Investigating the Coronal Mass Ejections associated with DH type-II radio bursts and solar flares during the ascending phase of the solar cycle 24

We studied a set of 74 CMEs, with shedding the light on the halo-CMEs (HCMEs), that are associated with decametric – hectometric (DH) type-II radio bursts (1–16?MHz) and solar flares during the period 2008–2014. The events were classified into 3 groups (disk, intermediate, and limb events) based on their longitudinal distribution.We found that the events are mostly distributed around 15.32° and 15.97° at the northern and southern solar hemispheres, respectively. We found that there is a clear dependence between the longitude and the CME’s width, speed, acceleration, mass, and kinetic energy. For the CMEs’ widths, most of the events were HCMEs (～62%), while the partial HCMEs comprised ～35% and the rest of events were CMEs with widths less than 120°. For the CMEs’ speeds, masses, and kinetic energies, the mean values showed a direct proportionality with the longitude, in which the limb events had the highest speeds, the largest masses, and the highest kinetic energies. The mean peak flux of the solar flares for different longitudes was comparable, but the disk flares were more energetic. The intermediate flares were considered as gradual flares since they tended to last longer, while the limb flares were considered as impulsive flares since they tended to last shorter.A weak correlation (R?=?0.32) between the kinetic energy of the CMEs and the duration of the associated flares has been noticed, while there was a good correlation (R?=?0.76) between the kinetic energy of the CMEs and the peak flux of the associated flares. We found a fair correlation (R?=?0.58) between the kinetic energy of the CMEs and the duration of the associated DH type-II radio bursts.     

Latitudinal distribution of solar coronal active regions

We studied the cyclic evolution of the latitudinal distribution of solar coronal active regions based on daily images from SOHO EIT for the period 1995–2017. Fully automated software was used, which included the following steps: initial preparation of images in the data series, normalization of histograms and correction of limb brightening, segmentation of images using threshold intensity values obtained from their histograms, scanning of segmented images in heliographic coordinates and obtaining profiles of latitudinal distribution of coronal active regions for each image of the data series. From the output data, we obtained a temporary change in the latitudinal distribution profiles and the migration of activity centers on the solar disk. From the period of minimum activity to the next minimum in both hemispheres, activity centers begin to migrate from high latitudes towards the equator. At the same time, the general center of activity repeatedly changes the direction of migration. The latitudinal distribution of the so-called presence factor of coronal active regions closely resembles the magnetic butterfly diagram, which proves their direct causal relationships. Variations in the presence factor of coronal active regions are correlated with cyclic variations in the sunspot daily numbers.     

日冕边界条件与太阳风共转相互作用

本文根据第二十太阳周太阳风数据的统计分析结果,用太阳风二维理想流体模型探讨近太阳区的不同边界条件太阳风与共转相互作用对1AU处太阳风各参数影响,得到共转相互作用不能引起太阳风速度和马赫数的反相扰动,推断在太阳风加速区温度扰动对太阳风的影响最大,而在太阳风传播区速度扰动对太阳风的影响最大.      

飞机燃油质量特性计算及供油顺序的设计

采用将油箱分割成多单元斜六面体的方法解决了外形复杂油箱的描述问题;采用切片法计算燃油质量特性,方法本身考虑了飞机姿态角对燃油形状的影响。解决了在给定重心活动范围情况下供油顺序设计问题。算例证明本方法具有很高的精确度和应用价值。     

混杂复合材料层合板抗冲击性能研究

为了探究复合材料层合板在实际应用中因承受冲击载荷而造成的结构安全问题,本研究采用实验和仿真相结合的方法,首先探究冲头形状对复合材料层合板损伤机理的影响,然后结合不同冲击能进一步揭示层合板的承载力和能量吸收变化规律。结果表明,相同冲击能下,层合板的损伤范围和承载力随着圆锥头、半球头、平头依次增加;相应的层合板的临界穿透能量随着圆锥头、半球头、平头依次增大;冲头形状和冲击能对层合板的吸能能力有较大的影响。     

旋转固体火箭发动机随质量变化的姿态运动分析

旋转固体火箭发动机是否稳定主要取决于其微小的侧向角速度是否被耗散或被放大。就发动机内部随燃烧而质量发生变化,且使飞行器整体质心前移的圆柱形装药结构进行姿态动力学分析,得到在几种典型装药形式下侧向角速度随时间的变化情况。结果指出,质量的减小对飞行角速度的变化是有影响的,由于误差等因素所引入的初始侧向角速度也会被逐渐耗散掉。此外,在某些装药形式及燃烧方式下,其侧向角速度在燃烧过程中会以指数规律增加,通过对计算结果的分析,提出了对发动机设计的稳定性要求。     

Near-infrared study of open clusters Teutsch 10 and Teutsch 25

The astrophysical parameters have been estimated for two unstudied open star clusters Teutsch 10 and Teutsch 25 using the Two Micron All Sky Survey ($2\mathit{MASS}$) database. Radius is estimated as 4.5 arcmin for both clusters using radial density profiles. We have estimated proper motion values in both RA and DEC directions as $2.28\pm 0.3$ and $-0.38\pm 0.11$?mas?yr^?1 for Teutsch 10 and $0.48\pm 0.3$ and $3.35\pm 0.16$?mas?yr^?1 for Teutsch 25 using $\mathit{PPMXL}$¹ catalog. By estimating the stellar membership probabilities, we have identified 30 and 28 most likely members for Teutsch 10 and Teutsch 25 respectively. We have estimated the reddening as $E(B-V)=0.96\pm 0.3$?mag for Teutsch 10 and $0.58\pm 0.2$?mag for Teutsch 25, while the corresponding distances are $2.4\pm 0.2$ and $1.9\pm 0.1$?kpc. Ages of $70\pm 10$?Myr for Teutsch 10 and $900\pm 100$?Myr for Teutsch 25 are estimated using the theoretical isochrones of metallicity Z?=?0.019. The mass function slopes are derived as $1.23\pm 0.30$ and $1.09\pm 0.35$ for Teutsch 10 and Teutsch 25 respectively. Estimated mass function slope for both the clusters are close to the Salpeter value ($x=1.35$) within the errors. Estimated values of dynamical relaxation time are found to be less than cluster’s age for these objects. This concludes that both objects are dynamically relaxed. The possible reason for relaxation may be due to dynamical evolution or imprint of star formation or both.     

地面燃气轮机单管燃烧室流量分配试验

对设计的100kW地面燃气轮机单管燃烧室空气流量分配进行了试验研究。在常压环境下采用堵孔法分别得到了旋流器、主燃孔和掺混孔的流量特性曲线,分析得到燃烧室不同结构的流量系数;试验研究了不同进口流量条件下燃烧室的流量分配,测量得到了燃烧室总压损失。研究发现:随着进口空气流量的增加,燃烧室的流量分配比例基本保持稳定,并且与燃烧室的设计空气比例基本吻合;随着燃烧室进口流量（雷诺数）的增加,旋流器、主燃孔和掺混孔的流量系数呈线性降低;随着进口流量（雷诺数）的增加,燃烧室总压损失逐渐增大;对主燃孔和掺混孔的流量特性测量中,两种测量方法得到的试验结果稍有差别,总体上看两种测量方法的试验结果较为接近。通过对比分析证明两种试验测量方法真实可靠,该研究结果可为100kW地面燃气轮机燃烧室的设计与优化提供依据。      

用于空间探测飞行时间质谱仪的真空系统和取样系统设计

文章介绍了可用于空间探测飞行时间质谱仪的真空系统和取样系统设计,并建立了该TOFMS原理样机的地面试验系统。为适应空间探测和地面试验2种不同工作模式,设计了2套不同的真空系统。根据文章建立的气体样本进样的理论分析模型进行理论分析计算,并通过地面适应性试验测定了质谱室的真空度、空气的Voltage-Amu谱图、Kr样本Voltage-Amu谱图及进样时间。试验结果表明:真空系统和取样系统设计合理,能够满足试验需求;理论分析模型正确,能够用于指导试验。     

The effective temperatures of O-type stars from UV spectroscopy

We present an analysis of high resolution spectra in the far-UV – UV range (∼905–2000 Å) with non-LTE, spherical, hydrodynamical, line-blanketed models, of three O-type Galactic stars, and derive their photospheric and wind parameters. These data extend previously analyzed samples and fill a gap in spectral type coverage. The combined sample confirms a revised (downward) T_eff scale with respect to canonical calibrations, as found in our previous works from UV and optical spectra, and in recent works by other authors.