Experimental study on the competitive adsorption of metal ions onto minerals

The study on the competitive adsorption shows that the magnitude order of metal ions adsorbed onto oxide and silicate minerals in near-neutral solution with low ionic strength is in mole/nm² as follows: CaCO₃ > quarte > hydromuscovite > kaolinite > Ca-montmorillonite > goethite > gibbsite. These minerals can be divided into three groups according to their surface equilibrium constantsK _M of the adsorption reactions, which are the function of the dielectric constants ε of the absorbent minerals. The relationships between constantsK _M and mineral dielectric constants ε are described as follows: lgK _M ¹ = 7.813-26.15/ε lgK _M ² = 9.030-26.15/ε lgK _M ³ =11.63-26.15/ε for the adsorption reaction: >SO^- + Mⁿ⁺≥SOM^n-1)+ (n = 1, 2, 3) The first group of minerals include quartz, goethite, 1:1 phyllosilicates and other oxide minerals; the second: gibbsite, brucite and 2:1 phyllosilicates; the third: carbonate, sulphate and phosphorate minerals. The appearance reaction constants have a variation of magnitude ±0.5 for different metal ions with the same mineral. This project was financially supported by the National Natural Science Foundation of China (No. 49572091).     

On the nature of the radial velocity variability of Aldebaran: a search for spectral line bisector variations

The shape of the Ti  i 6303.8-Å spectral line of Aldebaran as measured by the line bisector was investigated using high signal-to-noise ratio, high-resolution data. The goal of this study was to understand the nature of the 643-d period in the radial velocity for this star reported by Hatzes & Cochran. Variations in the line bisector with the radial velocity period would provide strong evidence in support of rotational modulation or stellar pulsations as the cause of the 643-d period. A lack of any bisector variability at this period would support the planet hypothesis.
Variations in the line asymmetries are found with a period of 49.93 d. These variations are uncorrelated with the 643-d period found previously in the radial velocity measurements. It is demonstrated that this 50-d period is consistent with an m =4 non-radial sectoral g-mode oscillation. The lack of spectral variability with the radial velocity period of 643 d may provide strong evidence in support of the hypothesis that this variability stems from the reflex motion of the central star due to a planetary companion having a mass of 11 Jupiter masses. However, this long-period variability may still be the result of a low-order ( m =2) pulsation mode as these would cause bisector variations of less than the error measurement.     

Fast variability of the outflow in the Z CMa system

High-resolution, time-resolved spectroscopic observations of Z CMa carried out on 1997 January 14–17 are presented. Large night-to-night and hour-to-hour variations in Hα, Hβ and Na i D P Cygni absorptions, as well as an Hβ emission peak, were observed. Variations in the red wings of the hydrogen emission lines were also detected. The high-velocity wide-emission component on the blue side of Hα appeared on January 17. The observations are discussed in the framework of current wind models.     

Effective collision strengths for fine-structure forbidden transitions among the 2s22p3 levels of Ne iv

Effective collision strengths for electron-impact excitation of the N-like ion Ne  iv are calculated in the close-coupling approximation using the multichannel R-matrix method. Specific attention is given to the 10 astrophysically important fine-structure forbidden transitions among the ⁴S^o, ²D^o and ²P^o levels in the 2s²2p³ ground-state configuration. The expansion of the total wavefunction incorporates the lowest 11 LS eigenstates of Ne  iv , consisting of eight n  = 2 terms with configurations 2s²2p³, 2s2p⁴ and 2p⁵, together with three n  = 3 states of configuration 2s²2p²3s. We present in graphical form the effective collision strengths obtained by thermally averaging the collision strengths over a Maxwellian distribution of velocities, for all 10 fine-structure transitions, over the range of electron temperatures log T (K) = 3.6 to log T (K) = 6.1 (the range appropriate for astrophysical applications). Comparisons are made with the earlier, less sophisticated close-coupling calculation of Giles, and excellent agreement is found in the limited temperature region where a comparison is possible [log T (K) = 3.7 to log T (K) = 4.3]. At higher temperatures the present data are the only reliable results currently available.     

Recombination of helium-like ions – I. Photoionization cross-sections and total recombination and cooling coefficients for atomic helium

A new calculation of photoionization cross-sections is described for the ground and excited states of atomic helium up to principal quantum number n =25 and angular momentum quantum number l =5. These cross-sections are used to calculate total recombination and cooling coefficients for atomic helium for electron temperatures given by log( T )=1(0.2)4.4. A comparison of the threshold photoionization cross-sections obtained here with extrapolations of the highly accurate bound–bound oscillator strength calculations by Drake shows that the new calculations are in error by no more than 1 per cent. The accuracy of the photoionization cross-sections used by previous workers to derive recombination coefficients is also discussed.     

An intensity/linewidth analysis of opacity: first applications to a solar prominence and He II line profiles

An analysis is described which can derive optical thicknesses and associated quantities from measured intensities and linewidths using convenient expressions for photon escape probabilities and for opacity-broadened line halfwidths. An associated analysis of the effect of observational errors is provided. The analysis treats intensities and linewidths independently so that internal consistency of results can provide a measure of observational accuracy, which is shown here to be a stringent requirement. As examples, first applications are made to Si  II lines in a solar prominence and to some high-resolution observations of the solar He  II 303.78-Å resonance line.     

EQUILIBRIUM COASTAL PROFILES:Ⅰ. REVIEW AND SYNTHESIS

naomONProfilesonsandycoastSaresiInilarintheirmorphologyundersjmilarndbotandhydrodynandc(tidaluntandwave)conditions.SuchanobservationhastaltotheconceptofcoastalequilibriunLAssodatalwiththeconceptareanUInbeofcrudelissues,indudingt(i)theevidencetodemonstratetheexisteneeofequilibriny(ii)calculationsoftheshapeofanequilibriumcoastalprofile,and(iii)theperiodoftimerequbotoaschtheequilibriumstate(knownastheresponsetiIne).TherehaveformanyeffortSlookingforsolutionstotheseprobbo,sincethestudAsundCftak…     

EQUILIBRIUM COASTAL PROFILES:Ⅱ. EVIDENCE FROM EOF ANALYSIS

IamODUCTIoNInoIdertoestablishtheconceptofeqUilibriumforbeachprofiles,anuInberofproh-lemsmustbesolved,including:(i)pndoftheealstehceofeqUilibrium;(ii)definitionoftheshapeofaneqUilibriumcOaStalprofile;and(iii)evaluationofthePeriodoftimere-qUiredtoreachtheeqUilibritunstate(knownastheresPOnsetime).Forthefirstoftheseprohlems,areviewofpreviousinvestigationsandaSynhesisarepresentedelsewhere(GaoandCollins,1998).Accowhngtosuchtheoreticalconsidera-tions,threetwrsofeqUilibriurnInayoccurinnatllT…     

我国境外旅游本底趋势线的建立及科学意义

提出了旅游本底趋势线的概念,依据１９７８￣１９９６年共计１９境外客流量统计数据,经过“滤波”订正,建立了外国人,港澳台胞,华侨及境外客流总量４条本底趋势线;利用旅游本底趋势表“晴雨表”功能说明‘８９风波地我国境外旅游业的影响,利用预测功能预估了未来４年我国境外旅游业的发展趋势。