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181.
182.
李业欣 《沈阳航空工业学院学报》2011,28(4):42-46
在生产、处理或加工材料的过程中,由于材料的局部区域的不均匀塑性变形,产生了残余应力。残余应力对疲劳强度、抗蚀性、尺寸稳定性、相变、硬度等均有影响;提高表面塑变抗力,降低表层的有效拉应力,可以抑制疲劳裂纹的萌生和扩展,提高疲劳强度。本文主要以结构钢、不锈钢类材料为研究对象,应用x射线衍射原理测定表面残余应力,讨论x射线法测残余应力的要点,分析能够影响测定结果的技术因素、材料因素及被测件的几何因素,并找出应力分析仪最佳的测试参数。 相似文献
183.
面向X射线脉冲星周期估计的压缩感知(CS)中测量矩阵尺寸大,进而导致计算量大。针对这一问题,提出了一种基于经验模态分解-压缩感知(EMD-CS)的脉冲星周期超快速估计方法。将不同畸变度的脉冲轮廓进行EMD分解,得到一系列固有模态函数(IMF)。由于IMF包含了不同时间尺度的局部特征信号,脉冲轮廓畸变度这一微弱局部特征可体现在某些IMF中。采用迭代剔除法剔除冗余的IMF,剩下的IMF构成了测量矩阵。由于IMF的数量较少,采样率大幅减少。利用EMD-CS可实现X射线脉冲星周期超快速估计。通过计算复杂度分析结果可知,采样率与计算量呈正比关系。仿真结果中表明,EMD-CS的采样率为0.25%,仅为FFT-CS的1/29,因而计算量更小。 相似文献
184.
S. Hayakawa T. Kii Y. Tawara 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1984,3(10-12)
The precursor associated with a long X-ray burst is interpreted in terms of the stellar envelope expansion. The mass flow driven by the radiation pressure in excess of the local Eddington limit and the grey atmosphere model correctly describe the burst profiles in different energy ranges. 相似文献
185.
FY-2C卫星太阳X射线探测器性能定标 总被引:5,自引:0,他引:5
通过具体的实验对FY-2C太阳X射线探测器进行了详细的定标.太阳X射线探测器的传感器采用充Ar气的正比计数器.主要探测能量大于4 KeV的太阳X射线流量.在坪特性、效率、正比性、能道划分、能量分辨率和时间分辨率等6个方面详细介绍了定标的方法及结果.定标结果表明,FY-2C卫星的太阳X射线探测器在各个方面都具有很好的性能.最后对FY-2C的在轨探测数据与GOES卫星进行了比较.GOES卫星的太阳X射线传感器采用电离室.FY-2C的探测结果与GOES的探测结果非常吻合.结果表明,FY-2C太阳X射线探测器可以很好地监测太阳X射线的流量变化,为空间环境监测提供有效的服务. 相似文献
186.
187.
V.P. Uryadov F.I. Vybornov A.A. Kolchev G.G. Vertogradov M.S. Sklyarevsky I.A. Egoshin V.V. Shumaev A.G. Chernov 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2018,61(7):1837-1849
The article presents the results of the observation of a strong magnetic storm and two X-ray flares during the summer solstice in 2015, and their impact on the HF signals characteristics in ionospheric oblique sounding. It was found that the negative phase of the magnetic storm led to a strong degradation of the ionospheric channel, ultimately causing a long blackout on paths adjacent to subauroral latitudes. On mid-latitude paths, the decrease in 1FMOF reached ~50% relative to the average values for the quiet ionosphere. It is shown that the propagation conditions via the sporadic Es layer during the magnetic storm on a subauroral path are substantially better than those for F-mode propagation via the upper ionosphere. The delay of the sharp decrease in 1FMOF during the main phase of the magnetic storm allowed us to determine the propagation velocity of the negative phase disturbances (~100 m/s) from subauroral to mid-latitude ionosphere along two paths: Lovozero – Yoshkar-Ola and Cyprus – Nizhny Novgorod. It is shown that both the LOF and the signal/noise ratio averaged over the frequency band corresponding to the propagation mode via the sporadic Es layer correlate well with the auroral AE index. Using an over-the-horizon chirp radar with a bistatic configuration on the Cyprus – Rostov-on-Don path, we located small-scale scattering irregularities responsible for abnormal signals in the region of the equatorial boundary of the auroral oval. 相似文献
188.
相对于公式法,双标记法解决了焦距和焦点位移测量误差所带来的问题.但此方法在射线检测领域普及程度并不高,其中原因,首先是原理较复杂,针对性研究少,其次是测量精度没有被量化,可信度不高.本文从公式法入手,通过对原理公式的变化分析和线性化分析,明晰了双标记法缺陷深度定位原理,推导了缺陷深度定位公式,利用简化模型,对双标记法的定位精度做了进一步的分析与计算,最后针对具体被检测物,测试验证了双标记法的计算公式和测量精度,用理论和实践证明了方法和精度的可靠性. 相似文献
189.
Yuichiro Ezoe Kumi Ishikawa Takaya Ohashi Noriko Y. Yamasaki Kazuhisa Mitsuda Ryuichi Fujimoto Yoshizumi Miyoshi Naoki Terada Yasunobu Uchiyama Yoshifumi Futaana 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
Recent results of solar system planets observed with the Japanese X-ray astronomy satellite Suzaku are reviewed. Thanks to the low instrumental background and good energy resolution, X-ray CCDs onboard Suzaku are one of the best probes to study diffuse X-ray emission. An overview of the Suzaku data of Jupiter and Earth is presented, along with preliminary results of Mars. Firstly, diffuse hard X-ray emission is discovered in 1–5 keV at Jovian radiation belts. Its spectrum is represented by a power-law continuum with a photon index of ∼1.4. This emission could originate from inverse-Compton scattering of solar photons by tens MeV electrons. Secondly, variable diffuse soft X-rays are serendipitously found during observations in the directions of the north ecliptic pole and galactic ridge. Good time correlations with the solar wind and emission lines found in the X-ray spectra are firm evidences of a solar wind charge exchange emission with Earth’s exosphere. Thirdly, diffuse X-ray emission from Martian exosphere via the solar wind charge exchange is investigated for the first time at solar minimum. A stringent upper limit on the density of the Martian exosphere is placed from the Suzaku data. 相似文献
190.
Tuanhui Zhou Haisheng Ji Guangli Huang 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2008,41(8):1195-1201
In this paper, we analyze the footpoint motion of two large solar flares using observations made by the Transition Region and Coronal Explorer (TRACE) and Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI). The two flares are the M5.7 flare of March 14, 2002 and the X10 flare of October 29, 2003. They are both classical two-ribbon flares as observed in TRACE 1600 or 171 Å images and have long-duration conjugate hard X-ray (HXR) footpoint emission. We use the ‘center-of-mass’ method to locate the centroids of the UV/EUV flare ribbons. The results are: (1) The conjugate UV/EUV ribbons and HXR footpoints of the two flares show a converging (inward) motion during the impulsive phase. For the two flares, the converging motion lasts about 3 and 10 min, respectively. The usual separation (outward) motion for the flare ribbons and footpoints take place only after the converging motion. (2) During the inward and the outward motion, the conjugate ribbons and footpoints of the two events exhibit a strong unshear motion. In obtaining above results, TRACE UV/EUV and RHESSI HXR data show an overall agreement. The two events demonstrate that the magnetic reconnection for the flares occurs in highly sheared magnetic field. Furthermore, the results support the magnetic model constructed by Ji et al. [Ji, H., Huang, G., Wang, H. Astrophys. J. 660, 893–900, 2007], who proposed that the contracting motion of flaring loops is the signature of the relaxation of sheared magnetic fields. 相似文献