考虑冷气掺混的涡轮气动性能数值研究

采用数值求解雷诺平均N-S方程的方法,数值模拟了带冷气掺混的涡轮内部全三维黏性流场,研究了冷气掺混对涡轮流动损失和气动性能的影响。数值计算结果表明,对于具有单排孔冷气入射的气膜冷却情况,当入射角是30°时,随着冷气流量增加,流动损失减小;而对于多排气膜孔冷气入射,各排气膜孔冷气之间的干扰是引起流动损失的主要原因,对不同位置冷气流量的优化选择,可以明显减小前后排冷气的掺混损失。为了降低冷气掺混的流动损失,基于数值实验的结果,本文首次引入了叶片表面气膜孔沿径向交错排列结构。     

Fuzzy energy-based dual contours model for automated coronal hole detection in SDO/AIA solar disk images

The presence of coronal holes in solar disk plays an important role in influencing the space weather and generation of the solar wind. As such there lies a requirement in proper study and prediction of coronal holes occurs in the solar disk. This, in turn, arises the necessity of detection of coronal holes present in the solar disk. In this work, a Hough transformed inspired fuzzy-energy simulated dual contours-based segmentation technique has been proposed for the detection and extraction of holes in solar disk. In the proposed method Hough transform has been induced to initialize the contour for the contour-based method of segmentation. In the algorithm, two contours (active and static) have been initiated and made to evolve based on the energy function by incorporating the gray-scale intensity. Here in the work one contour is made to deform its shape while the other contour is kept static for the coronal holes detection purpose. The experiment has been carried out on few benchmark datasets and the corresponding outcomes have been compared with the results of other existing algorithms. The comparison results highlight the performance of the proposed technique in detection of coronal holes in solar disk.     

高压涡轮尾切凹槽叶尖冷却换热特性

为研究尾切凹槽状涡轮叶片叶尖的表面换热,通过瞬态风洞实验得到无冷却和带除尘孔两种情况下叶尖表面传热系数,并将其与数值模拟结果进行对比,实验结果的不确定度小于5%。分析叶尖间隙流场情况,无冷却时,由于腔底的空腔涡和凸肩壁的分离泡,高表面传热系数集中在压吸力侧凸肩和腔底前缘处;腔底后半段沿压力侧存在条状低表面传热系数分布。有除尘孔冷却时,冷却气体分为高低能两股流体,高能流体随泄漏流流出,造成吸力侧凸肩存在多段高表面传热系数集中分布;低能流体紧贴凹槽压力侧向后流动,对应位置冷却效率可达0.4以上。      

基于加力内锥冷却的红外隐身技术研究

应用数值仿真方法计算多种冷却方式下的加力内锥流场和温度场,利用红外辐射特性计算软件分析加力内锥的红外辐射特性。研究结果表明：采用小孔与缝隙组合冷却的效果比单用小孔冷却或单用缝隙冷却的好,采用孔/缝组合冷却的加力内锥的红外辐射强度降低68.49%。     

Relation between solar wind velocity and properties of its source region

Different kinds of coronal holes are sources of different kind of solar winds. A successful solar wind acceleration model should be able to explain all those solar winds. For the modeling it is important to find a universal relation between the solar wind physical parameters, such as velocity, and coronal physical parameters such as magnetic field energy. To clarify the physical parameters which control the solar wind velocity, we have studied the relation between solar wind velocity and properties of its source region such as photospheric/coronal magnetic field and the size of each coronal hole during the solar minimum. The solar wind velocity structures were derived by using interplanetary scintillation tomography obtained at Solar-Terrestrial Environment Laboratory, Japan. Potential magnetic fields were calculated to identify the source region of the solar wind. HeI 1083 nm absorption line maps obtained at Kitt Peak National Solar Observatory were used to identify coronal holes. As a result, we found a relation during solar minimum between the solar wind velocity and the coronal magnetic condition which is applicable to different kind of solar winds from different kind of coronal holes.     

MHD Waves and Heating in Coronal Holes

Coronal holes have been identified as source regions of the fast solar wind, and MHD wave activity has been detected in coronal holes by remote sensing, and in situ in fast solar wind streams. I review some of the most suggestive wave observations, and discuss the theoretical aspects of MHD wave heating and solar wind acceleration in coronal holes. I review the results of single fluid 2.5D MHD, as well as multi-fluid 2.5D MHD models of waves in coronal holes, the heating, and the acceleration of the solar wind be these waves.     

压力探针临壁效应的试验与计算

临壁效应会使压力探针的测量结果发生误差。由于探针属非流线形物休，所以其临壁效应的机理与流线形的机翼不同，不能简单套用机翼的结论．对圆柱三孔针的试验结果表明，可以用叠加点涡的方法来描述其临壁效应。点涡强度随离壁距离的减少而增强．     

Gamma rays from accreting matter onto collapsed objects

In the spherical accretion onto massive objects, the matter may be heated up to temperatures as high as 10¹² °K. In such a hot plasma, the thermal bremsstrahlung (e-e and e-p) and π° decay from inelastic collisions of protons are the main γ-ray sources. We determined the γ -ray production spectra from the π° decay and from bremsstrahlung for different temperatures. The expected γ-ray spectra were evaluated too in order to fit experimental data. We have fitted COS B data from 3C 273 using a two temperatures plasma model. The best fit is for

Full-size image (1K)

(M₈ is the black hole mass in 10⁸ M) which gives . The hard X-ray measurements do not contradict the bremsstrahlung spectrum.     

On the primordial black holes in the earth

Astrophysical limitations do not exclude the possibility of some number of dark matter primordial Black Holes (BH) being seeded in the interiors of the Earth at the epoch of planet condensation in the young Solar System. We show that limitations on the neutrino radiation due to the BH quantum evaporation and accretion growth of BH mass completely forbid the existence of primordial BH of any mass in the Earth.     

Comptonization efficiencies of the variability classes of GRS 1915 + 105

The Galactic microquasar GRS 1915 + 105 exhibits at least seventeen types of variability classes. Intra and inter class transitions are reported to be observed within seconds to hours. Since the observation was not continuous, these classes appeared to be exhibited in a random order. Our goal is to predict a sequence of these classes. In this paper, we compute the ratio of the photon counts obtained from the power-law component and the blackbody component of each class and call this ratio as the ‘Comptonizing efficiency’ (CE) of that class. We sequence the classes in the ascending order of CE and find that this sequence matches with a few class transitions observed by RXTE satellite and IXAE instruments on board IRS-P3. A change in CE corresponds to a change in the optical depth of the Compton cloud. Our result implies that the optical depth of the Compton cloud gradually rises as the variability class becomes harder.