橄榄石高温高压含水效应与光学性质实验研究   总被引：2，自引：1，他引：1  

顾芷娟  孙天泽  张虹 《地球物理学进展》2000,15(4):36-40

高温高压下橄榄石（多晶）含水效应实验表明,水不但可进入矿物孔隙,且能进入其晶格中。从而与原（干）样相比,橄榄石显示了特有的光学性质和红外吸收谱带,矿物比重也下降约０．０２。这些变化可能是上地幔低速层成因的构成因素。  相似文献   

从第22届IUGG大会看地震预测研究     

钱家栋  陈祺福  傅征祥  李丽  吕培苓 《国际地震动态》2000,(4):12-18

1999年 7月 19～ 3 0日 ,第 2 2届 IUGG大会在英国伯明翰大学举行。从提交的论文中可以看出 ,有关地震预测和地震灾害的研究仍是地学界关注的热点问题。文章介绍了这次大会反映出的有关地震预测研究的情况。  相似文献   

Three types of 2-degree field compensating atmospheric dispersion correctors for prime focus     

Xu Wen-li  Wang Ya-nan 《Chinese Astronomy and Astrophysics》1993,17(4):464-472

Three types of prime focus correctors for Chinese 2.16m telescope are introduced in this paper. Each corrector has a 2 degree field and can be used to compensate the atmospheric dispersion of 6″. All the three correctors have excellent image quality and the angles between the principal rays and the optical axes are quite small. There is no special technological difficulty in their fabrication. These designs can not only be used in the 2.16m telescope but also be applied to other large telescopes.  相似文献   

温度对平流层气溶胶光学常数及辐射特性的影响     

张建云  张国栋  许丽生 《成都信息工程学院学报》1993,(4)

本文阐述平流层气溶胶的光学常数在不同温度下取值时,用Mie散射理论对不同浓度的平流层气溶胶红外波段的辐射特性进行的计算和分析。分析结果表明:在卫星遥感中,由温度引起的平流层气溶胶光学常数的变化对某些红外波段的平流层气溶胶辐射特性的影响是不容忽视的。  相似文献   

第21届IUGG大会简介（IAG部份）     

赖锡安  徐菊生 《大地测量与地球动力学》1995,(4)

简要介绍了第２１届国际大地测量与地球物理大会概况和部分专题报告，并着重介绍了ＩＡＧ（国际大地测量协会）组织的学术报告内容以及近年来国际上大地测量学科的新发展。  相似文献   

慢旋转星体结构的微扰方法     

吴雪君  须重明 《天文学报》1996,37(3):254-266

本文用微扰的方法求解在广义相对论框架下，均匀慢旋转的轴对称的稳定星体的结构方程，对旋转的处理精确到角速度的二级近似．并用１０种可能的中子星的物态方程，计算了相应的稳定星体的结构．通过对物态方程Ｇ的详细计算结果，具体讨论了旋转对中子星的结构参量及各种性质的影响．  相似文献   

上海天文台大铯钟的研究与现状     

王关忠 《时间频率学报》1994,(Z1)

本文介绍了上海天文台长铯束管束光学系统改进扫得的７条拉比台跃迁曲线和７条莱姆塞跃过曲线及连续开机四个月得到的数据．  相似文献   

Bounds for mass and rotation of black holes in the observable universe     

A. De Vries  R. Böhme  Th. Schmidt-Kaler 《Astrophysics and Space Science》1995,225(2):221-226

The bounds for the energy change rate of a Maxwell field in the outer space of a rotating black hole, calculated by de Vries (1994) and de Vries (1995), enable us to deduce limits for the rotation and the mass of black holes. For this purpose we assume that a certain part of the anisotropies of the cosmic background radiation is due to absorption or superradiance of black holes (Teukolsky, 1973, Starobinskii and Churilov, 1973). The knowledge of these anisotropies yields bounds for rotation and mass of the black holes in the observable universe.  相似文献   

光干涉测量中光程差的加权最小二乘估计     

肖金宏 《时间频率学报》1992,15(2):126-132

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Magnetic fields of sunspots based on combined optical and radio observations     

V. E. Abramov-Maksimov  G. F. Vyalshin  G. B. Gelfreikh  V. I. Shatilov 《Solar physics》1996,164(1-2):333-343

In the present paper we present the results of measurement of magnetic fields in some sunspots at different heights in the solar atmosphere, based on simultaneous optical and radio measurements. The optical measurements were made by traditional photographic spectral observations of Zeeman splitting in a number of spectral lines originating at different heights in the solar photosphere and chromosphere. Radio observations of the spectra and polarization of the sunspot - associated sources were made in the wavelength range of 2–4 cm using large reflector-type radio telescope RATAN-600. The magnetic field penetrating the hot regions of the solar atmosphere were found from the shortest wavelength of generation of thermal cyclotron emission (presumably in the third harmonic of electron gyrofrequency). For all the eight cases under consideration we have found that magnetic field first drops with height, increases from the photosphere to lower chromosphere, and then decreases again as we proceed to higher chromosphere and chromosphere-corona transition region. Radio measurements were found to be well correlated with optical measurements of magnetic fields for the same sunspot. An alternative interpretation implies that different lines used for magnetic field measurements refer to different locations on the solar surface. If this is the case, then the inversion in vertical gradients of magnetic fields may not exist above the sunspots. Possible sources of systematic and random errors are also discussed.  相似文献