New and little‐known arietellidae (Copepoda: Calanoida) mainly from the south‐west pacific

Three species of Arietellidae are described from the south‐west Pacific: a new species of Paraugaptilus, a species which can not be separated from P. buchani, and Arietellus aculeatus. The identity of A. aculeatus is clarified by comparison of type material and material from the U.S. National Museum of Natural History, and an unidentified Atlantic species of Arietellus, evident from the comparison, is described.     

Weed preference and growth of young grass carp in New Zealand

In each of eight 5‐day pond experiments carried out at intervals over a year, 0+ to 1 +‐year‐old grass carp, Ctenopharyngodon idella Val., were offered a choice of at least 10 species of water weeds from the Rotorua area. Water temperature was measured each day. Food selectivity decreased with increasing temperature and size of fish, but preference for the weeds did not change. At summer temperatures the fish ate much weed and grew at about 4g/fish/day, but in winter little food was taken and growth was slow.     

南海3种小型砗磲的外壳形态差异分析

本研究对中国南海3种小型砗磲(Tridacnaspp.)[番红砗磲(Tridacnacrocea,包括2种外壳形态)、长砗磲(Tridacna maxima)和诺亚砗磲(Tridacna noae)]的外壳形态性状进行生物统计学差异分析。研究表明,4组砗磲外壳存在显著形态学差异。单因素方差分析发现9个外壳比例性状能够较好区分3种砗磲,且2种不同外壳形态的番红砗磲在壳宽/壳长、足丝孔宽/壳长、壳质量/壳长和左右壳厚比壳长存在显著性差异(P<0.05);在基于欧氏距离Ward法且指定聚类数k=4的条件下,4组砗磲层次聚类效果较好;主成分分析提取3个主成分建立散点图,累计主成分贡献率73.85%,各主成分贡献率依次为50.47%,13.78%和9.60%;线性判别分析得出3个判别函数,方差解释率依次为70.13%、20.97%和8.90%。3种多元统计方法从不同角度解释各组砗磲的外壳形态差异,结果均显示两组番红砗磲的外壳形态更为接近,同时长砗磲与诺亚砗磲的外壳形态较为接近。     

Gigamasers: the key to the dust-obscured star formation history of the Universe?

A numerical model of the Leonid stream is developed, based on an earlier model which has been applied to the Perseid stream. The results for this model are applied to the 2001 Leonid return. By examining the full three-dimensional dispersion of individual 'streamlets' released from the Leonid parent comet, 55P/Tempel–Tuttle, we have derived an estimate for the temporal change in spatial density of each trail. Using this result along with an estimate for the location of the centres for individual streamlets and fits to previous Leonid storm profiles, we estimate that the activity from the shower will be broad and relatively strong (zenithal hourly rates perhaps in excess of 1000). In particular, streamlets from the 1766 and 1799 ejections contribute to activity peaking near 10 and 12 ut on 2001 November 18, respectively. Additional older material from 1633, 1666 and 1699, as well as more recent ejections from 1866 and 1833, contributes to a much broader secondary maximum near 17.5 ut on November 18. Comparison with other published models of predicted Leonid activity in 2001 shows general agreement in terms of timing, but the models differ significantly in terms of the relative magnitude of the activity (which other models suggest will be larger). Significant anisotropy in the impact hazard exists for satellites in the geostationary belt, with those over western longitudes most likely to be affected. Integrated fluences for the 2001 Leonid return suggest a hazard of order one magnitude greater than occurred for the 1999 Leonid storm.     

The magnitude distribution, perihelion distribution and flux of long-period comets

The mass distribution and perihelion distribution of long-period comets are re-assessed. The mass distribution index is found to be 1.598±0.016 , indicating that the distribution is somewhat steeper than was obtained by previous analyses of an amalgam of all the available historical data. The number of long-period comets that have orbital perihelion distances, q , that fall in a specific q to q +d q range is found to be independent of q . It is also noted that the flux of long-period comets to the inner Solar system has remained constant throughout recorded history.
The number of long-period comets, , per 1-au interval of perihelion distance, per year, brighter than H , entering the inner Solar system is found to be given by log₁₀ =−2.607+0.359 H . It is therefore estimated that, for example, about 0.5, 30 and 2000 long-period comets with absolute magnitudes brighter than 0, 5 and 10 respectively pass the Sun on orbits with perihelion distances less than 2.0 au, every century.     

O-rich SR and Mira variables in DENIS

Previous VLA observations of the triple radio continuum source in Serpens showed that it has very unusual and extraordinary characteristics. While this source is associated with a star forming region, its outer components exhibit a combination of thermal and nonthermal spectra and large proper motions, Furthermore, the NW lobe has knotty and extended emission connecting the central source with the bright outer knot. Here, we present results of new VLA radio continuum high-angular resolution observations of this Radio Jet. Combining these observations with those obtained previously, we find that: a) one of the knots along the main body of the radio jet (knot G) exhibits proper motions similar to those observed in the outer NW and SE components, and the time variable knot A; b) the outer knots are moving away from the central source in slightly different directions; and c) the orientation of the central source seems to change with time. These results are consistent with a central precessing source that undergoes periodic ejection of material.     

Evidence for Chemical Heterogeneity in the Nucleus of C/1995 O1 (Hale–Bopp)

We present an analysis of OH, CN, and C₂ jets observed in thecoma of Comet Hale–Bopp on UT April 22, 23, and 25, 1997. Monte Carlomodels designed to simulate the gas jets were employed to analyze thenuclear active areas responsible for the observed coma gas jets. Ourresults indicate that four active areas are necessary to reproduce theCN and C₂ jets while five active areas are required to simulatethe OH jets. The additional OH active area must produce significantlevels of OH, but cannot emit measurable quantities of either carbonradical. This difference suggests that the nucleus of Comet Hale–Boppis chemically heterogeneous.     

西藏知不拉和浪母家果矽卡岩铜矿地质特征及驱龙-知不拉-浪母家果成矿系统的确定

西藏驱龙巨型斑岩铜钼矿床周围产出有知不拉与浪母家果矽卡岩铜矿。通过揭示知不拉和浪母家果的地质特征、成矿侵入体的地球化学特征和硫同位素特征,结合前人的年代学资料,确立两者与驱龙斑岩铜矿共同构成斑岩-矽卡岩成矿系统。结果显示知不拉与浪母家果矽卡岩矿床中的侵入岩地球化学特征与驱龙矿区的侵入岩地球化学特征相似,属于准铝质、钙碱性-高钾钙碱性岩石;稀土元素表现为强烈的LREE和HREE的分异,除知不拉的细晶岩有很强的Eu负异常,其他具有很弱的Eu负异常;明显富集大离子亲石元素(LILE)和高场强元素(HFSE),K、Pb的正异常,Ta、Nb、Ti的负异常。知不拉硫化物硫同位素与驱龙斑岩铜钼矿的硫同位素相比有明显的差异,这样的差异可能是由于成矿热液氧逸度的变化和晚期高δ34S值的天水加入造成的。研究确立驱龙-知不拉-浪母家果斑岩-矽卡岩成矿系统,主要基于:时代相近,空间毗邻;驱龙斑岩铜矿花岗闪长岩接触带发育有明显矽卡岩矿化;与矿化有关的侵入岩地球化学特征相似性;成矿物质演化趋势相似;矽卡岩连续演化的物理化学条件。而钙质围岩、多期次侵位且侵位较浅的岩浆与区域内构造活动及矿区内断裂、裂隙发育,共同决定了斑岩-矽卡岩系统的产出。