中等贫金属星的元素丰度分析

给出 １１颗中等贫金属星－１．３ ５［Ｆｅ／Ｈ］ ≤－０．６的观测资料,确定了这些样本星的恒星大气参数,得到了这些星中１４种元素的丰度．讨论了各类元素丰度比随金属丰度的变化。α元素（Ｍｇ、 Ｓｉ、 Ｃａ、 Ｔｉ）相对于铁均表现超丰,每一金属丰度处都存在不同程度的弥散．大部分的铁峰元素（Ｖ、Ｃｒ、Ｎｉ、Ｃｕ）也相对于铁超丰,不随［Ｆｅ／Ｈ］而变化,而［Ｍｎ／Ｆｅ］则随金属丰度的增加而增加．［Ｎａ／Ａｌ］在［Ｆｅ／Ｈ］＞－１．１的样本星中表现超车,在［Ｆｅ／Ｈ］＜－１．１的样本中却明显过贫．     

Wavelength dependence of angular diameters of M giants: an observational perspective

We discuss the wavelength dependence of angular diameters of M giants from an observational perspective. Observers cannot directly measure an optical-depth radius for a star, despite this being a common theoretical definition. Instead, they can use an interferometer to measure the square of the fringe visibility. We present new plots of the wavelength-dependent centre-to-limb variation (CLV) of intensity of the stellar disc as well as visibility for Mira and non-Mira M giant models. We use the terms 'CLV spectra' and 'visibility spectra' for these plots. We discuss a model-predicted extreme limb-darkening effect (also called the narrow-bright-core effect) in very strong TiO bands which can lead to a misinterpretation of the size of a star in these bands. We find no evidence as yet that this effect occurs in real stars. Our CLV spectra can explain the similarity in visibilities of R Dor (M8IIIe) that have been observed recently, despite the use of two different passbands. We compare several observations with models, and find that the models generally underestimate the observed variation in visibility with wavelength. We present CLV and visibility spectra for a model that is applicable to the M supergiant α Ori.     

A spectroscopic study of V603 Aquilae: stellar parameters and continuumline variations

A time-resolved spectroscopic study of V603 Aql (Nova Aquilae 1918) is presented. An orbital period of P _orb=01385±00002, consistent with previous results, and a radial velocity semi-amplitude of K =20±3 km s¹ are obtained from the radial velocity variations of the H emission line. Similar K values are also found in H , H , and He  i emission lines. Using the measured FWHM of the H line and assuming that the derived semi-amplitude is that of the white dwarf, we deduce a most likely mass ratio of q =0.24±0.05 and stellar masses of M ₂=0.29±0.04 M and M ₁=1.2±0.2 M for the secondary and primary (the white dwarf) star, respectively. The dynamical solution also indicates a very low orbital inclination, i =13°±2°. We find that the continuum and line variations are modulated with both the positive and the negative superhump periods, indicating that they arise from similar regions of the accretion disc. Moreover, we find, for the first time from spectroscopy, evidence of negative superhumps in addition to the positive superhumps. Positive superhumps are explained within the disc instability model as caused by an eccentric disc surrounding the white dwarf, which is precessing (apsidal advance) because of tidal instabilities, causing the observed positive superhumps. A nodal precession in the accretion disc is currently believed to be the cause of the observed negative superhumps. The low value of q is consistent with the expected value for systems that show superhumps, in accordance with the eccentric disc model. We find no evidence of periodicity associated with the spin period.     

On the accuracy of the measurements of low-ℓ solar acoustic oscillations

Using a 1154 d long measurement of solar oscillations, obtained by the Global Oscillation Network Group from 1995 June 10 to 1998 August 6, we study the dependence of the accuracy of radial p-mode parameters on the duration of the observations. It is shown that relatively rare pulses of large power lead to the decrease of the accuracy achievable for a given duration of the observations and it is usually underestimated. The corresponding correction factor to the Libbrecht formula for a frequency accuracy estimation is provided. We have also investigated the influence of the solar activity on the mode parameters soon after the solar activity minimum. There is a clearly visible increase of the radial p-mode power in the beginning of the new solar cycle while the mode frequency variations are within the corresponding error bars.     

DISCUSSION: APPLICATION OF THE QDa–Md METHOD OF ENVIRONMENTAL DISCRIMINATION TO PARTICLE SIZE ANALYSIS OF FINE SEDIMENTS

Duck's recent finding (R. W. Duck, Earth Surface Processes and Landforms, 1994, 19 , 525–529) that QDa and Md parameters derived from pipette and SediGraph analysis of sediments from Loch Tummel returned similar results can be interpreted in two ways. The observed consistency could result from (i) a general agreement between the methods (as is suggested by Duck) or (ii) from the use of inappropriate parameters (Md and QDa) to describe polymodal distributions.     

姚安地震序列与大姚地震序列震源参数的对比研究

2000年1月15日在云南省姚安县发生了M_S6.5地震, 2003年7月21日和10月16日在云南省大姚县发生了M_S6.2、 M_S6.1地震。 这两个地震序列均发生在滇中块体, 震中位置相距42.5 km, 构造、 应力背景相似, 但序列类型不同, 时间间隔短。 为深入研究姚安地震和大姚地震序列的特征, 根据昆明区域数字台网记录的数字地震波资料, 利用遗传算法计算了2000年姚安地震和2003年大姚地震序列的震源参数。 研究结果表明, 姚安地震序列和大姚地震序列的地震矩和近震震级有很好的线性关系, 它们的地震矩M₀均在10¹²~10¹⁴ N·m, 地震矩与震源半径之间呈线性关系。 应力降随震级变化不明显。 拐角频率和地震矩之间有明显的依赖关系, 用最小二乘法拟合拐角频率和地震矩的关系式, 利用此关系式可计算出给定地震矩的拐角频率估计值f_a, 进而可分析实际计算的拐角频率与估计值之差(f_c-f_a)的时间变化曲线。 姚安地震序列和大姚地震序列实际计算的拐角频率与估计值之差(f_c-f_a)及应力降随时间的变化表现出了不同的特征: 姚安地震序列的应力降和拐角频率差值在4.3级和4.6级强余震前均有一个上升-下降过程, 反映余震区应力场有一个增高-下降过程; 大姚地震序列应力降和拐角频率差值在M_S≥4.6强余震发生之前均会出现高值异常, 但在M_S4.6～4.7地震之前出现的高值异常持续时间短, 在M_S6.1地震前出现的高值异常持续较长。 文中结合两个地震的发震构造, 序列类型等特征进行了分析讨论。     

福建及沿海地区地震活动力源探讨

综合地震震源机制解和地壳形变观测资料的研究, 求得福建及其沿海地区现代震源应力场, 认为这与台湾地区、 台湾海峡应力场相互衔接, 主压应力轴优势方位为NW-SE向, 力轴仰角较小, 应力场近于水平挤压, 形变场反映近期福建沿海亦受北西方向, 接近与海岸垂直的挤压力。 进一步分析该区域内的断裂构造特征和地震活动强度由东至西逐渐减弱的规律, 认为菲律宾海板块与欧亚板块的相互作用力不仅是台湾强震力源所在, 而且其影响向西扩展, 福建及其沿海地区地震活动主要力源仍然是来自这两大板块的相互作用力。     

2004年印尼8.7级强震前昌黎台的远场电性异常特征探讨

分析了在2004年12月26日印尼8.7级地震前河北昌黎台记录到的自然电位及电场异常, 结果显示昌黎台自电位、 电场正常时段观测到的半日、 半月潮汐波周期变化在震前1个多月发生畸变, 周期消失, 变化幅度相应减小, 震后快速恢复, 且潮汐波记录比震前正常时段更加清晰。 该台地电阻率的观测结果显示起始下降变化比较平缓, 震前一周左右, 变化加剧, 出现多次阶变。 究其原因, 在强震发生前断层的蠕滑作用导致孔隙压力变化, 产生一种可以在岩石中传播的应变波, 由于台站下方岩土层对小应变信号具有很好的放大作用, 所以记录到了这种小幅度的应变波, 也就是远场的静态应变效应。 随着地震临近, 应力作用加强, 远程应变波引起台站下方水位、 水化学性质以及岩石孔隙度、 渗透率等的改变, 导致电阻率、 电场大幅度的阶变, 这反映了远场应变波的动态效应。 当然就异常幅度而言, 应变波的效应还嫌弱一些, 因此昌黎台异常变化可能还叠加了震源区激发的电磁波。     

京津冀地区井水温度的数字化观测及其地震前兆监测效能的评估

较为系统的分析了北京、 天津、 河北地区井水温度观测现状及年、 月、 日不同层次上的动态特征, 及其在相关的地震前兆监测中发挥效能的可能性做了宏观的评估。 评估结果表明, 74.7%井的水温观测正常运行, 58.6%的井在地震中期或中短期的前兆监测发挥效能, 67.8%的井在地震短期前兆监测发挥效能, 41.2%的井在地震短临前兆监测中有可能发挥一定效能。 文中还提出了进一步发挥井水温度观测监测效能的若干建议。