Multi-wavelength coordinated observations of ionospheric irregularity structures from an anomaly crest location during unusual solar minimum of the 24th cycle

The present paper reports coordinated ionospheric irregularity measurements at optical as well as GPS wavelengths. Optical measurements were obtained from Tiny Ionospheric Photometer (TIP) sensors installed onboard the Constellation Observing System for Meteorology, Ionosphere, and Climate (COSMIC) satellites. GPS radio signals were obtained from a dual frequency GPS receiver operational at Calcutta (22.58°N, 88.38°E geographic; geomagnetic dip: 32.96°; 13.00°N, 161.63°E geomagnetic) under the SCIntillation Network Decision Aid (SCINDA) program. Calcutta is located near the northern crest of Equatorial Ionization Anomaly (EIA) in the Indian longitude sector. The observations were conducted during the unusually low and prolonged solar minima period of 2008–2010. During this period, four cases of post-sunset GPS scintillation were observed from Calcutta. Among those cases, simultaneous fluctuations in GPS Carrier-to-Noise ratios (C/N_o) and measured radiances from TIP over a common ionospheric volume were observed only on February 2, 2008 and September 25, 2008. Fluctuations observed in measured radiances (maximum 0.95 Rayleigh) from TIP due to ionospheric irregularities were found to correspond well with C/N₀ fluctuations on the GPS links observed from Calcutta, such effects being noted even during late evening hours of 21:00–22:00 LT from locations around 40° magnetic dip. These measurements indicate the existence of electron density irregularities of scale sizes varying over several decades from 135.6 nm to 300–400 m well beyond the northern crest of the EIA in the Indian longitude sector during late evening hours even in the unusually low solar activity conditions.     

Thermal and nonthermal flare emission observed with the Nobeyama Radio Heliograph

The early phases of three flares, observed by the Nobeyama Radio Heliograph, are studied. Nonthermal and thermal radio sources are identified by comparison with soft X-ray images taken by the Soft X-ray Telescope onboard the Yohkoh satellite. Two of the flares are mainly of nonthermal origin and their location coincides with one of the footpoints of soft X-ray loops. Another flare has both thermal and nonthermal components which start to brighten simultaneously. This suggests that particle acceleration and plasma compression develop simultaneously.     

毫微秒脉冲雷达高度表的超低空静态模拟测高及其结果分析

本文主要介绍一种新型脉冲雷达高度表,装于CK1E超低空靶机模型上静态测高的试验方法和结果。结果分析表明该高度表适用于CK1E靶机的飞行控制系统,作为高度传感器,在超低空进行精确而稳定的测高成功。     

某型直升机超短波电台互相干扰的问题分析

某型直升机装备的两超短波电台在使用中出现某些频点下的互相干扰现象,尽管地面采取了相应措施却均未改善。本文在常规修理方法的基础上,采用了一些新方法找到了此故障的根源,并为类似电台干扰问题提供参考。     

TOFS:一种新的宽带源DOA估计算法

介绍了一种新的宽带源DOA估计方法:TOFS。与TOPS(投影子空间正交性测试)方法类似,该方法通过同时测试频域各频段噪声子空间与阵列搜索流型之间的正交性来进行DOA估计。作为对比,根据非相关MUSIC方法,提出了一种新的适用于宽带的非相关MUSIC方法,称为I-MUSIC方法。与宽带相关方法不同,TOFS方法不需要任何初始值的预估。与宽带非相关方法也不相同,TOFS方法同时测试各频段噪声子空间与阵列搜索流型之间的正交性。仿真了TOFS与I-MUSIC、CSSM、TOPS的性能比较。仿真结果表明,CSSM方法在低信噪比时有较好的性能,TOFS方法在中等信噪比以上时,有较好的性能。同时,TOFS方法避免了TOPS方法中常常出现的伪峰。     

雷达-电子战-通信的一体化

为充分发挥武器系统的作战效能，对作战平台上的雷达-电子战-通信一体化技术进行了研究。阐述了雷达与电子战、雷达与通信一体化的必要性和特点，并对一体化的关键技术，如以线性调频与伪随机编码信号的组合为共用信号、共用孔径及其波束控制技术等进行了分析。最后给出了一个采用软件无线电技术的雷达-无线电-通信一体化系统的方案。     

差分编码OQPSK调制解调器设计

OQPSK调制性能大大优于 QPSK,但由于 OQPSK调制的特殊性 ,其差分编解码相应比较复杂 ,文中对DOQPSK的差分编解码和调制解调原理进行了深入的分析 ,针对传统 DOQPSK相干解调和解码方法存在的问题 ,给出一种简单高效的改进 DOQPSK解调和解码方法。该方法不仅结构简单 ,同时消除了与 DQPSK解调相比存在的 3 d B解调损失问题 ,大大提高系统的解调性能     

Infrared radiation from compact X-ray sources

Observations of the X-ray binaries 4U 0115+634 and A 0535+262 performed in 1981 – 1982 revealed significant IR variabilities of these sources. 4U 0115+634 was observed twice, in the state close to X-ray activity, and in the state of low activity, thus changing from K = 7^m.75 to K > 9^m. A 0535+262 shows the temporal variations ranged from tens minutes to some days. The regular variations of IR brightness are suspected with teh period close to 104 s that corresponds to the period of axial rotation of neutron star in A 0535+262. The results obtained present arguments in favour of hypothesis that IR radiation is generated near the accreting neutron star and is possibly of maser nature.     

Supersoft X-ray sources

More than 100 supersoft X-ray sources (SSS) are reported in 20 external galaxies, the Magellanic Clouds (MCs) and our Galaxy. The effective temperatures of the brighter SSS are 20–100 eV. SSS with luminosities below ≈3 × 10³⁸ erg s⁻¹ are consistent with accreting white dwarfs (WDs) with steady nuclear burning or post-novae. Optical identifications exist for SSS in our Galaxy and the MCs (including orbital period determinations) and for SSS in M31 (with novae and symbiotic stars, SySs). High resolution X-ray spectra of the brightest SSS in our Galaxy and the MCs reveal the existence of spectral features due to high gravity WDs. Timing studies in X-rays (combined with the optical) of the stable nuclear burning phase in steady nuclear burning sources and in post-novae allow to constrain the mass accretion rate onto and the mass of the nuclear burning WD. The nature of a few SSS with luminosities 10³⁹ erg s⁻¹ remains unclear.     

Relationships between energetic storm particle events and interplanetary shocks driven by full and partial halo coronal mass ejections

We have analysed energetic storm particle (ESP) events in 116 interplanetary (IP) shocks driven by front-side full and partial halo coronal mass ejections (CMEs) with speeds $>$400 km s^?1during the years 1996–2015. We investigated the occurrence and relationships of ESP events with several parameters describing the IP shocks, and the associated CMEs, type II radio bursts, and solar energetic particle (SEP) events. Most of the shocks (57 %) were associated with an ESP event at proton energies $>$1 MeV.The shock transit speeds from the Sun to 1 AU of the shocks associated with an ESP event were significantly greater than those of the shocks without an ESP event, and best distinguished these two groups of shocks from each other. The occurrence and maximum intensity of the ESP events also had the strongest dependence on the shock transit speed compared to the other parameters investigated. The correlation coefficient between ESP peak intensities and shock transit speeds was highest (0.73 $\pm$ 0.04) at 6.2 MeV. Weaker dependences were found on the shock speed at 1 AU, Alfvénic and magnetosonic Mach numbers, shock compression ratio, and CME speed. On average all these parameters were significantly different for shocks capable to accelerate ESPs compared to shocks not associated with ESPs, while the differences in the shock normal angle and in the width and longitude of the CMEs were insignificant.The CME-driven shocks producing energetic decametric–hectometric (DH) type II radio bursts and high-intensity SEP events proved to produce also more frequently ESP events with larger particle flux enhancements than other shocks. Together with the shock transit speed, the characteristics of solar DH type II radio bursts and SEP events play an important role in the occurrence and maximum intensity of ESP events at 1 AU.