent prominence magnetic topology does show the possibility for launching a reconnection island (or secondary O-line) that might be thought of as a “CME’’.     

Near infrared studies of the massive X-ray binary 2S 0114+65

We present near-infrared spectroscopy of the massive X-ray binary 2S 0114+650. These observations covering the spectral range 1.08–2.35 μm span the region where Paschen and Brackett series recombination lines of hydrogen are expected to be seen, namely, Paβ , Brγ and Br 10–17 lines. The absence of any of these lines in emission supports earlier inferences that the optical component in 2S 0114+650 is unlikely to be a Be star but rather a B type supergiant. Near-IR photometry gives J = 8.78, H = 8.53 and K = 7.96; these values show marginal variations from earlier reported measurements.     

Keck observations of ROSAT ultra-luminous X-ray source candidates

We present results of optical follow-up observations of candidate ultra-luminous X-ray sources (ULXs). Using Keck optical spectroscopy, 17 of the candidates from the Colbert and Ptak [Colbert, E.J.M., Ptak, A.F. A catalog of candidate intermediate-luminosity X-ray objects. ApJS 143, 25–45, 2002] catalog have been identified; this is one of the largest sets of optical identifications of such objects thus far. Fifteen are background active galactic nuclei (AGN); two are foreground stars in our Galaxy. These findings are consistent with background and foreground object expectations, as derived from log N–log S relations. Also, the results are briefly discussed in terms of the spiral-galaxy/ULX connection.     

扇面波导中馈电探针输入电阻数值计算

推导出扇面波导中激励探针的等效输入电阻表达式，探针是伸入波导中的同轴线的内导体，在Ｘ波段，计算了输入电阻值随着探针伸入波导中不同长度的变化。     

高职高专院校建设数字化校园过程中应注意的问题

21世纪以来,数字化和信息化成为现代社会的主要标志。高职高专院校为了提高自己的管理水平,跟上时代的步伐,也都在着手数字化校园的建设。本文从数字化校园的基本概念入手,介绍数字化校园的组成、建设内容、建设步骤以及建设过程中应注意的问题,并给出了数字化校园的基本模型。     

Effects of the photo-ionized absorber on the continuum spectra of EXO 0748–676

We report on the analysis of XMM-Newton archival data of EXO 0748–676. We studied changes of the continuum spectra due to the presence of photo-ionized plasma on the line of sight. We show that the ionization degree of the plasma could change largely during the X-ray bursts and the dips. These changes can significantly modify the soft-band spectrum, which was in fact observed from EXO 0748–676. We discuss the effect of the photo-ionized plasma on the continuum spectra in comparison with a frequently used model such as partial covering absorption.     

弹簧杆校正原理及其在力矩控制系统中的应用

 为了掌握自动飞行器的工作特性,在它飞上空中之前,工程技术人员要在地面进行各种仿真试验。研制力矩控制系统的目的在于模拟随高度、速度变化且连续作用在飞行器翼面上的气动铰链力矩。这种装置广泛应用于各种型号舵机。 我们研制的力矩控制系统力案如图1所示。     

航行情报服务(AIS)及其属性初探

本篇首次运用情报的广义属性从理论上分析和概括了航行情报的定义、宗旨和有关性质,并给出了航行情报服务的流程图和交流图。对促进和加强这一学科的教学研究有一定的参考意义。     

模拟JJ—7飞机纵向摆动试飞研究

本文论述了BW-1变稳机空中飞行模拟H-7飞机发生两次纵向摆动时飞行状态特性,通过试飞研究其飞行品质,校核驾驶员诱发振荡(PIO)发生的可能性;并对解决PIO的方案进行了验证试飞研究,提出了排除PIO较适宜的参数值.试飞证明,空中飞行模拟试验是研究PIO的有效方法之一.     

低速壁压信息洞壁干扰修正方法两个重要的新改进

本文介绍了对美国洛克希德公司Hackett,J.E.等人研究的壁压信息洞壁干扰修正方法两个重要的新改进。建立了一个简便方法,消除了原方法必须要在模型下游测到壁压的渐近分布,才能进行准确修正的苛刻条件;建立了一个测压试验洞壁干扰的改进修正方法,使测压与测力试验的修正方法一致。文中给出了两组模型的验证结果。本文的两个新改进,消除了壁压信息法应用中的突出难关,不仅拓宽了应用,并大为提高了测力、测压试验洞壁干扰修正的准确性。