DCMT枢轴误差的光电测定     

朱紫  李志刚 《时间频率学报》1993,(2)

枢轴误差是影响天体位置测量精度的重要因素.对于现代子午环的高精度天体测量而言,枢轴误差的精确测定是必不可少的.利用DCMT的自校准光源的像,并采用V形光栅的光电扫描直接测定DCMT枢轴误差在赤经和赤纬上的分量。通过几次测量结果的比较表明,该方法具有很高的测量精度与重复性.  相似文献   

高精度磁测直接找油方法技术     

周绵远  张工会  郭新顺 《地球科学与环境学报》1992,(2)

本文从成岩磁铁矿理论出发,讨论了油气藏上方的磁异常形态,阐述了利用高精度磁测直接寻找油气田的可能性及其方法技术。文章指出,用磁测直接找油,不仅要提高磁测精度,而且关键在于要能找到并能成功提取与油气藏有关的磁异常信息的方法。文中还列举了引用本文所述方法预测油气田的效果。  相似文献   

初探单片微机改造精密激光测距仪     

刘良刚 《大地测量与地球动力学》1992,(1)

本文从硬件和软件两个方面阐述了用单片微计算机改造我们原先研制的“JCY-3型精密激光测距仪”的试验情况,详细说明了应用单片微计算机管理仪器的工作过程及其用于数据处理的硬件、软件设计。  相似文献   

An upper limit to coronal X-rays from single,magnetic white dwarfs     

Rob Cavallo  Keith A. Arnaud  Virginia Trimble 《Journal of Astrophysics and Astronomy》1993,14(3-4):141-143

Pointed ROSAT PSPC exposures of 9277 and 6992 sec, directed toward the nearby, single, cool, magnetic white dwarfs GR 290 and EG 250 yielded no counts significantly above the expected background rate. The corresponding flux limits (for an assumed source temperature of l keV) are 1.0 and 1.7 × 10⁻¹⁴erg cm⁻² s⁻¹, within the 0.1–2.5 keV bandpass of the instrument (99% confidence limits). This is more than an order of magnitude below the tentative detection level (for GR 290) and limits (for four other similar stars) obtained from archival Einstein data in 1991. The corresponding limits on coronal electron density are comparable with those implied if cyclotron emission is not responsible for any of the features observed in the optical spectra of magnetic white dwarfs. X-ray data currently provide no evidence for the existence of coronae around these stars. A final long observation (25,000 sec of GD 356) is scheduled for later this year on ROSAT, along with coordinated EUVE observations.  相似文献   

Measurement of near surface soil water content using a capacitance probe     

M. Robinson  T. J. Dean 《水文研究》1993,7(1):77-86

The portable surface capacitance insertion probe was used to measure the in situ water content of near surface soil layers. The probe readings were calibrated against gravimetric samples collected over a wide range of water contents, and were found to be very closely correlated. The capacitance probe was used repeatedly in time and space at a field site where ridges and furrows ensured a regular pattern of soil water variations. The observed spatial variations of the water content were related to topography and land mangement. The degree of variability was dependent on the average water content.  相似文献   

流动形变及重磁综合监测断层的研究     

车兆宏  巩曰沐 《大地测量与地球动力学》1995,(4)

分析了目前利用流动形变、重力、地磁复测资料进行地震预测所存在的困难，探讨了综合利用三种手段追踪应力场及地下介质动态的途径，提出了断层综合监测布点的原则，并介绍了依此原则所建的京西试验场的基本情况。  相似文献   

太阳射电微波爆发及其精细结构研究进展   总被引：1，自引：0，他引：1  

李舒浩  王蜀娟  钟晓春 《天文学进展》2005,23(4):331-345

太阳射电微波爆发携带着爆发源区的物理环境及辐射机制等诸多重要信息。其辐射频段较高，通常来自低日冕磁重联区，尤其是微波爆发的精细结构，持续时间短、变化快、结构复杂，可以反映重联过程复杂的磁场结构、高能粒子运动等许多特征。综述了太阳微波射电爆发分类研究的3个主要阶段，介绍了每一阶段的重要爆发类型、物理机制研究及相应的观测设备，讨论了进一步研究的方向。  相似文献   

The efficiency of electron acceleration in solar type-IV radio pulsations with a zebra pattern     

V. V. Zaitsev  E. Ya. Zlotnik  H. Aurass 《Astronomy Letters》2005,31(4):285-290

Based on a comprehensive analysis of the October 25, 1994 event, we consider the balance of energetic particles in a type-IV solar radio emission source with a zebra-type fine structure (in a coronal magnetic loop). The zebra pattern is formed through the injection of fast electrons into a trap and the formation of a ring-type nonequilibrium electron distribution function. We estimated the characteristic zebra-pattern lifetime, which is determined by the escape of fast particles from the trap into the loss cone. In addition, we determined the number of fast particles that must be injected into the trap to provide the observed radio brightness temperature in zebra-pattern stripes by analyzing the plasma emission mechanism responsible for the zebra-pattern generation. As a result, we estimated the efficiency of the electron acceleration mechanism in coronal magnetic loops at the post-flare evolutionary phase of an active region.  相似文献   

Polar Coronal Holes During Solar Cycles 22 and 23     

J.Woch  S.Solanki 《中国天文和天体物理学报》2005,5(5):531-538

Data from the Solar Wind Ion Composition Spectrometer (SWICS) on Ulysses and synoptic maps from Kitt Peak are used to analyze the polar coronal holes of solar activity cycles 22 and 23 (from 1990 to end of 2003). In the beginning of the declining phase of solar cycles 22 and 23, the north polar coronal holes (PCHs) appear about one year earlier than the ones in the south polar region. The solar wind velocity and the solar wind ionic charge composition exhibit a characteristic dependence on the solar wind source position within a PCH. From the center toward the boundary of a young PCH, the solar wind velocity decreases, coinciding with a shift of the ionic charge composition toward higher charge states. However, for an old PCH, the ionic charge composition does not show any obvious change, although the latitude evolution of the velocity is similar to that of a young PCH.  相似文献   

Peculiar oscillations in the microwave emission of Jupiter during the impact of K fragment of comet Shoemaker-Levy 9     

Hari Om Vats  M. R. Deshpande  O. P. N. Calla  N. M. Vadher  B. M. Darji  V. Sukumaran 《Earth, Moon, and Planets》1996,75(2):127-133

In this article we report the peculiar oscillations in the intensity of microwave (4.15 GHz) emission seen during the impact of K fragment of comet Shoemaker-Levy 9 on July 19, 1994. The oscillations begin at 10h 13m 25s UT suddenly with a frequency of ~0.3 Hz and gradually the frequency of these oscillations increases to ~ 1 Hz. The oscillations are not due to local atmosphere or the radio interference from signals of geostationary satellite. They are intrinsic to the microwave emission from Jupiter during the impact of K fragment. Peak-to-peak amplitude of the oscillations is about 34% of the total microwave emission from Jupiter. If we assume that only 50% of the microwave emission is non-thermal and only the non-thermal emission suffered oscillations, then the oscillations are about 68% of the non-thermal emission from Jupiter. The observations also indicate that there are three continuum enhancements during this event and periodic oscillations almost all through. The third enhancement was the largest and during this enhancement there were some additional aperiodic variations. The aperiodic variations were of the order of few minutes and were possibly generated by the gravity waves. The periodic oscillations could be synchrotron emission modulated by the plasma oscillation in the outer magnetosphere. kg]Key words  相似文献