The Local Bubble and Interstellar Material Near the Sun

The properties of interstellar matter at the Sun are regulated by our location with respect to a void in the local matter distribution, known as the Local Bubble. The Local Bubble (LB) is bounded by associations of massive stars and fossil supernovae that have disrupted dense interstellar matter (ISM), driving low density intermediate velocity ISM into the void. The Sun appears to be located in one of these flows of low density material. This nearby interstellar matter, dubbed the Local Fluff, has a bulk velocity of ∼19 km s⁻¹ in the local standard of rest. The flow is coming from the direction of the gas and dust ring formed where the Loop I supernova remnant merges into the LB. Optical polarization data suggest that the local interstellar magnetic field lines are draped over the heliosphere. A longstanding discrepancy between the high thermal pressure of plasma filling the LB and low thermal pressures in the embedded Local Fluff cloudlets is partially mitigated when the ram pressure component parallel to the cloudlet flow direction is included.     

WSO-UV project

During last three decades, astronomers have enjoyed continuous access to the 100–300 nm ultraviolet (UV) spectral range where the resonance transitions of the most abundant atoms and ions (at temperatures between 3000 and 300 000 K) reside. This UV range is not accessible from ground-based facilities. The successful International Ultraviolet Explorer (IUE) observatory, the Russian ASTRON mission and successor instruments such as the Galaxy Evolution Explorer (GALEX) mission or the COS and STIS spectrographs on-board the Hubble Space Telescope (HST) prove the major impact of observations in the UV wavelength range in modern astronomy. Future access to space-based observatories is expected to be very limited. For the next decade, the post-HST era, the World Space Observatory – Ultraviolet (WSO–UV) will be the only 2-m class UV telescope with capabilities similar to the HST. WSO–UV will be equipped with instruments for imaging and spectroscopy and it will be a facility dedicated, full-time, to UV astronomy. In this article, we briefly outline the current status of the WSO–UV mission and the science management plan.     

离心叶轮全三维反问题方法设计误差稳定性研究

用流线曲率全三维反问题方法和引入滑移因子模型的准三维流线曲率反问题方法设计了叶片数不同的和增压比不同的小型高速离心叶轮.用商用计算流体力学(CFD)求解器估算了这些叶轮的性能.对比了这两种反问题方法的设计误差稳定性,考察了分流叶片对设计误差的影响.结果表明,流线曲率全三维反问题方法能够根据叶片负荷对叶片设计做出恰当调整.较准三维反问题方法,流线曲率全三维反问题方法所设计叶轮的增压比普遍偏高.随叶片负荷增加,较准三维反问题方法,流线曲率全三维反问题方法的设计误差变化较小,即其设计误差稳定性明显较好.分流叶片对准三维反问题方法设计结果的影响明显较小.      

On the electrodynamics of counter stream in pulsar’s inner annular cap region

The electric properties of pulsar’s inner annular gap are explored in this paper. Under two main assumptions, (1) the pulsar is alive, (2) the total charge of pulsar should not vary with time, the condition for the acceleration of negative particle in the annular region is derived. The acceleration condition is j₋ ? 0.5j₊, i.e., the current carried by negative particles is greater than or equal to 0.5 times of the current carried by positive particles. This condition holds even when the backward flow of positive particles exists in the annular region. It is noted that the outflow of negative particles offers good opportunities to understand the current closure problem of pulsar as well as wide radiation beam of pulsar observed at high energy band.     

旋翼桨叶动力学设计技术

桨叶动力学设计,其实质是求解非线性高维动力学逆问题的具体实施。本文较全面地阐述了这方面的进展情况,提出了切实可行、有效实用的数值方法。     

ISAR欺骗干扰效果评估方法研究

逆合成孔径雷达（ISAR）能够获取运动目标的一维像和二维像,利用宽带特征识别出真实空间目标.宽带成像欺骗干扰是对抗ISAR雷达目标识别的有效措施.构建了基于目标结构特征的ISAR欺骗干扰效果评估体系,提出了相应的干扰效果评估准则,研究了ISAR欺骗干扰效果评估方法.利用仿真评估软件进行仿真分析,验证了评估方法的合理性.     

新型通用飞机机载数据记录仪的研究

分析了国内外通用飞机机载数据记录仪的现状,指出我国现有通用飞机机载数据记录仪所存在的不足之处.同时,根据未来通用飞机的发展,深入研究了新型通用飞机机载数据记录仪的功能、特点需求,并且基于模块化思想,提出了新型通用飞机机载数据记录仪的设计思路,给出了新型通用飞机机载数据记录仪的软硬件体系结构,并对其核心模块的功能进行了详细的阐述.最后,简述了新型通用飞机机载数据记录仪的应用.     

Probing the first stars and black holes in the early Universe with the Dark Ages Radio Explorer (DARE)

A concept for a new space-based cosmology mission called the Dark Ages Radio Explorer (DARE) is presented in this paper. DARE’s science objectives include: (1) When did the first stars form? (2) When did the first accreting black holes form? (3) When did Reionization begin? (4) What surprises does the end of the Dark Ages hold (e.g., Dark Matter decay)? DARE will use the highly-redshifted hyperfine 21-cm transition from neutral hydrogen to track the formation of the first luminous objects by their impact on the intergalactic medium during the end of the Dark Ages and during Cosmic Dawn (redshifts z = 11–35). It will measure the sky-averaged spin temperature of neutral hydrogen at the unexplored epoch 80–420 million years after the Big Bang, providing the first evidence of the earliest stars and galaxies to illuminate the cosmos and testing our models of galaxy formation. DARE’s approach is to measure the expected spectral features in the sky-averaged, redshifted 21-cm signal over a radio bandpass of 40–120 MHz. DARE orbits the Moon for a mission lifetime of 3 years and takes data above the lunar farside, the only location in the inner solar system proven to be free of human-generated radio frequency interference and any significant ionosphere. The science instrument is composed of a low frequency radiometer, including electrically-short, tapered, bi-conical dipole antennas, a receiver, and a digital spectrometer. The smooth frequency response of the antennas and the differential spectral calibration approach using a Markov Chain Monte Carlo technique will be applied to detect the weak cosmic 21-cm signal in the presence of the intense solar system and Galactic foreground emissions.     

通用航空FBO经营发展的基本模式

FBO经营发展具有多种商业形态,而当前国外通航发达国家FBO经营发展具有较为成熟的模式,国内FBO发展还处在起步阶段,必须学习借鉴国外的成熟模式,通过不同的方式尽快使经营走向成熟。同时,国内FBO又需要根据内外部发展环境,创新自身经营模式,更好地推进通用航空FBO的发展。     

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.