共查询到20条相似文献，搜索用时 62 毫秒
1.
斑点干涉成像技术是克服大气湍流影响,提高地面大口径望远镜分辨本领的有效途径之一。该技术利用斑点相机拍摄一系列的短曝光像,使得大气湍流冻结,再经过图像处理获得高分辨率重建像。该技术设备简单,易于实现,很快在观测天文学中得到了广泛的应用,尤其是对双星的研究。首先回顾了天文高分辨率重建技术的发展,并介绍了相关研究成果。描述了几种典型的斑点干涉成像处理方法及其优缺点。对图像噪声类型及滤波方法进行了分析。在上海天文台1．56m望远镜上开展了双星斑点干涉观测实验,目标星等4～7mag,双星目标星等差小于2。分别采用斑点干涉术和迭代位移叠加法成功实现了双星目标的高分辨率成像,初步证明了在1．56m望远镜上进行斑点干涉成像实验,能够达到接近望远镜衍射极限的分辨率水平。 相似文献
2.
《天文研究与技术》2016,(3)
利用组成星座的小卫星,分别携带分离的子望远镜和合光成像望远镜,构成Fizeau型光学综合孔径干涉系统,实现高分辨率的面源目标成像是当前的研究热点之一。这种光干涉成像系统,由于稀疏度较大,UV覆盖不全,即空间频率采样不连续,表现为系统光学传递函数有零值存在。要克服UV覆盖不全的影响,获得等效的大孔径望远镜成像效果,需要改变子孔径的空间排布,获得不同基线条件下的图像,进行空间频率信息的提取和合成,最后采用逆滤波的方法达到提高图像质量的目的。在分析单子孔径传递函数与系统传递函数关系的基础上,优化子孔径的排布方式,采用不同的频域滤波器将不同基线获得的图像中信噪比高的频率区域提取出来进行合成,再变换到空域并进行逆滤波处理,得到改善的合成图像。仿真结果显示,当得到的干涉图信噪比较低时,该方法可以有效地提高合成图像的质量。 相似文献
3.
4.
5.
闭合相位技术、U -V覆盖技术和像重构技术是光学综合孔径干涉成像的三个关键技术。文中简要介绍了光学综合孔径技术的发展历史、这三种关键技术和光学综合孔径望远镜阵的构成 ,对之进行了多光束干涉的计算机仿真和实验仿真 ,两者结果一致说明了光学综合孔径干涉成像技术中有关干涉的理论的正确性 ,指出了下一步的研究方向。 相似文献
6.
7.
《天文研究与技术》2017,(3)
消除综合孔径望远镜子孔径之间的相对光程差是实现高分辨率干涉成像的前提条件,条纹检测法是一种检测相对光程差的有效办法。因子孔径的空间位置排布使干涉条纹具有一定的方向性,若不能精确获知干涉条纹的角度,则无法沿条纹的法线方向行采样,进而无法根据对比度变化曲线的最大值获得子孔径之间的最小光程差位置。提出了一种基于傅里叶变换和图像二值化阈值遍历的获得干涉条纹角度的方法,首先介绍了算法的基本原理,其次通过对条纹角度为43°的仿真数据进行算法验证得到的角度为43.007 8°,与理论值的误差为0.018%,证实了方法的可行性。最后对比了未旋转相机和旋转相机两种情况下的条纹对比度变化曲线,可知通过旋转相机使条纹转至相机靶面纵轴方向再进行采样的办法,更有利于精确得到相对光程差的最小位置。 相似文献
8.
9.
先进天基太阳天文台(ASO-S)是计划于2021年底或2022年上半年发射的中国首颗综合性太阳探测卫星,莱曼阿尔法太阳望远镜(LST)作为ASO-S的有效载荷之一,具体包括莱曼阿尔法全日面成像仪(SDI)、日冕仪(SCI)以及白光望远镜(WST) 3台科学仪器和2台导行镜(GT),其主要目标是在多个波段对太阳上的两类剧烈爆发现象(太阳耀斑和日冕物质抛射)进行连续不间断的高分辨率观测.为了实现这一观测目标, LST所有仪器的观测模式中均包含了一种针对爆发事件而设置的爆发模式.该模式下, SCI将以更高的频率进行图像采集, SDI和WST则以更高的频率对爆发所在区域进行图像采集.测试结果表明,观测图像经过中值滤波、像元合并处理后,可以通过监测图像各像元亮度的相对变化提取爆发事件的时间和位置信息.这些信息将为LST观测模式间的相互切换提供重要电子学输入. 相似文献
10.
11.
The shape of the Earth and of planets depends on the exciting forces and on the rheology of the medium. From the equilibrium equation, we present the main modelisations of the viscous and inviscid fluids and we essentially describe the characteristics of linear viscoelastic deformations, for the Maxwell viscoelastic model of rheology. We use the elastic, viscoelastic and fluid Love numbers in order to investigate the associated relaxation modes. For these various kinds of rheology of the planets interior, we compute the geoid and the topography induced by an internal mass distribution. Finally, we show the importance of this viscoelastic deformation calculations in the study of the celestial body rotations. 相似文献
12.
本文给出UK Schmidt 823天区,23~h47~m<赤经<24~h00~m,赤纬< 00°00′的四分之一区域内Q=4的类星体候选者106个的坐标,B_f~*星等及证认图。对其中Q≥5的天体进行了谱线证认,给出它们的红移值。 相似文献
13.
本文采用了两点相关函数方法,团分析方法(渗流方法)重度函数方法对两个类星体候选者样品进行了类星体成团性的分析。发现与Monte-Carlo无规抽样的平均结果无非常明显的差别,但显示出有尺度为100Mpc的极弱成团性。 相似文献
14.
15.
J. Svoreň 《Earth, Moon, and Planets》1995,68(1-3):539-544
Not considering very rare in situ measurements of cometary nuclei, observations of comets at large heliocentric distances are the only direct source of our knowledge on their sizes. Observations of a cometary nucleus in pure reflected sunlight, at the time when coma is absent, are the way in which the nucleus size can be estimated. Probabilities that extreme observations represent non—active stages of cometary nuclei and also reliability of derived cometary nucleus sizes are investigated. Statistical analysis is based on a sample of 2842 photometric observations of 67 long-period comets observed at large heliocentric distances. For any long-period comet, there is a probability of 2:3 that the sizes derived on the basis of observations at extreme distances are in good agreement with the real nucleus sizes. For new comets in Oort's sense the probability is 3:4 independent of investigated arcs of orbits. For old comets a chance to estimate correct sizes is 1:2 but on the pre-perihelion arc only 1:3. It is also demonstrated that a premature start of activity prior to perihelion or a longer fading after perihelion is more frequent than a short-time isolated activity at large heliocentric distances. 相似文献
16.
引力常数变化对地球自转长期变化的影响 总被引：1，自引：0，他引：1
李林森 《中国科学院上海天文台年刊》2002,(1)
探讨和估计了各种引力常数变化理论对地球角速度和日长变化的影响。各种引力常数变化理论包括了引力常数G随时间、空间以及速度变化等几个方面的影响。另外也估计了对地球自转角速度和日长变化产生的效应。其中有些研究对探讨地球自转变化也有启发意义。 相似文献
17.
大行星轨道运动与太阳黑子数的中长周期变化 总被引：1，自引：1，他引：0
杨志根 《中国天文和天体物理学报》1988,(4)
本文对不同序列的太阳黑子数资料作了分析研究,计算得到了可能的太阳黑子活动的中长周期变化,并分别与由大行星轨道运动引起的日心轨道角动量变化的周期进行比较,发现二者具有比较一致的谱结构。基于本文的讨论和文[17]的结论,我们进一步认为大行星轨道运动是太阳黑子数周期性变化的可能的外部因素。 相似文献
18.
R. Caimmi 《Astronomische Nachrichten》1992,313(3):165-182
This paper investigates the effect of the initial shape of expanding, homogeneous, ellipsoidal density perturbations, at some special stages of evolution, namely at the occurrence of: (i) turn-around along the axes, (ii) maximum volume, (iii) strong decoupling from the Hubble flow, assumed to take place at overdensities equal to unity. To this aim, previous theory is reviewed and extended involving – among others – a deep analysis on the gravitational force induced on the unit mass at the top axes of the ellipsoid, an explicit expression of the overdensity, and a detailed investigation on the limiting cases of flat (two-dimensional) and oblong (one-dimensional) configurations. Then some physical parameters related to the above mentioned stages of evolution are computed for a wide range of initial shapes, in connection with an Einstein-de Sitter universe and an initial overdensity, which is typical for inhomogeneities with galactic masses in a classical CDM scenario. If the gain of spin by tidal torques grows in proportion to time until either the stage of evolution (i) or (ii), or (iii) is attained, it is found a difference in angular momentum related to the initial shape, which never exeeds a factor of about 3.6, 2.0, 1.4, respectively. 相似文献
19.
Magnetars are the neutron stars with the highest magnetic fields up to 1015–1016 G. It has been proposed that they are also responsible for a variety of extra-galactic phenomena, ranging from giant flares in nearby galaxies to fast radio bursts. Utilizing a relativistic mean field model and a variable magnetic field configuration, we investigate the effects of strong magnetic fields on the equation of state and anisotropy of pressure of magnetars. It is found that the mass and radius of low-mass magnetars are weakly enhanced under the action of the strong magnetic field, and the anisotropy of pressure can be ignored. Unlike other previous investigations, the magnetic field is unable to violate the mass limit of the neutron stars. 相似文献
20.
Fred L. Whipple 《Celestial Mechanics and Dynamical Astronomy》1992,54(1-3):1-11
Two indices have been developed for the purpose of comparing the natures of various classes of comets. The first is the Activity Index (AI), measuring the inherent magnitude increase in brightness from great solar distances to maximum near perihelion. The second, or Volatility Index (VI), measures the variation in magnitude near perihelion. Tentative determinations of these two indices are derived from observations by Max Beyer over more than 30 years for long-period (L-P) and short-period (S-P) comets near perihelion and from other homogeneous sources. AI determinations are made for 32 long-period (L-P) comets and for 14 short-period (S-P). The range of values of AI is of the order of 3 to 10 magnitudes with a median about 6. An expected strong correlation with perihelion distance q, is found to vary as q
–2.3. Residuals from a least-square solution (AI) are used for comparing comets of different orbital classes, the standard deviation of a single value of AI is only ±1m.1 for L-P comets and ±1m.2 for S-P comets.Among the L-P comets, 19 of period P larger than 104 years yield AI = 0m.27 ± 0m.25 compared to 0m.39 ± 0m.26 for 13 of period between 102 years and 104 years. This denies any fading with aging among the L-P comets. Also no systematic change with period occurs for the VI index, leading to the same conclusions. Weak correlations are found with the Gas/Dust ratio of comets. No correlations are found between the two indices, nor of either index with near-perihelion magnitudes or orbital inclination.The various data are consistent with a uniform origin for all types of comets, the nuclei being homogeneous on the large scale but quite diverse on a small scale (the order of a fraction of kilometer in extent). Small comets thus may sublimate away entirely, leaving no solid core, while huge comets may develop a less volatile core by radioactive heating and possibly become inactive like asteroids after many S-P revolutions about the Sun. When relatively new, huge comets may be quite active at great solar distances because of volatiles from the core that have refrozen in the outer layers. 相似文献