Growth of marine bacteria and ammonium regeneration from substrates in different C: N ratios

Natural assemblages of marine bacteria were chosen in a batch culture experiments. The impact of varying nitrogen substrate concentrations and the substrate C:N ratios (C:N_S) on the bacterial C:N ratio (C:N_B), the bacterial growth efficiency (BGE) and ammonium regeneration was mainly examined. The C:N_S ratios varied from 5:1 (carbon limitation) to 40:1 (nitrogen limitation) with varying combinations of glucose and NO₃^-. The C:N_B ratio had positive relationship with the C:N_S ratio (r=0.93, n=8), whose value was 3.77 when the C:N_S ratio was 5:1 but increased to 6.47 when the C:NS ratio was 40:1. These results indicate that the C:N_B ratio is a potential diagnostic tool for determining the bacterial growth in natural waters controlled by either, carbon or nitrogen. BGE decreased with the declining nitrate concentration and negatively related to C:N_s (r=-0.51, n=8). The average value of BGE was 0.20. This value was a little lower than other reports, which could be induced by the nitrogen source used in our experiments. Finally, regeneration time of ammonium delayed with the increasing C:N_S ratio, which indicates that there were different metabolism mechanisms when bacterial growth was limited by carbon source and nitrogen source.     

雅砻江流域主汛期降水长期预报的一种方法

本文使用天气学方法，从影响雅砻江区域主汛期降水量的长期预报有关因子出发，再运用数理统计方法反复筛选，仅取３个主要因子：西部青藏高原８个站冬春积温，北部冬季极涡面积指数，南部冬季印缅槽平均强度，建立逐步回归预报方程。结果显示：对主汛期６～９月降水量预报拟合准确率为１６／１７即约９４％。回归分析中发现：尽管西太平洋副热带高压对盆地西部降水有很大影响，盛夏且与高原积温有较密切相关，但由放大范围长时段的青藏高原积温，对于雅砻江区域主汛期降水量的影响超过西太平洋副热高压，因而在逐步回归过程中，副高因子仍被剔除．     

The 1978 outburst of the recurrent nova WZ Sagittae

We give the results of photographic observations of the recurrent nova WZ Sge during its 1978 outburst, between December 5 and 25, using the double astrograph of Beijing Observatory. We discuss the observed properties and calculate the total energy released during the outburst to be about 1.07 (+40) erg. We estimate that the next outburst will occur around the year 2011.     

Evidence for the Retrograde Accretion onto Supermassive Black Holestwo

Recently, Sloan Digital Sky Survey successfully carried out the reverberation mapping of a sky area, aiming to test the R ? L relation that has been already widely used. Here, R is the responsivity-weighted radius of the broad line region, and L is the optical luminosity at 5100 Å. Two results have been obtained from the data in the first year: (1) The time lags of AGNs (Active Galactic Nuclei) with a high accretion rate are much shorter than that estimated from the R ? L relation, which confirmed the results of reverberation mapping observations made by the Lijiang 2.4 meter telescope. (2) Some AGNs with a lower accretion rate also have very short time lags. The shortening of the time lags of the AGNs with a low accretion rate is caused by the retrograde accretion of black holes. This result has verified from observations the theoretical prediction made by Wang et al. (2014). The discovery of the black holes with a retrograde accretion has important significance, it indicates that the cosmological evolution of the black holes in quasars is implemented via the inherently random accretion.     

宽波段傅里叶变换太阳光谱仪等光程差采样系统设计

太阳成像光谱探测是诊断太阳大气磁场和热力学参数的主要手段. 傅里叶变换太阳光谱仪(Fourier Transform Solar Spectrometer, FTSS)具有宽波段的优势, 是当前中红外高分辨率太阳光谱探测的最佳选择. FTSS通过采集目标辐射等光程差干涉图, 反演获得光谱图, 等光程差采样的间隔决定了反演光谱波长范围. 因此从FTSS宽波段光谱观测对不同等光程差采样间隔需求出发, 基于现场可编程门阵列(Field Programmable Gate Array, FPGA)技术, 采用全数字分频、倍频方案, 设计了一套宽波段FTSS等光程差采样系统. 采用分布式余数补偿方法, 有效解决了在参考激光干涉信号倍频过程中, 输出采样信号在输出信号周期间误差累积问题, 并降低了输出采样信号的误差及非均匀性; 经功能仿真及实验测试, 系统在200Hz--50kHz频率范围内, 频率误差delta $<$ 0.04%, 可有效满足FTSS的300nm--25μm宽波段的光谱观测数据采集需求, 为后续可见和红外波段FTSS的研制奠定了技术基础.     

太阳活动区的磁场观测

我们利用北京天文台太阳磁场望远镜在1983年投入试观测期间取得的资料,对该年6月份的一群黑子的磁场以及耀斑作了综合分析,得到一些结论。以光球纵场为边界条件,计算了常α无力场。根据挤压无力场耀斑模式,我们认为耀斑爆发的能量,来自异极性黑子的相互靠近。磁中性线的扭曲程度,反映了无力场的状态。     

激变变星中的快速光变

文中综述了激变变星中快速光变的研究进展，讨论了闪变，相干振荡和准周期振荡的观测特征和可能的产生机制。     

Keck II spectroscopy of mHz quasi-periodic oscillations in Hercules X-1

We present Keck II spectroscopy of optical mHz quasi-periodic oscillations (QPOs) in the light curve of the X-ray pulsar binary Hercules X-1. In the power spectrum it appears as 'peaked noise', with a coherency ∼2, a central frequency of 35 mHz and a peak-to-peak amplitude of 5 per cent. However, the dynamic power spectrum shows it to be an intermittent QPO, with a lifetime of ∼100 s, as expected if the lifetime of the orbiting material is equal to the thermal time-scale of the inner disc. We have decomposed the spectral time series into constant and variable components and used blackbody fits to the resulting spectra to characterize the spectrum of the QPO variability and constrain possible production sites. We find that the spectrum of the QPO is best fitted by a small hot region, possibly the inner regions of the accretion disc, where the ballistic accretion stream impacts on to the disc. The lack of any excess power around the QPO frequency in the X-ray power spectrum, created using simultaneous light curves from RXTE , implies that the QPO is not simply reprocessed X-ray variability.     

康普顿化的计算-推广的Kompaneets方程与Monte Carlo方法比较

在X射线天文学以及辐射物理学中,当硬X射线穿过" 冷"的等离子体时所发生的Compton软化是一种重要的辐射转移过程.简要介绍推广的Kompaneets方程,该方程在hv〈mec2及kTe〈mec2较宽松的条件下广泛成立,因此不仅能处理Compton硬化过程,而且也适用于Compton软化过程,后者在目前快速发展的X射线和γ射线天文学中十分重要.基于此方程,我们对天体物理中4种常见辐射谱(Gauss型发射谱线、黑体辐射谱、幂律辐射谱和热轫致辐射谱)在Compton软化情况下的谱演化进行了数值求解,并同Monte Carlo模拟结果做比较,证实了推广的Kompaneets方程的正确性和有效性.最后指出此方程在X射线天文学和γ射线天文学中的重要意义和潜在应用.     

巨分子云的寿命

巨分子云的碰撞造成了大质量恒星在碰撞分子云中的形成,这些大质量恒星的形成产生了膨胀的HII区域,从而使巨分于云碎裂成小质量的分子云。这是本文提出的巨分子云碎裂机制。因此巨分子云的寿命也主要由区分子云间的碰撞几率所决定。我们的分析表明,巨分子云的寿命有赖于巨分子云所在的旋涡星系中的不同位置。寿命的最大可能存在区间为8.18×10~7yr与2.45×10~8yr。利用我们提出的机制可以在分子云研究的数值计算与数值模拟中得到应用。