Magnetic Field Strengths and Structures from Radio Observations of Solar Active Regions

Radio observations of some active regions (ARs) obtained with the Nobeyama radioheliograph at λ=1.76cm are used for estimating the magnetic field strength in the upper chromosphere, based on thermal bremsstrahlung. The results are compared with the magnetic field strength in the photosphere from observations with the Solar Magnetic Field Telescope (SMFT) at Huairou Solar Observing Station of Beijing Astronomical Observatory. The difference in the magnetic field strength between the two layers seems reasonable. The solar radio maps of active regions obtained with the Nobeyama radioheliograph, both in total intensity (I-map) and in circular polarizations (V-map), are compared with the optical magnetograms obtained with the SMFT. The comparison between the radio map in circular polarization and the longitudinal photospheric magnetogram of a plage region suggest that the radio map in circular polarization is a kind of magnetogram of the upper chromosphere. The comparison of the radio map in total intensity with the photospheric vector magnetogram of an AR shows that the radio map in total intensity gives indications of magnetic loops in the corona, thus we have a method of defining the coronal magnetic structure from the radio I-maps at λ=1.76 cm. Analysing the I-maps, we identified three components: (a) a compact bright source; (b) a narrow elongated structure connecting two main magnetic islands of opposite polarities (observed in both the optical and radio magnetograms); (c) a wide, diffuse, weak component that corresponds to a wide structure in the solar active region which shows in most cases an S or a reversed S contour, which is probably due to the differential rotation of the Sun. The last two components suggest coronal loops on different spatial scales above the neutral line of the longitudinal photospheric magnetic field.     

H II regions and radio visibility of quasar nuclei

The core (injector) and the jet (relativistic plasma outflow) of AGN objects are surrounded by an ionized medium, an H II region observed in emission lines. The synchrotron radiation from the core and the jet is observed through a thin screen that cocoons the structure under consideration. The screen transparency depends on wavelength and distance from the injector. We consider the objects 3C 345 and 1803+784 whose core emission at decimeter wavelengths is absorption by more than 25 dB. The visible bright compact component is the bright nearby portion of the jet that extends outside the dense part of the screen. We explore the possibility of measuring the screen transparency from absorption in Hα recombination lines with different quantum numbers at centimeter wavelengths.     

Mid-infrared observations of methanol maser sites and ultracompact H ii regions: signposts of high-mass star formation

N -band (10.5 μm) and/or Q -band (20.0 μm) images taken with MANIAC on the ESO/MPI 2.2-m telescope are presented for 31 methanol maser sites and 19 ultracompact (UC) H  ii regions. Most of the maser sites and UC H  ii regions are coincident with mid-infrared (MIR) sources to within the positional uncertainties of ∼ 3 arcsec, consistent with the maser emission being powered by the MIR source. The IRAS source positions, however, do not always coincide with the MIR sources.
Based on an average infrared spectral energy distribution, we deduce that the MIR objects are luminous enough that they should also produce a strong ionizing radiation. Some sources are consistent with stars of later spectral type, but not all can be. A number of maser sites show no detectable radio continuum emission associated with MIR emission, despite a powering source luminous enough potentially to produce an UC H  ii region. Since no signs of an UC H  ii region are detected here, these maser sites might be produced during a very early stage of stellar evolution.
We present objects that show evidence of outflow activity stemming from a maser site, exhibiting CO and/or CS line profiles indicative of outflows coincident with the MIR source. These cases are promising examples of maser sites signposting the earliest stages of high-mass star formation.     

青藏高原西部赛利普中新世火山岩源区:地球化学及Sr-Nd同位素制约

青藏高原拉萨地块西部赛利普地区新生代火山岩依据主量元素可划分为超钾质、钾质和钙碱性系列,主要的岩石类型为粗面安山岩、粗面岩,一个超钾质岩石的40Ar-39Ar年龄为17.58Ma,指示出火山活动为中新世.超钾质、钾质和钙碱性火山岩都显示出富集LREE及LILE(Th、U)、亏损HFSE(Nb、Ta、Ti)的特征.超钾质火山岩具有较高的K2O(6.31%～8.55%)、MgO(6.75%～8.96%)、Cr(270.7×10-6～460.4×10-6)、Ni(142.3×10-6～233.9×10-6)含量,较高的(87Sr/86Sr)i(0.71883～0.72732)和较低的εNd(-14.78～-15.37),指示可能起源于一个前期亏损并经后期俯冲作用改造的富钾的方辉橄榄岩富集地幔源区.钾质火山岩具有比超钾质火山岩低的K2O、MgO、Cr、Ni含量以及高的Ba、Sr含量,初始87Sr/86Sr为0.71553～0.71628,初始143Nd/144Nd为0.51197～0.51198,在空间上与超钾质火山岩共生,可能是前者母岩浆的演化产物.钙碱性火山岩具有较高的Sr(881.7×10-6～1309.2×10-6)、Sr/Y比值(50～108)和较低的Y(12.05×10-6～18.02×10-6),明显亏损重稀土Yb(0.93×10-6～1.30×10-6),类似于典型的埃达克质岩成分特征但相对高钾,并具有相对低的(87Sr/86Sr);(0.70928～0.71374)以及高的εNd(-7.90～-10.91),指示起源于富钾增厚下地壳物质的部分熔融.区域上拉萨地块超钾质岩、钾质岩与N-S向地堑系在空间上共存、时间上相吻合,由此本文认为拉萨地块中新世钾质.超钾质岩和南北向地堑系的形成可能与中新世早期北向俯冲的印度大陆岩石圈断离有关.     

赤潮叉角藻18SrDNA和ITS区序列测定与分析

采用PCR及克隆测序的方法，对1998年引发渤海赤潮的叉角藻18SrRNAadldey DNAITS区（Internal Transcribed Spacer Regions)进行了序列测定与分析。并通过因特网从国际分子生物学数据库中获取甲藻另外15个种的18rDNA序列，以Tetrahymena corlissi作为类群，分别采用Neighbor-Joining和Fitch方法构建甲藻较为一致和可靠的进化树图，探讨具有高度多样性和在分类上争议较多的甲藻各类群之间的形态与分子进化关系。结果表明，Prorocentrum(有2个简单的壳板）出现得较早，而大多数多甲藻目（覆盖着多个壳板）、裸甲藻目（大多数不具壳板）和膝沟藻目的成员较晚出现。另外，对叉角藻ITS区的分析表明，ITS区为高变区，是良好的分子标记，可用于叉角藻快速鉴定的专一性核酸分子探针的研制。     

环台湾岛海域半日潮波特征的三维模拟

用1997版POM海洋模式,首次应用于环台湾岛海域的潮波数值研究.得到该海域的半日潮波主要为23°N以南西太平洋传来的胁振潮.影响台湾海峡的半日潮波分别由海峡南北口传入的两支潮波,且北支强于南支.福建沿岸湄州湾-兴化湾为最强潮区,其M₂分潮最大振幅可达240cm.最强潮流区位于澎湖水道,M₂分潮最大潮流达196cm/s.环台湾岛海域潮波潮流水平结构上除海峡北部原有一个圆流点外,还发现另外存在4个新的圆流点.潮流垂直结构上主要为右偏,接近底层处为左偏.     

干旱区凝结水研究进展

凝结水是维系干旱、半干旱地区主要食物链的水分来源之一,具有重要的生态意义。较详细地列举了目前国内外在干旱区测定凝结量及其持续时间所采用的研究方法,从凝结水的数量特征以及时间格局两方面阐述了不同地域凝结水的时空差异性,并从气象因素、凝结面的类型及其位置、周边植被对其作用等方面综合分析了影响凝结水发生的主要因素,探讨了干旱区凝结水的生态作用及其意义,展望了干旱区凝结水未来的研究趋势。提出在未来的干旱区凝结水研究中应加强与气象学、生态学等多学科的交叉,从能量平衡角度加强对凝结水量的研究;同时,改进和规范凝结水的测量方法,开展荒漠植被对凝结水的生理响应研究以及凝结水对极端干旱胁迫植物的作用研究。