Possible Suzaku detection of non-thermal X-ray signals from a rotating magnetized white dwarf

Although rotating neutron stars (NSs) have been regarded as being textbook examples of astrophysical particle acceleration sites for decades, details of the acceleration mechanism remain a mystery; for example, we cannot yet observationally distinguish “polar cap” models from “outer gap” models. To solve the model degeneracy, it is useful to study similar systems with much different physical parameters. Strongly magnetized white dwarfs (WDs) are ideal for this purpose, because they have essentially the same system geometry as NSs, but differ largely from NSs in the system parameters, including the size, magnetic field, and the rotation velocity, with the induced electric field expected to reach 10¹³–10¹⁴ eV. Based on this idea, the best candidate among WDs, AE Aquarii, was observed with the fifth Japaneses X-ray satellite, Suzaku. The hard X-ray detector (HXD) on-board Suzaku has the highest sensitivity in the hard X-ray band over 10 keV. A marginal detection in the hard X-ray band was achieved with the HXD, and was separated from the thermal emission. The flux corresponds to about 0.02% of its spin-down energy. If the signal is real, this observation must be a first case of the detection of non-thermal emission from WDs.     

Source investigation of impulsive He-rich particle events

We have investigated the source characteristic and coronal magnetic field structure of six impulsive solar energetic particle (SEP) events selected from Wang et al. [Wang, Y.-M., Pick, M., Mason, G.M. Coronal holes, jets, and the origin of ³He-rich particle events. ApJ 639, 495, 2006] and Pick et al. [Pick, M., Mason, G.M., Wang, Y.-M., Tan, C., Wang, L. Solar source regions for ³He-rich solar energetic particle events identified using imaging radio, optical, and energetic particle observations. ApJ 648, 1247, 2006]. Some results are obtained: first, 2 events are associated with wide (≈100°) CMEs (hereafter wide CME events), another 4 events are associated with narrow (?40°) CMEs (hereafter narrow CME events); second, the coronal magnetic field configuration of narrow CME events appear more simple than that of the wide CME events; third, the photospheric magnetic field evolutions of all these events show new emergence of fluxes, while one case also shows magnetic flux cancellation; fourth, the EUV jets usually occurred very close to the footpoint of the magnetic field loop, while meter type III bursts occurred near or at the top of the loop and higher than EUV jets. Furthermore, the heights of type III bursts are estimated from the result of the coronal magnetic field extrapolations.     

Active Region Dynamics

New methods of local helioseismology and uninterrupted time series of solar oscillation data from the Solar and Heliospheric Observatory (SOHO) have led to a major advance in our understanding of the structure and dynamics of active regions in the subsurface layers. The initial results show that large active regions are formed by repeated magnetic flux emergence from the deep interior, and that their roots are at least 50 Mm deep. The active regions change the temperature structure and flow dynamics of the upper convection zone, forming large circulation cells of converging flows. The helioseismic observations also indicate that the processes of magnetic energy release, flares and coronal mass ejections, might be associated with strong (1–2 km/s) shearing flows, 4–6 Mm below the surface.     

The hemispheric asynchrony of polar faculae during solar cycles 19–22

We investigate the north–south (N–S) asynchrony of the polar faculae and compare it with the hemispheric asynchrony of solar activity at low latitudes. We find that, (1) both the solar activity at high and low latitudes do not synchronously occur in the northern and southern hemispheres, there is phase shifts between the two hemispheres; (2) the N–S asynchrony of the polar faculae is a function of latitudes, implying that the asynchrony of the polar faculae between the two hemispheres is related to the hemispheric asymmetry and latitudinal distribution of the polar faculae.     

新一代空间交会对接光学成像敏感器

摘要： 为满足中国未来空间交会对接任务对光学成像敏感器工作能力尤其是杂光抑制能力的更高需求,研制新一代空间交会对接光学成像敏感器.该产品多项指标优于其上一代产品神舟八号CCD光学成像敏感器,测量距离由原来的150~2 m范围提升为250~0.9 m范围;目标捕获时间由10 s缩短为0.32 s;抗杂光干扰能力大幅提升,实现准全天候工作.该产品已在中国神舟十一号载人飞船、天舟一号货运飞船与天宫二号的交会对接任务中成功验证,可在后续更好地服务中国空间站、探月三期等工程的交会对接任务.介绍该产品的测量原理、系统组成、地面试验和在轨工作表现等情况,并给出相应结论.     

SSRT: First results of millisecond spike observations

We present the results of the first observations of spike-like phenomena with the Siberian Solar Radio Telescope (SSRT) in the one-dimensional mode at the frequency of 5.7 GHz with high spatial and temporal resolutions.     

ASAP: A systematic approach to plasma spectral synthesis

ASAP (Analysis System for Astrophysical Plasmas), developed at the Osservatorio Astronomico di Palermo, is a package of procedures based on IDL. It is aimed at the detailed presentation of theoretical models of astrophysical plasmas and the accurate comparison with observational data, up to fittings of specific observations. It is also useful for the prediction of specific observations, and for the simulation of the expected performances of forthcoming instruments, for instance those on board SOHO.     

摄影技术基础课程教学实践浅析

本文分析了我院开设摄影技术基础课程的背景，初步研究探讨了摄影课在本院的教学情况，指出摄影教学在我国大力提倡素质教育的今天，大有可为。我院现时大规模发展的同时，加强摄影教学具有现实意义。     

如何使大学英语课堂更具吸引力

本文探讨了学生上英语课的动机，教师在课堂教学中究竟起到什么作用。以及如何根据学生的要求，教师来充分展示英语课堂的魅力，使它富于变化，充满活力，把更多的学生吸引到课堂上来，改善学生的出勤率。     

反馈严格正实输出的充分必要条件

给出了多输入线性系统具有反馈严格正实输出的充分必要条件，由于这一条件用矩阵Ａ、Ｂ和Ｃ直接给出，所经检查比较方便。