山东地震前兆台网地下流体数据跟踪分析     

温丽媛  刘春国  陈其峰  王伟  张玲  管贻亮 《内陆地震》2019,(2):166-173

介绍了山东省地震前兆台网地下流体学科数据跟踪分析工作概况,从观测系统、自然环境、场地环境、人为干扰、地球物理事件、不明原因等方面分析了2015年1月至2017年6月跟踪到的非正常变化事件。通过数据跟踪分析,查明了山东区域前兆台网流体学科观测运行的制约因素,提出了合理化建议,以提高观测数据质量。并对荣成鲁32井水温观测数据出现的典型非正常变化事件进行了跟踪分析,判定其为地震前兆异常。  相似文献   

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罗三明  黄曲红  王西宁  陈德立  王太松  张俊青 《大地测量与地球动力学》2009,29(6):93-96

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Evolution of a Coronal Loop System     

G. Tsiropoula  K. Tziotziou  T. Wiegelmann  Th. Zachariadis  C. Gontikakis  H. Dara 《Solar physics》2007,240(1):37-48

The temporal variation of a loop system that appears to be changing rapidly is examined. The analyzed data were obtained on 15 May 1999, with the Transition Region and Coronal Explorer (TRACE) during an observing campaign and consist of observations in the Fe ix/Fe x 171?Å and Fe xii 195?Å passbands taken at a cadence of ～10 min. The special interest in this loop system is that it looks like one expanding loop; however, careful examination reveals that the loop consists of several strands and that new loop strands become visible successively at higher altitudes and lower loop strands fade out during the one hour of our observations. These strands have different widths, densities, and temperatures and are most probably consisting of, at least, a few unresolved thinner threads. Several geometric and physical parameters are derived for two of the strands and an effort is made to determine their 3D structure based on the extrapolation of the magnetic field lines. Electron density estimates allow us to derive radiative and conductive cooling times and to conclude that these loop strands are cooling by radiation.  相似文献   

Oscillations of coronal loops and second pulsations of solar radio emission     

Yu. G. Kopylova  A. V. Melnikov  A. V. Stepanov  Yu. T. Tsap  T. B. Goldvarg 《Astronomy Letters》2007,33(10):706-713

The dispersion properties of the sausage eigenmodes of oscillations in a thin magnetic flux tube are numerically analyzed in terms of ideal magnetohydrodynamics (MHD). The period of the modes accompanied by the emission of MHD waves into the surrounding medium, which leads to acoustic damping of oscillations, is determined by the radius of the tube, not by its length. The dissipation of the sausage oscillations in comparatively high (?0.7R _⊙) and tenuous (?6 × 10⁸ cm^?3) coronal loops is considered. Their Q factor has bound found to be determined by the acoustic damping mechanism. The ratio of the plasma densities outside and inside the loop and the characteristic height of the emission source have been estimated by assuming the quasi-periodic pulsations of meter-wavelength radio emission to be related to the sausage oscillations.  相似文献   

Observation of quasi-periodic pulsations in the solar flare SF 900610     

O. V. Terekhov  A. V. Shevchenko  A. G. Kuz’min  S. Yu. Sazonov  R. A. Sunyaev  N. Lund 《Astronomy Letters》2002,28(6):397-400

A quasi-periodic component was found at the maximum of the X-ray light curve for the June 10, 1990 solar flare detected by the Granat observatory. The pulsation period was 143.2±0.8 s. The intensity of the pulsing component is not constant; the maximum amplitude of the pulsations is ～5% of the total flare intensity. An analysis of the data showed the characteristic size of the magnetic loop responsible for these pulsations to be ～(1–3)×10¹⁰ cm.  相似文献   

太阳活动区冕环若干研究进展     

封莉  甘为群 《天文学进展》2005,23(3):215-225

日冕加热是太阳物理中一个基本问题。随着一批高性能仪器（如TRACE、SOHO、Yohkoh）投入观测，作为太阳日冕中一种基本结构的冕环，其观测资料日益丰富。冕环加热是日冕加热的一个重要组成部分，越来越得到人们的重视。在简要介绍冕环最新观测和研究进展后，以其一维模型为基础，着重讨论了现有冕环加热结构和加热机制的研究进展。  相似文献   

Σ-D Relations and Main Galactic Radio Loops     

Dejan Urošević 《Astrophysics and Space Science》2003,283(1):75-86

This paper represents the updated empirical Galactic andextragalactic Σ-D relations (relations between the surface brightness Σ and the diameter D) for supernova remnants(SNRs), with checking the connection of the main Galactic radio loops (Loop I, II, III and IV) with these relations. We present results which suggest, once again, that the radio loops may have an SNR origin. The updated relations for old SNRs have been measured to have slopes, β ≈ 2 in log-log space. The best Σ-D relations for M31 and M33 galaxies were derived and these relations are shown to be flatter (β ≲2) than those for Galactic SNRs alone. A Σ-D relation with168 reliable calibrators (both Galactic and extragalactic) is derived. This revised version was published online in July 2006 with corrections to the Cover Date.  相似文献   

定天镜的伺服驱动原理     

张竹恒  孙淑琴 《时间频率学报》1996,19(1):23-26

主要介绍恒星光干涉仪实验系统的定天镜伺服驱动原理．采用电细分和逐级升、降速的方法来减小定天镜在转动时的振动，提高定位、跟踪精度．由于应用了４００的电细分和１０００倍的传速比，步进电机的步距角达到０．００６４８°．  相似文献   

Thermal cyclotron radiation from hot coronal loops and peculiarities of the polarization structure of solar microwave emission sources: I. Brightness temperature     

E. Ya. Zlotnik  T. I. Kaltman  O. A. Sheiner 《Astronomy Letters》2007,33(3):168-181

We discuss the possible contribution of the thermal cyclotron radiation from hot coronal magnetic loops to the observed characteristics of the microwave emission from solar active regions. Based on the simplest three-dimensional model of a loop in the shape of a hot torus, we have calculated the expected peculiarities of the frequency and polarization structures of microwave emission sources associated with sunspots and containing coronal loops. Our model calculations of the two-dimensional brightness temperature distributions at various wavelengths for the ordinary and extraordinary modes and the wavelength dependences of the brightness temperatures are presented in the first part of the work. The loop size, the electron density, and the source position on the disk have been found to affect these characteristics. Our numerical calculations of the brightness temperature distributions and spectra have confirmed the well-known assumption that under certain conditions the spectrum of a hot filament can contain cyclotron lines and the sense of the polarization can change over the range. The results obtained here refer to the brightness temperature along the line of sight that crosses the photosphere at a point with given coordinates, i.e., these are the emission characteristics at a fixed point of the source. Integrated characteristics (the flux from the entire source and its polarization) and a discussion of the hot loop model will be given in the second part of the work.  相似文献   

Analysis of Two Coronal Loops with Combined TRACE and SOHO/CDS Data     

J. T. Scott  P. C. H. Martens  J. W. Cirtain 《Solar physics》2008,252(2):293-304

We use an innovative research technique to analyze combined images from the Coronal Diagnostic Spectrometer (CDS) on the Solar and Heliospheric Observatory (SOHO) and the Transition Region and Coronal Explorer (TRACE). We produce a high spatial and temporal resolution simulated CDS raster or “composite” map from TRACE data and use this composite map to jointly analyze data from both instruments. We show some of the advantages of using the “composite” map method for coronal loop studies. We investigate two postflare loop structures. We find cool material (250 000 K) concentrated at the tips or apex of the loops. This material is found to be above its scale height and therefore not in hydrostatic equilibrium. The exposure times of the composite map and TRACE images are used to give an estimate of another loop’s cooling time. The contribution to the emission in the TRACE images for the spectral lines present in its narrow passband is estimated by using the CDS spectral data and CHIANTI to derive synthetic spectra. We obtain cospatial and cotemporal data collected by both instruments in SOHO Joint Observations Program (JOP) 146 and show how the combination of these data can be utilized to obtain more accurate measurements of coronal plasmas than if analyzed individually. Electronic Supplementary Material  The online version of this article () contains supplementary material, which is available to authorized users.  相似文献