共查询到19条相似文献,搜索用时 359 毫秒
1.
利用布里奇曼法进行了InAsSb半导体合金的生长,并对其结构、光学及电学特性进行了表征.研究发现,As替位掺杂造成X射线(111)衍射峰略微右移,同时其半高宽明显展宽.基于X射线衍射数据,利用Vegard定律计算出的As组分与能谱测量得到的结果基本吻合.此外,As的掺入使得材料背景载流子浓度略有上升.傅里叶变换红外光谱结果显示,As的替入使得材料带隙明显变小,拟合得到的光学带隙与通过Woolley-Warner经验公式得到的值定性一致.研究结果表明,As掺杂是减小InSb带隙,开拓其面向第二个大气窗口红外探测应用的有效途径. 相似文献
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本文对109个X射线选择的类星体和114个射电及光学选择的类星体进行统计分析.发现在它们的红移、光学光度以及平均光学-X射线谱指数的直方分布图上, X射线选择类星体统计上都分布在这些参数图的低端.在所有样品的单色X射线光度lX与单色光学光度lO的关系图上, X射线选择类星体绝大部分处在光学暗的低光度区域.若以lglo=31.2erg/s·Hz为分界点, 可把光学光度划分为光学亮和暗两个区域, 则发现射电及光学选择类星体在图中光学亮区内的斜率b=0.64, 在光学暗区内的斜率b=0.95, 而X射线选择类星体的b仅为0.78, 因而暗示出它们可能是类星体现象中的一个次型. 相似文献
3.
本文对247个类星体的X射线性质进行了统计分析,这些X射线资料是由爱因斯坦卫星在0.5—4.5keV的能带内观测到的。主要结果是:在各种视亮度和红移(或距离)的已知1619个类星体中,都有百分比相近的部分为X射线源。Ⅰ型Seyferc星系的发射线Hβ与[OⅢ]的等值宽度比REW同X射线光度Lx强相关,这可作为Ⅰ型Seyfert星系的X射线光度的一个新指标。光学辐射以及2.5GHz以上的高频射电辐射都同X射线辐射相关,说明这三种辐射的区域依次相邻而且机制也相似。色指数U-B和B-V都同X射线辐射不相关,但U-B同B-V弱相关。 相似文献
4.
胡世高 《中国空间科学技术》1988,8(6):56
本文叙述了我国首次在空间微重力下进行的碲镉汞(MCT)晶体生长试验及一些观测结果。生长是从熔体进行的。在空间90min的加热时间内,将MCT多晶试样熔化,然后随炉冷却,最后在地面上再结晶。于是,生长出约3cm长的晶体,其表面光滑.结构致密,无孔洞,由1~3个大晶粒组成,其中单晶占74%。X射线能量色散分析(EDS)表明,其径向组分均匀性优于±0.02,其中约1cm长的一段晶体的径向组分均匀性优于±0.01。电学特性与地面上生长的样品基本相同。 相似文献
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基于一种低的交流电压条件(10 V),在NaOH和Na2SiO3的混合溶液体系中,对AZ91D镁合金进行电化学阳极氧化处理.利用扫描电镜(SEM)、X射线能谱仪(EDS)、X射线衍射仪(XRD)、电化学测试技术等手段研究了AZ91D镁合金表面阳极氧化的成膜过程、膜层生长的特点以及氧化工艺参数对膜层性能的影响规律.试验结果表明:在10 V这样低的交流电压下,在镁合金表面获得的氧化膜层表面均匀,为无孔洞的平层状膜层,其生长过程呈叠加式特点;获得的氧化膜层的主要成分为Mg2SiO4;在质量分数为3.5%的NaCl溶液中,经过电化学阳极氧化的镁合金的耐蚀性优于未经处理的镁合金. 相似文献
8.
王金良 《北京航空航天大学学报》2005,31(1):1-4
过渡金属与硅的接触系统一直被人们所关注,是因为它们在界面处具有肖特基势垒的形成、过渡金属硅化物的外延生长、制作器件的稳定和耐高温等重要性.因此在硅基底上形成金属硅化物薄膜也被广泛应用于半导体工业.对硅衬底上蒸发的Cr、Fe、Mn薄膜进行热处理,通过固相反应法(SPR)制备过渡金属硅化物薄膜,即经过对过渡金属硅化物(薄膜)/Si系统进行各种温度、不同时间的热处理,制备出各种过渡金属硅化物薄膜.对于制成的各种硅化物薄膜,用X射线衍射法(XRD)和软X射线发射分光光谱法(SXES)对它们的组成成分进行了分析和确认.并且,由这两种分析方法表明:各种过渡金属硅化物薄膜在硅衬底上各形成了单一相的均匀层硅化物薄膜. 相似文献
9.
对ISEE-3人造卫星在1980年5月—1981年8月中,观测到的48个X射线耀斑进行了分析,发现其中有1/3是在6个活动区中重复爆发的.研究这部分X射线耀斑的物理性质与所在活动区的黑子面积、活动区类型及磁结构的关系,得到了一些结果:(1)发生在同一活动区中的X射线耀斑,其硬X射线峰值积分流量及谱硬度与活动区黑子面积成正相关;(2)多次爆发X射线耀斑的活动区全部具有δ型磁结构;(3)发生在不同活动区中的X射线耀斑,其物理特征与所在活动区的面积大小无明显关系.由此可以认为,活动区磁场梯度的大小,亦即活动区电流的大小,在爆发耀斑的过程中具有决定性作用.此外,还用电流环模型从理论上讨论了上述特征. 相似文献
10.
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
11.
L van Driel-Gesztelyi P.K Manoharan M Pick P.P Démoulin 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1997,19(12):1883-1886
Yohkoh X-ray images, multifrequency two-dimentional observations of the Nancay Radioheliograph, Kitt Peak and Mees magnetograms provide a unique set of data with which to study a C4.7 long-duration flare that was observed close to the equator (S07, W11) on 25 Oct. 1994 at 09:49 UT. Linear force-free field extrapolations indicate a very high degree of non-potentiality in the active region. The X-ray flare started with the expansion of spectacular twisted loops. Fifteen minutes after the flare onset sporadic radio (type III) bursts were observed spreading over an area of almost 1/3 of the solar disc and two remote X-ray brightenings appeared over quiet regions of opposite magnetic polarity located in on opposite hemispheres of the Sun. In the close vicinity of these remote brightenings two coronal holes formed. The timing and location of these events combined with the overall magnetic configuration provide evidence for a large-scale magnetic reconnection occurring between the expanding twisted loops and the overlying huge loops which inter-connect quiet solar regions. 相似文献
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Salvatore Serio 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1982,2(9):271-278
As a result of the large body of data available from solar and stellar coronae, our understanding of the mechanisms responsible for the heating of coronal plasmas to temperatures of the order of ~ 108 K has changed. The solar corona is highly structured by magnetic fields and the acoustic shocks which, according to early theories, should have acted as the coronal energy source have not been observed. Einstein Observatory data show moreover that coronae are present in most regions of the H-R diagram. The observed relationship between X-ray luminosity and rotational velocity in dwarf stars from spectral types F to M again suggests an active role for the magnetic fields.The basic picture which is emerging is that coronae in stellar types from F to M are produced because of the interaction of the magnetic field with the convective velocity fields generated in the photosphere resulting in MHD waves or currents which dissipate in the corona. X-ray emission in early type stars cannot be explained with this mechanism and the models which have been proposed for these stars are not yet completely satisfactory. 相似文献
13.
C. L. Sarazin 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1993,13(12):365-368
ROSAT HRI images were obtained for two clusters of galaxies which contain strong cooling flows, A2029 and 2A0335+096. These observations confirm that gas is cooling at rates of
in A2029 and
in 2A0335+096. In both clusters, the X-ray emission from the inner cooling flow regions (r 100 kpc) is very inhomogeneous, with the X-ray surface brightness being dominated by a number of X-ray emitting filaments. Using the crude spectral resolution of the HRI, we show that these filaments are the result of excess emission, rather than foreground X-ray absorption. Although there are uncertainties in the pointing, many of the X-ray features in the cooling flow region of 2A0335+096 correspond to features in H optical line emission. This indicates that the 104 K gas originates through the cooling of hot X-ray emitting gas. The gas is the filaments is too dense to be in hydrostatic equilibrium, and it is likely that other forces such as rotation, turbulence, and magnetic fields influence the dynamical state of the gas. The filaments may be supported in part by magnetic fields and may be connected with the filaments of very strong Faraday rotation seen in several nearly cooling flows. 相似文献
14.
H. Hara 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1997,20(12):2279-2288
A study on solar coronal activities related to the 11-year activity cycle is presented from the Yohkoh soft X-ray observations. Yohkoh was launched in August 1991, just after the solar maximum of the cycle 22 and continues to observe the Sun in the declining phase of the magnetic activity cycle toward the solar minimum. The soft X-ray flux from the whole Sun in the declining phase essentially decreases with the size of active regions. The X-ray intensity in quiet regions in the declining phase decreases with the magnetic flux observed at the photosphere. The whole-Sun soft X-ray flux does not monotonically decrease, but there are periodic enhancements of the flux with about a one-year interval. The activity appears as bright clusters in the butterfly diagram of the soft X-ray intensity and corresponds to the emergence of complexes of activity in the sunspot zones. The high-latitude activity is also studied, and we find that the X-ray intensity of high-latitude regions fluctuates with time scale of about one year. 相似文献
15.
M.E. Machado A.M. Hernández M.G. Rovira C.V. Sneibrun 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》1984,4(7):91-94
We have studied soft and hard X-ray images of 13 solar flares from six active regions observed by the Hard X-ray Imaging Spectrometer (HXIS). Our results indicate the presence of pre-hard X-ray burst excesses in the 11.5–30.0 keV range, indicating a slow buildup of the acceleration process or a strong preheating. During the impulsive phase, all of the events show the simultaneous energization of neighboring field structures, which, in the case we show in some detail, share about equal amounts of the released energy. This association seems to be indicative of strong acceleration and energy release triggered by the interaction between magnetic loops. 相似文献
16.
Debi Prasad Choudhary 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2012
We observed 10 active regions through their disk passage during June 25–August 25, 1988, with the Tower Vector Magnetograph (TVM) of Marshall Space Flight Center. The TVM was used in scanning mode to measure the photospheric Doppler velocities with the Line-Center-Magnetogram (LCM) technique in the spectral line of FeI 5250.2 Å. In this paper we present the result of a subset of observations obtained while the active regions were situated away from the solar limb. A wide range of magnetic complexity and associated chromospheric activity characterized these active regions. It was found that the value of zero-crossing wavelength of the integrated Stokes-V profile of two opposite magnetic polarities were different, corresponding to Doppler velocities ranging from ∼100 m s−1 to ∼1475 m s−1. The measurements of relative velocities between different locations, connected by magnetic flux tubes as inferred from YOHKOH soft X-ray and TRACE 171 Å Fe IX images, showed widely different values of dominant localized flows. The region of parasite polarity, which showed recurrent chromospheric activity, was blue shifted with respect to the main “magnetic element” of the same polarity. Some of them were also the sites of sheared magnetic field configuration. The magnitude of the relative velocity between the leading and following polarity is more for the active regions of higher “field asymmetry”. 相似文献
17.
B. Schmieder P. Démoulin E. Pariat T. Török G. Molodij C.H. Mandrini S. Dasso R. Chandra W. Uddin P. Kumar P.K. Manoharan P. Venkatakrishnan N. Srivastava 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2011
During the maximum of Solar Cycle 23, large active regions had a long life, spanning several solar rotations, and produced large numbers of X-class flares and CMEs, some of them associated to magnetic clouds (MCs). This is the case for the Halloween active regions in 2003. The most geoeffective MC of the cycle (Dst = −457) had its source during the disk passage of one of these active regions (NOAA 10501) on 18 November 2003. Such an activity was presumably due to continuous emerging magnetic flux that was observed during this passage. Moreover, the region exhibited a complex topology with multiple domains of different magnetic helicities. The complexity was observed to reach such unprecedented levels that a detailed multi-wavelength analysis is necessary to precisely identify the solar sources of CMEs and MCs. Magnetic clouds are identified using in situ measurements and interplanetary scintillation (IPS) data. Results from these two different sets of data are also compared. 相似文献
18.
M.R. Kundu V.I. Garaimov 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2003,32(12):2497-2502
We discuss a class of microwave flares whose source regions exhibit a distinctive spatial configuration; the primaryenergy release in these flares results from the interaction between emerging magnetic flux and an existing overlying region. Such events typically exhibit radio, X-ray and EUV emission at the main flare site (the site of interaction) and in addition radio emission at a remote site up to 1 × 105 km away in another active region. We have identified and studied more than a dozen microwave flares in this class, in order to arrive at some general conclusions on reconnection and energy release in such solar flares. Typically, these flares show a gradual rise showing many subsidiary peaks in both radio and hard X-ray light curves with a quasi-oscillatory nature with periods of 5–6 seconds, a bright compact X-ray & EUV emitting loop in the main flare source, a delay of the radio emission from the remote source relative to the main X-ray-emitting source. The magnetic field in the main flare site changes sharply at the time of the flare, and the remote site appears to be magnetically connected to the main flare site. 相似文献
19.
S. Masuda J. Sato 《Advances in Space Research (includes Cospar's Information Bulletin, Space Research Today)》2003,32(12):2455-2458
An intense (X9.4/2B) flare, which occurred on 6 November 1997, was observed with the hard X-ray telescope on board Yohkoh. In the M2- (33 – 53 keV) and H-band (53 – 93 keV), This flare clearly show double footpoint sources during its impulsive phase. We have analyzed the locations and motions of these sources in detail. It is found that, at 11:53:06 UT, one of the footpoint sources in the M2-band moved to a new position earlier than the corresponding source in the H-band. The time-lag is about one second and the separation between the old and new positions is 5 arcsec. This happened between two major spikes in the time profile of hard X-ray intensity. This apparent motion might indicate that an epoch of energy release finished somewhere high in the corona and the next epoch started in another magnetic field system. This observation clearly shows that higher energy electrons precipitate into the footpoint region later. We try to interpret this particular phenomenon under the two assumptions, which are the direct precipitation model and the trap-and-precipitation model. 相似文献