地震前电磁辐射信息特征研究

反映电磁辐射信息的地震前异常变化很多,但都有一个震前平静－加强－平静然后发震的特征,为了更好地体现这种特征,根据十几年来河北廊坊电磁台网的观测资料,通过给不同强度段的各台日信息量赋予不同的权值,并把当日各台权值累加来反映当日内多台信息量集中的强弱,然后把上述权累加和用一种不连续积分的方法反映异常的持续时间,通过对监测范围内４次Ｍｓ≥５．０地震震例分析,发现该方法反映震前异常特征明显,短临效果很好,     

拱星OH脉泽辐射频谱的双峰结构和多重分离的膨胀拱星壳

对一些OH／IR星的拱星OH脉泽的观测结果表明,在双峰结构谱线轮廓上常常可以发现一些小峰叠加在双峰上,即在谱线轮廓的双峰结构中的每个峰是由几个小峰叠加而成的．从脉泽的辐射转移方程和拱星包层的速度结构出发,研究拱星OH脉泽辐射频谱的轮廓特征,提出多重分离的膨胀拱星亮模型,很好地解释了双峰结构的奇特观测现象．     

Observational limits to source confusion in the millimetre/submillimetre waveband

The first observations to detect a population of distant galaxies directly in the submillimetre waveband have recently been made using the new Submillimetre Common-User Bolometer Array (SCUBA) on the James Clerk Maxwell Telescope (JCMT). The results indicate that a large number of distant galaxies are radiating strongly in this waveband. Here we discuss their significance for source confusion in future millimetre/submillimetre-wave observations of both distant galaxies and cosmic microwave background radiation (CMBR) anisotropies. Earlier estimates of such confusion involved significant extrapolation of the results of observations of galaxies at low redshifts; our new estimates do not, as they are derived from direct observations of distant galaxies in the submillimetre waveband. The results have important consequences for the design and operation of existing and proposed millimetre/submillimetre-wave telescopes: the Planck Surveyor survey will be confusion-limited at frequencies greater than 350 GHz, even in the absence of Galactic dust emission; a 1σ confusion noise limit of about 0.44 mJy beam⁻¹ is expected for the JCMT/SCUBA at a wavelength of 850 μm; and the subarcsecond resolution of large millimetre/submillimetre-wave interferometer arrays will be required in order to execute very deep galaxy surveys.     

Thermalization by synchrotron absorption in compact sources: electron and photon distributions

The high-energy continuum in Seyfert galaxies and galactic black hole candidates is likely to be produced by a thermal plasma. There are difficulties in understanding what can keep the plasma thermal, especially during fast variations of the emitted flux. Particle–particle collisions are too inefficient in hot and rarefied plasmas, and a faster process is called for. We show that cyclo-synchrotron absorption can be such a process: mildly relativistic electrons thermalize in a few synchrotron cooling times by emitting and absorbing cyclo-synchrotron photons. The resulting equilibrium function is Maxwellian at low energies, with a high-energy tail when Compton cooling is important. Assuming that electrons emit completely self-absorbed synchrotron radiation and at the same time Compton scatter their own cyclo-synchrotron radiation and ambient UV photons, we calculate the time-dependent behaviour of the electron distribution function, and the final radiation spectra. In some cases, the 2–10 keV spectra are found to be dominated by the thermal synchrotron self-Compton process rather than by thermal Comptonization of UV disc radiation.     

QINGHAI-XIZANG SURFACE LONG-WAVE RADIATION PARAMETERIZATION WITH ITS CLIMATIC CALCULATION*

In the context of August 1982- July 1983 radiation balance data of the Qinghai-Xizang Plateau, detailed study is made of the relation between the active-surface temperature and surface temperature, proposing two parameterization schemes on surface long-wave radiation(SLWR)of the form U=kδσ(T₀+273)⁴ and U=δσ[(T₀+273)⁴+△T)]⁴, where k and △T are indicated by parameterization equations, separately, others being in conventional notation. Retrieved verification shows the two formulae to be of the same fitting accuracy with the mean relative error of 3.6% and suitable for computing instantaneous and mean flux density, alongside analyzed daily and annual variations of k and △T. Eventually. SLWR in the target area is investigated and its climatic characteristics examined.     

CONCENTRATION AND FLUX OF CO_2, TURBULENCE FLUXES AND RADIATION BALANCE IN THE NEAR SURFACE LAYER OVER WHEAT FIELD

The gradient of CO_2 concentration, photosynthetically active radiation (PAR). net radiation.soil heat flux, profiles of wind speed, and air temperature and humidity were measured above awheat field during May and June 1985 at Beijing Agro-Ecosystems Experimental Station. Beijing,China. Fluxes of carbon dioxide, sensible heat, latent heat and momentum were calculated byusing the aerodynamic method. The observation site. equipment, calibration techniques, theerrors associated with the measurement, and the computational procedures are described. Theresults show that the diurnal variations of amplitude of CO_2 concentrations were 103.8 to 27. 0. 86.3 to 22.8 and 69.8 to 11.6 ppm: the average CO_2 concentrations were 331.5. 339.9 and 364.6 ppmfor the photosynthesis type, and 369.6. 364.0 and 375.2 ppm for the respiration type at 1. 2 and10 m above surface, respectively, from May 14 to June 15. In the daytime, transfer direction ofthe CO_2 fluxes and gradients is from air to crop canopy, and at noon (1100 to 1300 BT (BeijingTime)) the transfer rate reaches negative maximum value. At night, transfer of CO_2 fluxes andgradients is in the reversed direction and reaches positive maximum in the early morning (0400 to0600 BT). There are strong negative correlations between CO_2 flux and the net radiation (Rn),available energy (H LE). photosynthetically active radiation (PAR) and momentum flux (τ).     

卷云与水云的短波透射与反射特性

利用矩阵算法计算了对不同太阳天顶角下不同光学厚度的卷云与水云,在4π空间内0～360o的不同方位与0～90o不同天顶角下的波长为1.39 μm太阳短波波段的透射与反射,其天顶角间隔为5.6o,方位角间隔为5.0o。可以看出两种云透射和反射辐射的差别及它们随着光学厚度变化而变化的情况。同时,将其与波长为0.55 μm的可见光波段的透射和反射进行了比较。     

Evidence of the Link between Broad Emission Line Regions and Accretion Disks in Active Galactic Nuclei

1 INTRODUCTION Most bright active galactic nuclei (AGNs) exhibit broad emission lines, with full width at half maximum (FWHM ≥ 103 km s?1) (Peterson et al. 1999). Some type 1 AGNs could have very broad emission lines (FWHM≥ 20 000 km s?1). Type 2 AGNs s…     

Development dynamics of intense solar proton flares

We consider the relationship of electromagnetic radiation in the three most intense flares of solar cycle 23, more specifically, those of October 28, 2003, January 20, 2005, and September 7, 2005, to the acceleration and release of protons into interplanetary space. The impulsive phase of these flares lasted ～ 20 min and consisted of at least three energy release episodes, which differed by their manifestation in the soft (1–8 Å, GOES) and hard (>150 keV, INTEGRAL) X-ray ranges as well as at radio frequencies of 245 MHz and 8.8 GHz. The protons and electrons were accelerated in each episode, but with a different efficiency; the relativistic protons were accelerated only after 5–6min of impulsive-phase development after the onset of a coronal mass ejection. It is at this time that maximum hard X-ray fluxes were observed in the September 7, 2005 event, which exceeded severalfold those for the other two flares considered. We associate the record fluxes of protons with energies > 200MeV observed in the heliosphere in the September 7, 2005 event with the dynamics of the impulsive phase. The extreme intensities of the microwave emission in the October 28, 2003 and January 20, 2005 events were probably attributable to the high-energy electron trapping conditions and did not reflect the acceleration process.