X-ray activity from different types of stars

X-ray emission is an important indicator of stellar activity. In this paper, we study stellar Xray activity using the XMM-Newton and LAMOST data for different types of stars. We provide a sample including 1259 X-ray-emitting stars, of which 1090 have accurate stellar parameter estimations. Our sample size is much larger than those used in previous works. We find a bimodal distribution of the X-ray to optical flux ratio(log(fX/fV)) for G and K stars. We interpret that this bimodality is due to two subpopulations with different coronal heating rates. Furthermore, using the full widths at half maxima calculated from Hα and Hβ lines, we show that these stars in the inactive peaks have smaller rotational velocities. This is consistent with the magnetic dynamo theory that presumes stars with low rotational velocities have low levels of stellar activity. We also examine the correlation between log(fX/fV) and luminosity of the excess emission in the Hα line, and find a tight relation between the coronal and chromospheric activity indicators.     

Stratospheric in situ measurements of H2SO4 and HSO3 vapors during a volcanically active period

In situ measurements of stratospheric H₂SO₄ and HSO₃vapors using passive chemical ionization mass spectrometry were made in October 1982 after the eruption of volcano El Chichon. Data were obtained between about 20 and 41 km showing [H₂SO₄ + HSO₃] sum concentrations between about 10⁴ and 2 × 10⁵ cm^?3 below 29 km and a steep rise above this altitude. Maximum [H₂SO₄ + HSO₃] values of about 3 × 10⁶ cm^?3 are reached above 35 km.Partial [HSO₃] concentrations increase above 34 km reaching about $\text{4 × 10}{}^5\text{cm}{}^{\mathrm{?3}}$ around 40 km. From the measurements it is concluded that H₂SO₄ and probably HSO₃photolysis have an important influence above 34 km leading to the observed increase of [HSO₃] and a depletion of H₂SO₄vapor.It also seems that the data support the view of heterogeneous HSO₃ removal. If correct, this would imply that stratospheric aerosols are formed primarily from HSO₃ rather than H₂SO₄vapor.     

温度和体重对花尾胡椒鲷幼鱼最大摄食量的影响

研究了花尾胡椒鲷幼鱼的最大摄食量与温度和体重的关系。花尾胡椒鲷幼鱼的最大摄食量与体重呈正相关 ,二者的关系为 :Cmax=1 5 95 .3W0 .6 87(Cmax:最大摄食量 ,J/d ;W :体重 ,g)。最大摄食量随温度的变化情况为 :在实验温度为 2 2～ 2 8℃范围内 ,二者呈正相关 ,超过 2 8℃之后呈负相关。最大摄食率与体重的相关关系为 :Rmax=1 5 0 7.6W-0 .313[(Rmax:最大摄食率 ,J/(d·g) ]。采用回归分析 ,建立了由温度和体重预测该种鱼的最大摄食量和最大摄食率的模型 :Cmax=2 86 790e-0 .90 4ln(T3-77.738T2 1985 .185T -16 42 9.710 ) W0 .6 16 　n =1 6 ,r =0 .994Rmax=0 .887e1.2 6 4ln(-T3 78.0 6 1T2 -2 0 0 3.397T 172 36 .5 2 0 ) W-0 .2 83　n =1 6 ,r=0 .978     

选择性滤波同位网格有限差分法在地震波数值模拟中的应用.

引入计算空气声学领域的选择性滤波同位网格有限差分算法（SFFD法）用于二维地震波数值模拟．SFFD法使用经过优化的11点DRP同位网格差分格式,对空间一阶导数进行离散近似,同时采用选择性滤波方法来消除同位网格差分所产生的格点高频振荡,它既提高了数值模拟的精度, 又保证了求解过程的稳定性．数值实验结果表明,SFFD法能够达到O(Delta;x8, Delta;t4)阶交错网格算法同样的精度,同时该方法还具有很强的适应性,能够应用于存在着强泊松比差异的介质模型中,完整地模拟地震波传播过程中各类型的波场,并且对复杂非均匀介质的适应能力也很好．此外,由于避免了交错网格算法在曲线坐标系和一般各向异性介质的数值模拟时所需进行的复杂的插值运算, SFFD法在这些问题上也有着很好的应用前景．      

A large excess of 210Po in the overlying water of the Zhubi Coral Reef flat, in the South China Sea

The temporal variability of ²¹⁰Po and ²¹⁰Pb was examined in the overlying water of the Zhubi Coral Reef flat to detect nutrient-like behavior of ²¹⁰Po. Different mechanisms influencing their geochemical behaviors were observed. Excess ²¹⁰Po relative to ²¹⁰Pb revealed an additional input of ²¹⁰Po other than in situ production from ²¹⁰Pb. The ²¹⁰Po input comes from the reef flat sediment through diffusion. The diffusion contributes 62% of the total ²¹⁰Po. This diffusion of ²¹⁰Po directly highlights its nutrient-like behavior. No input, but the slight removal, of ²¹⁰Pb was observed. Fractionation factors indicate that particulate matter prefers to adsorb ²¹⁰Po rather than ²¹⁰Pb. In combination with particulate composition, ²¹⁰Po diffusion was closely related to organic matter. These results reveal that ²¹⁰Po might be a potential tracer for quantifying nutrient recycling in the Coral Reef system.     

Measurement of aerosol effective density by single particle mass spectrometry

Single particle mass spectrometry has been widely used to determine the size and chemical compositions of atmospheric aerosols; however, it is still rarely used for the microphysical properties measurement. In this study, two methods were developed for determining aerosol effective density by a single particle aerosol mass spectrometer (SPAMS). Method I retrieved effective density through comparison between measured light scattering intensities and Mie theoretical modelled partial scattering cross section. Method II coupled a differential mobility analyzer (DMA) with SPAMS to simultaneously determine the electric mobility and vacuum aerodynamic diameter, and thus the effective density. Polystyrene latex spheres, ammonium sulfate and sodium nitrate were tested by these methods to help validate their effectiveness for determining the aerosol effective density. This study effectively extends SPAMS measurements to include particle size, chemical composition, light scattering, and effective density, and thus helps us better understand the environment and climate effects of aerosols.     

近海地震活动特征及其测震学前兆的某些研究

利用反映震级－频度关系的参量Ｃ值，η值，ｂ值和ｂ值谱以及反映地震空间分布的森下指等研究了近海地震活动的一些主要特征，发现近海强震前地震活动性指标及图象的变化特征与陆地上强震前的特征存在一定差异；给出了新研究的可用于近海及滨海地区强震预报的短期和临震     

底栖有孔虫(Florilus decors)壳体微量元素/钙比值的LA-ICP-MS原位微区分析方法及应用——以长江口外海域为例

深海沉积物中有孔虫壳体的微量元素、同位素测试技术已较为成熟,而河口近海沉积物中有孔虫壳体元素微区测试却鲜有报道。本文报道了一种利用激光剥蚀电感耦合等离子体质谱（LA-ICP-MS）分析法测试取自长江口外沉积物中的有孔虫壳体元素/钙比值的技术,研究了氦气载气流量、能量密度、束斑大小、激光剥蚀频率等参数对测试结果的影响,优化了活体有孔虫原位分析方法。应用确定的测试条件对2016年7月取自长江口外的底栖有孔虫优美花朵虫样品（Florilus decors）进行测试,发现Mg、Sr等元素/钙比值在壳体不同位置上无显著差异,而Mn的数据较为离散,可能与有孔虫生长过程中经历的水环境及其变化有关。     

基于自动探测方法的南海北部涡致海表温度锋面的特征研究

南海北部具有丰富的温度锋面和中尺度涡,它们调节着局地的热量和能量平衡。本文利用卫星海洋高度异常和海表温度数据,并基于自动探测方法,探究了2007年至2017年南海北部中尺度涡边缘的海表温度锋面（涡致锋面）特征。反气旋/气旋边缘出现锋面的概率可达20%。气旋涡在各个方向上出现锋面的概率比较均匀,反气旋涡的东北部和西南部出现锋面的概率大于西北部和东南部。中尺度涡致锋面的数量有明显的季节变化,而涡动能未表现出明显的季节变化。中尺度涡致锋区的总涡动能是中尺度涡内动能的3倍,并且反气旋涡致锋面的总涡动能明显强于气旋涡致锋面的总涡动能。中尺度涡致锋面的数量和涡动能的年际变化与厄尔尼诺南方涛动指数没有明显的相关性。本研究也讨论了中尺度涡致锋面的可能机制,但是中尺度涡对海表温度锋的贡献需要进一步定量研究。     

A Time Evolution Study of the Superhumps of the Dwarf Nova 1RXS J232953.9+062814 by Wavelet Transform

The time evolution behaviour of the superhumps of the dwarf nova1RXS J232953.9+ 062814 is investigated with the wavelet analysis method. On the basis of two nights CCD photometry performed during its first superoutburst as well as other published brightness data, we reveal the superhump's time-dependence as a function of periods and time. Our light curves, which phased in the rapid decay ending portion of the superoutburst and in the dawn of a following normal outburst, are important to help trace the superhump evolution for the star. Both the superhump period and the orbital period of the binary system are detected in the present data. We obtain P _sh=0.0458±0.0002d and P _orb=0.0450±0.0002d. They agree with those existing values. The two periods exchanged their roles during the superhump evolution. The general profile of brightness fading over the outbursts roughly followed an exponential decay law or a form of a five-order polynomial. This revised version was published online in July 2006 with corrections to the Cover Date.