Search for interstellar superheavy hydrogen

Models for fundamental physical interactions allow for the existence of stable or nearly stable elementary particles much heavier than the proton. Stellar spectra were searched for a positively charged superheavy particle, X(+), which, with a bound electron, should appear as apparently superheavy neutral hydrogen in the interstellar medium. An upper limit for the abundance of X relative to normal hydrogen in the line of sight toward the bright star gamma Cassiopeiae is 2 x 10(-8).     

Superheavy elements: an early solar system upper limit for elements 107 to 110

The abundance of samarium-152 in the Santa Clara iron meteorite is found to be 108 x 10(7) atoms per gram. This quantity, if attributed to fission of a superheavy element with atomic number 107 to 109, limits the amount of superheavy elements in the early solar system to 1.7 x 10(-5) times the abundance of uranium-238. For element 110, the limit is 3.4 x 10(-5).     

Barium isotopes in allende meteorite: evidence against an extinct superheavy element

Carbon and chromite fractions from the Allende meteorite that contain isotopically anomalous xenon-131 to xenon-136 (carbonaceous chondrite fission or CCF xenon) at up to 5 x 10(11) atoms per gram show no detectable isotopic anomalies in barium-130 to barium-138. This rules out the possibility that the CCF xenon was formed by in situ fission of an extinct superheavy element. Apparently the CCF xenon and its carbonaceous carrier are relics from stellar nucleosynthesis.     

Zodiacal dust and deep-sea sediments

The recent detection of radioactive Al(26) in marine sediments has led to the conclusion that it is brought into the earth's atmosphere by micrometeorites which have been exposed, in interplanetary space, to solar high-energy protons. The Al(26) method is not precise enough to yield directly a reliable value for the mass accretion rate to the earth to better than about 3 orders of magnitude, but is sufficiently accurate to allow a crucial decision between two widely differing of interplanetary dust which have been proposed to explain observations of the zodiacal light. The two models lead to Al(26) concentrations which would differ by about 5 orders of magnitude. Thus, the presence of Al(26) is consistent with the zodiacal dust model with particles of some tens of microns rather then with submicron particles. From this model a mass accretion to the earth then be calculated which is set at 1250 (upper limit, 2500; lower limit, 250) tons per day, or 2.8 x 10(-15) g/cm(2) sec, or 4.5 x 10(11) g over the earth per This value does not depend on the flux of the solar high-energy particles, which may be uncertain by an order of magnitude or more. The presence of Al(26) supports the idea that an important fraction of the dust is stony in composition material density, and thus eliminates some more exotic dust models, as such one consisting entirely of carbon grains. We may also conclude that the accreted dust particles have been in the solar system and exposed to protons from solar high-energy particles for a time interval which is greater than a significant of the Al(26) half-life (0.74 x 10(6) years).     

稻叶瘟病斑类型、日龄及温湿度对产孢影响的定量研究

文中报道了关于稻叶瘟病斑田间产孢若干问题的初步定量研究结果。研究表明:扩展型、中间型、停滞型病斑的产孢潜能比值约为100:30～40:5;病斑日龄(x)与病斑产孢潜能(y)的关系可用下式表达:y=1.04-|ln(0.5x+1.8)-1.57|,气温(t)与病斑相对产孢量(y)的关系可用下式表达:令x=4×(t-10),则y=sin(0.317857x+0.008125x~2+0.000067x~3);空气相对湿度(x)与病斑相对产孢量(y)的关系可表达为y=-1004+11.04x(x≥91％);依据保温保温时间(x)来推算叶温病斑相对产孢量(y)的计算式为:y=-12.96+4.42x(24>x>4)。上述研究结果为组建以田间病斑产孢为重要子模型的稻叶瘟流行模拟模型提供了基础资料。     

A direct measurement of the terrestrial mass accretion rate of cosmic dust

The mass of extraterrestrial material accreted by the Earth as submillimeter particles has not previously been measured with a single direct and precise technique that samples the particle sizes representing most of that mass. The flux of meteoroids in the mass range 10(-9) to 10(-4) grams has now been determined from an examination of hypervelocity impact craters on the space-facing end of the Long Duration Exposure Facility satellite. The meteoroid mass distribution peaks near 1.5 x 10(-5) grams (200 micrometers in diameter), and the small particle mass accretion rate is (40 +/- 20) x 106 kilograms per year, higher than previous estimates but in good agreement with total terrestrial mass accretion rates found by geochemical methods. This mass input is comparable with or greater than the average contribution from extraterrestrial bodies in the 1-centimeter to 10-kilometer size range.     

Luminescence of apollo 11 lunar samples

Luminescence measurements were made of four lunar rocks, two terrestrial rocks (granite and gabbro), and one terrestrial mineral (willemite) by comparing the spectral curves with the curve of a barium sulfate standard. Efficiencies with 3000 angstrom excitation were < 6 x 10(-5) for the lunar samples, < 8 x 10(-5) for gabbro of very similar composition to the lunar samples, approximately 10(-4) for granite, and approximately 2 X 10(-2) for willemite. If these are typical values for other ultraviolet excitation wavelengths, the Apollo 11 site appears to contribute little to the observed lunar luminescence.     

Paramagnetic unit in spinach subchloroplast particles: estimation of size

A pulsed ruby laser (wavelength, 694.3 nanometers) was used to measure the dependence on light intensity of light-induced electron paramagnetic resonance (ERR) signal 1 for short flashes of uniform duration (400 microseconds). Approximately 10(18) photons per square centimeter per flash from the unattenuated beam were available to the sample of subchloroplast "system 1" particles from spinach. The experimental dependence of the EPR signal height plotted as a function of the total number of incident photons per flash was exponential. From measurement of the slope at a very low relative photon flux and the saturated EPR signal amplitude, the value for the cross section or "effective size" of the light-induced paramagnetic unit, sigma(EPR), was found to be 300 x 10(-17) square centimeter. This result is compared with a measured optical absorption cross section, sigma(694nm), of 2.5 x 10(-17) square centimeter, for the identical sample at the laser wavelength. The hundredfold difference in size supports the thesis that the paramagnetic state is a property of an aggregate of chlorophyll molecules of the same general size as the photosynthetic unit.     

草莓种质资源果实主要数量性状变异及概率分级

通过对草莓种质资源的主要数量性状进行分析研究,得出了草莓果实主要数量性状的变异情况,并且对这些数量性状进行K-S检验,对符合正态分布的数量性状统一用(X-1.2818s)、(X-0.5246s)、(X 0.5246s)和(X 1.2818s)4个点分为5级,从而使性状值落入1~5级的概率分别为10%、20%、40%、20%和10%;或用(X 0.5246s)和(X 1.2818s)2个点分为3级,性状值落入3级的概率分别为30%、40%和30%。     

Solar particle tracks in glass from the surveyor 3 spacecraft

A glass filter from Surveyor 3 has a surface density of approximately 1 x 10(6) tracks per square centimeter from heavy solar flare particles. The variation with depth is best fitted with a solar particle spectrum dN/dE = 2.42 x 10(6) E(-2) [in particles per square centimeter per year per steradian per (million electron volts per nucleon)], where E is the energy and N is the number of particles, from 2 million electron volts per nucleon to approximately 7 million electron volts per nucleon and dN/dE = 1.17 x 10(7) E(-3) at higher energies. Not much difference is observed between 0.5 and 5 micrometers, an indication that there is a lack of track-registering particles below 0.5 million electron volts per nucleon. The Surveyor data are compatible with track results in lunar rocks, provided an erosion rate of approximately 10(-7) centimeter per year is assumed for the latter. The results also suggest a small-scale erosion process in lunar rocks.     

The ancient lunar core dynamo

Lunar paleomagnetism provides evidence for the existence of an ancient lunar magnetic field generated in an iron core. Paleointensity experiments give a surface field of 1.3 gauss, 4.0 x 10(9) years ago, subsequently decreasing exponentially. Thermodynamic arguments give a minimum value of the heat source in the core at that time: known sources, radioactive and other, are quantitatively implausible, and it is suggested that superheavy elements were present in the early moon.     

Herpes simplex virus: dry mass

Dry mass of herpes simplex virus particles was measured by quantitative electron microscopy after isolation by surface spreading and critical-point drying of infected cells. The core weighed about 2 x 10(-16) gram, the empty naked capsid 5 x 10(-16) gram, the full naked capsid 7 x 10(-16) gram, and the enveloped nucleocapsid 13 x 10(-16) gram.     

Isotopic abundances of actinide elements in lunar material

The abunldanzces of uranium and thorium were measured mass spectrometrically as 0.59 +/- 0.02 and 2.24 +/- 0.06 parts per million, respectively, in the fines of Apollo 11 builk sample. The ratio (235)U/(238)U was 0.007258 +/- 0.000016, in agreement with terrestrial uranium. The following upper limits were set: (236)U/(238)U相似文献   

Carbon Dioxide Transport by Ocean Currents at 25{degrees}N Latitude in the Atlantic Ocean

Measured concentrations of CO(2), O(2), and related chemical species in a section across the Florida Straits and in the open Atlantic Ocean at approximately 25 degrees N, have been combined with estimates of oceanic mass transport to estimate both the gross transport of CO(2) by the ocean at this latitude and the net CO(2) flux from exchange with the atmosphere. The northward flux was 63.9 x 10(6) moles per second(mol/s); the southward flux was 64.6 x 10(6) mol/s. These values yield a net CO(2) flux of 0.7 x 10(6) mol/s (0.26 +/- 0.03 gigaton of C per year) southward. The North Atlantic Ocean has been considered to be a strong sink for atmospheric CO(2), yet these results show that the net flux in 1988 across 25 degrees N was small. For O(2) the equivalent signal is 4.89 x 10(6) mol/s northward and 6.97 x 10(6) mol/s southward, and the net transport is 2.08 x 10(6) mol/s or three times the net CO(2) flux. These data suggest that the North Atlantic Ocean is today a relatively small sink for atmospheric CO(2), in spite of its large heat loss, but a larger sink for O(2) because of the additive effects of chemical and thermal pumping on the CO(2) cycle but their near equal and opposite effects on the CO(2) cycle.     

金露梅株丛的植物量及其空间分布的研究

研究了东祁连山金露梅株丛的植物量形成规律,空间分布特点及其与立地类型的关系。结果表明,地上植物量８月底最高,６月生长最快,１０月凋落速度最快。年凋落量是年增量的７２％左右。株丛植物量Y与株丛分枝数Ｘ１、丛高Ｘ２、株丛投影面积Ｘ３成正相关关系,可用多元线性回归方程Ｙ干质量＝－３２５.３４６十１０．４２１Ｘ2＋０.１１０Ｘ３（ｒ＝０.８５７,Ｐ＜０.０１）或Ｙ鲜质量＝２１０.６３７＋７.２１８Ｘ1＋１.４００Ｘ２＋０．０８７Ｘ３（ｒ＝０．８７２．Ｐ＜０．０１）来估测,估测精度分别为９１．２％和９５.８％。地上植物量的８０％分布于０～３０ｃｍ高度内,地下植物量的８５％集中分布于０～２０ｃｍ的土层中。株丛地下植物量３７８．９ｇ／ｍ２·ＤＭ是地上植物量３２６.６ｇ／ｍ２ＤＭ的１．２倍,地下部分所占空间是地上的３５～１０.２倍。不同立地条件下金露梅株丛的分枝数不同,单枝质量差异很大。     

Dust measurements in the coma of comet 81P/Wild 2 by the Dust Flux Monitor Instrument

We present measurements of the dust particle flux and mass distribution from the Stardust Dust Flux Monitor Instrument (DFMI) throughout the flyby of comet 81P/Wild 2. In the particle mass regime from 10(-14) to 10(-7) kilograms, the spacecraft encountered regions of intense swarms of particles, together with bursts of activity corresponding to clouds of particles only a few hundred meters across. This fine-scale structure can be explained by particle fragmentation. We estimate that 2800 +/- 500 particles of diameter 15 micrometers or larger impacted the aerogel collectors, the largest being approximately 6 x 10(-7) kilograms, which dominates the total collected mass.     

利用基于单链抗体的BIAcore技术检测蔬菜中的杀螟硫磷残留

为建立一种基于单链抗体的蔬菜中杀螟硫磷残留快速检测方法,测定了前期通过核糖体展示所获得的抗杀螟硫磷单链抗体的亲和力和特异性,并建立了基于该抗体和BIAcore X系统检测蔬菜样品中杀螟硫磷的方法。结果表明,获得3株高亲和力单链抗体,其与杀螟硫磷的解离平衡常数分别为4.56×10~(-10)、1.42×10~(-9)、2.66×10~(-10)mol/L,与除对硫磷外的其他有机磷农药的交叉反应率0.1%(与对硫磷的交叉反应率≤2.8%),说明获得的单链抗体对杀螟硫磷具有很高的特异性。样本添加回收率试验结果显示,该方法的平均回收率介于95.8%~102.2%,相对标准偏差(RSD)≤2.13%,说明该试验方法可靠,可用于实际蔬菜样品中杀螟硫磷的快速检测。     

种植密度与施肥技术对一年生盾叶薯蓣产量及效益的影响

[目的]探究种植密度和施肥技术对一年生盾叶薯蓣产量和效益的影响。[方法]选择盾叶薯蓣种植密度、氮肥用量和钾肥用量3个因素,采用二次饱和D-最优设计,布置田间参数试验,针对鲜盾叶薯蓣产量和净产值2个目标函数,分别研究、建立相应的回归数学模型,并据此进行综合分析,提出该试验条件下3个供试农艺因子的取值方案。[结果]种植密度(x1)、尿素用量(x2)、硫酸钾用量(x3)与鲜盾叶薯蓣产量(y1)的回归方程为:y1=5 692.95-176.85x1+1.05x2+158.70x3+121.95x12-332.40x22-449.40x32-238.50x1x2+24.45x1x3-390.75x2x3;种植密度(x1)、尿素用量(x2)、硫酸钾用量(x3)与鲜盾叶薯蓣净产值(y2)的回归方程为:y2=2 524.35+1 422.15x1-635.85x2-421.95x3+183.00x12-498.60x22-673.95x32-357.75x1x2+36.60x1x3-586.05x2x3。[结论]提高盾叶薯蓣种植密度,以及中等或中等偏上水平的氮肥和钾肥用量,有利于增产;而降低盾叶薯蓣种植密度、氮肥用量和钾肥用量却有利于净产值的提高。     

基于水稻根伸长的不同土壤中镉（Cd）毒性阈值（ECx）及预测模型

【目的】虽然土壤中镉（Cd）污染对水稻的生态风险受关注已久,然而大量研究集中在基于稻米中Cd限量标准的健康风险研究,而针对土壤中Cd污染的生态风险阈值研究较少。研究通过ISO11269-1根伸长毒性测试方法,测定不同性质土壤中Cd对水稻的毒性阈值（ECx,x=10,50）及其预测模型,以期为基于生态毒理效应的中国土壤Cd污染基准值的修订提供参考。【方法】采用中国8种不同性质农田土壤和3种不同Cd敏感性差异的水稻品种（T优167,T167;陆两优28,L28;湘早45,X45）为试材,每种土壤添加7个Cd浓度,通过ISO11269-1根伸长测试方法,测量水稻根的相对伸长量,并结合Log-Logistic分布函数模型测定不同土壤中水稻Cd毒性的剂量-效应关系、毒性阈值（ECx, x=10, 50）及其预测模型。【结果】随着土壤Cd浓度的增加,不同土壤中水稻的相对根长（%）逐渐减小,基于根伸长的Cd对水稻毒性的10%抑制浓度的毒性阈值（EC10）和半抑制浓度（EC50）值在不同土壤和不同Cd敏感性水稻品种间有较大差异。总体而言,在3种不同Cd敏感性（T167＞L28＞X45）水稻品种中,同一土壤中Cd的水稻毒性ECx（x=10,50）随着水稻对Cd胁迫的敏感性增强而降低;就单一品种水稻而言,不同土壤的Cd水稻毒性阈值ECx间有显著差异。其中,以Cd敏感性水稻品种T167测试的不同土壤EC10变化为1.40-5.25 mg•kg-1,最大相差275.0%,EC50变化为17.83-46.93 mg•kg-1,最大相差163.2%;以Cd非敏感性水稻品种X45测试的不同土壤EC10变化为1.72-8.22 mg•kg-1,最大相差377.9%,EC50变化为26.96-68.16 mg•kg-1,最大相差152.8%。通过水稻Cd毒性阈值ECx与土壤性质间的多元回归分析表明,土壤pH、有机碳（OC）、阳离子交换量（CEC）与水稻Cd毒性阈值间呈正相关关系,基于土壤主要性质的水稻Cd毒性预测模型表明,EC50实测值均在预测值2倍误差（±S.D）范围内。【结论】基于ISO11269-1根伸长毒性测试结果表明,不同土壤中Cd的水稻毒性阈值间有显著差异,土壤pH、OC及CEC与水稻Cd的毒性阈值间呈显著正相关关系（P＜0.05）,基于上述土壤性质的预测模型可以很好预测不同土壤中Cd对水稻的毒性;不同Cd敏感性品种对测定土壤中水稻Cd毒性阈值有明显差异,因此,在制订土壤中Cd的生态基准时应充分考虑不同物种的敏感性差异特征。     

桃树部分经济性状的种内变异及其分级标准研究

为了弥补桃树品种间性状变异和分级研究的不足,本文在前人成果基础上,借助计算机。对桃树12个主要经济性状在品种和品种群间的变异及其分布性进行了研究。并根据概率和正态分布理论,探讨了适于正态分布性状的统一的概率分级标准。研究结果表明,桃树不同性状的离散程度存在很大差异,品种间性状变异以产量指数、果肉可滴定酸含量和单宁含量最大,变异系数高达45～60％;以果肉含糖量和可溶性固形物含量的变异最小,变异系数在20％以下。品种群间性状变异情况与品种间表现一致。经正态总体函数的X~2检验,在供试12年主要经济性状中,单果重、果肉含糖量、核重、成熟期、果实生育期、座果率和产量指数等7个性状的性状值是正态分布。对正态分布性状,可统一用(X-1.2818＄),(X-0.5246＄)(X+0.5246＄)和X=1.2818＄)4个分点将性状值由低到高分为5级,以(X-0.5246＄)和(X+0.5246＄)2个分点将性状值分为3级。如此分级后,5级分级中1～5级性状值出现的概率分别为10％,20％、40%、20％、10％,3级分中1～3级性状值出现的概率分别为30％、40％和30%。本文还列出了7个性状的3级和5级分级标准,并对概率分级和经验分级进行了比较。