中国6种地带性土壤红外光谱特性研究

利用土壤原样研究了中国 6种典型地带性土壤的红外光谱特征。结果表明 ,砖红壤、红壤红外光谱属于高岭石型图谱 ,显著的 36 95 ,36 2 0 ,10 35 cm- 1峰以及 35 2 7cm- 1峰可作为用红外光谱判断热带、南亚热带地带性土壤的特征峰。黄棕壤、褐土、黑垆土、黄绵土红外光谱为蒙脱石型图谱 ,较弱的 36 2 1cm- 1峰 ,3435和 10 2 8～10 32 cm- 1的强宽带 ,以及显著的 14 37cm- 1峰可作为温带半湿润 -半干旱地区石灰性土壤红外光谱的特征标志。黄棕壤是石灰性土壤向热带、南亚热带地区过渡的地带性土壤 ,其红外光谱标志为较宽的 3435 ,10 32 cm- 1吸收带和明显的 36 2 0 cm- 1吸收峰 ,以及较弱的 36 95 cm- 1峰 ,但没有 14 37cm- 1峰。中国从南到北 ,土壤红外光谱的36 96 ,36 2 1cm- 1 峰、石英双峰 (798,780 cm- 1 )的 797cm- 1 峰吸收强度逐渐减弱 ,而石英双峰的 780 cm- 1 峰吸收强度逐渐增强。     

Infrared observations of the jovian system from voyager 1

The infrared spectroscopy and radiometry investigation has obtained spectra of Jupiter and its satellites between approximately 180 and 2500 cm(-1) with a spectral resolution of 4.3 cm(-1). The Jupiter spectra show clear evidence of H(2), CH(4) C(2)H(2), C(2)H(6), CH(3)D, NH(3), PH(3), H(2)O, and GeH(4). A helium concentration of 0.11 +/- 0.03 by volume is obtained. Meridional temperature cross sections show considerable structure. At high latitudes, the stratosphere is warmer in the north than in the south. The upper troposphere and lower stratosphere are locally cold over the Great Red Spot. Amalthea is warmer than expected. Considerable thermal structure is observed on Io, including a relatively hot region in the vicinity of a volcanic feature.     

High-accuracy ab initio rotation-vibration transitions for water

The spectrum of water vapor is of fundamental importance for a variety of processes, including the absorption and retention of sunlight in Earth's atmosphere. Therefore, there has long been an urgent need for a robust and accurate predictive model for this spectrum. In our work on the high-resolution spectrum of water, we report first-principles calculations that approach experimental accuracy. To achieve this, we performed exceptionally large electronic structure calculations and considered a variety of effects, including quantum electrodynamics, which have routinely been neglected in studies of small many-electron molecules. The high accuracy of the resulting ab initio procedure is demonstrated for the main isotopomers of water.     

Resolving the structure of ionized helium in the intergalactic medium with the far ultraviolet spectroscopic explorer

The neutral hydrogen (H I) and ionized helium (He II) absorption in the spectra of quasars are unique probes of structure in the early universe. We present Far-Ultraviolet Spectroscopic Explorer observations of the line of sight to the quasar HE2347-4342 in the 1000 to 1187 angstrom band at a resolving power of 15,000. We resolve the He II Lyman alpha (Lyalpha) absorption as a discrete forest of absorption lines in the redshift range 2.3 to 2.7. About 50 percent of these features have H I counterparts with column densities N(H I) > 10(12.3) per square centimeter that account for most of the observed opacity in He II Lyalpha. The He II to H I column density ratio ranges from 1 to >1000, with an average of approximately 80. Ratios of <100 are consistent with photoionization of the absorbing gas by a hard ionizing spectrum resulting from the integrated light of quasars, but ratios of >100 in many locations indicate additional contributions from starburst galaxies or heavily filtered quasar radiation. The presence of He II Lyalpha absorbers with no H I counterparts indicates that structure is present even in low-density regions, consistent with theoretical predictions of structure formation through gravitational instability.     

Infrared Spectra of Hydronium Ion in Micaceous Minerals

X-ray diffraction measurements of the d((001)) spacing and the infrared absorption spectra of hydrogensaturated saturated micas show that an ion of approximately the same size and properties as hydronium is present and gives a unique absorption band at about 3470 cm(-1).     

FT-IR法鉴定中药海金沙正品及其掺伪品

[目的]利用傅里叶变换红外光谱法(FT-IR法)鉴别中药材海金沙的正品及其掺伪品。[方法]在合适的条件下(光谱范围:4000~400 cm~(-1);分辨率:4 cm~(-1);透过率:0~100%;扫谱次数:32次;速度:0.632 9 cm/s;检测器:DTGSKBr;Thermo scientific EZ OMNIC仪器系统操作软件;图谱修正:水和二氧化碳;背景光谱管理:采集样品前采集背景),利用FT-IR法测定海金沙样品及其掺伪品的红外吸收谱图,并做比较。[结果]各海金沙样品的红外光谱图基本一致,海金沙的黄土掺伪品和海金沙的蒲黄掺伪品的红外吸收图谱与海金沙的红外吸收图谱存在明显差别。该试验方法的精密度、重复性及稳定性考察合格。[结论]此方法简便、准确,可用于中药材海金沙正品及其掺伪品的鉴别。     

Pygmy stars: first pair

The binary LP 101-15/16 having the proper motion of 1.62 seconds of arc per year has been studied with the prime-focus spectrograph of the 200-inch (508 cm) telescope. Indications are that LP 101-15/16 is the first pair of pygmy stars ever discovered. One of its components, LP 101-16, is probably a blue pygmy star which is at least four magnitudes fainter than the ordinary white dwarfs. Also, two of the Balmer lines in absorption appear to be displaced toward the red by amounts which indicate the existence of an Einstein gravitational red shift corresponding to about 1000 km sec-1. On the other hand LP 101-15 is red and shows an entirely new type of spectrum, which suggests that it may be a first representative of a type of red pygmy star which is 2.5 magnitudes fainter than the M-type dwarf stars of the main sequence.     

CH5+: the infrared spectrum observed

Protonated methane, CH5+, has unusual vibrational and rotational behavior because its three nonequivalent equilibrium structures have nearly identical energies and its five protons scramble freely. Although many theoretical papers have been published on the quantum mechanics of the system, a better understanding requires spectral data. A complex, high-resolution infrared spectrum of CH5+ corresponding to the C-H stretching band in the 3.4-micrometer region is reported. Although no detailed assignment of the individual lines was made, comparison with other carbocation spectra strongly suggests that the transitions are due to CH5+.     

Quantum Yield for Production of CH3NC in the Photolysis of CH3NCS

The ultraviolet spectrum of methyl isothiocyanate (CH(3)NCS) and the quantum yield for its dissociation into methyl isocyanide (CH(3)NC) and atomic sulfur at 308 nanometers, Phi = 0.98 +/- 0.24, were measured. Methyl isothiocyanate is widely used as an agricultural fumigant and readily enters the atmosphere during and after application. The results indicate that photodissociation by sunlight is an effective pathway for its removal from the atmosphere.     

Infrared observations of the saturnian system from voyager 1

During the passage of Voyager 1 through the Saturn system, the infrared instrument acquired spectral and radiometric data on Saturn, the rings, and Titan and other satellites. Infrared spectra of Saturn indicate the presence of H(2), CH(4), NH(3), PH(3), C(2)H(2), C(2)H(6), and possibly C(3)H(4) and C(3)H(8). A hydrogen mole fraction of 0.94 is inferred with an uncertainty of a few percent, implying a depletion of helium in the atmosphere of Saturn relative to that of Jupiter. The atmospheric thermal structure of Saturn shows hemisphere asymmetries that are consistent with a response to the seasonally varying insolation. Extensive small-scale latitudinal structure is also observed. On Titan, positive identifications of infrared spectral features are made for CH(4), C(2)H(2), C(2)H(4), C(2)H(6), and HCN; tentative identifications are made for C(3)H(4) and C(3)H(8). The infrared continuum opacity on Titan appears to be quite small between 500 and 600 cm(-1), implying that the solid surface is a major contributor to the observed emission over this spectral range; between 500 and 200 cm(-1) theopacity increases with decreasing wave number, attaining an optical thickness in excess of 2 at 200 cm(-1). Temperatures near the 1-millibar level are independent of longitude and local time but show a decrease of approximately 20 K between the equator and north pole, which suggests a seasonally dependent cyclostrophic zonal flow in the stratosphere of approximately 100 meters per second. Measurements of the C ring of Saturn yield a temperature of 85 +/- 1 K and an infrared optical depth of 0.09 +/- 0.01. Radiometer observations of sunlight transmitted through the ring system indicate an optical depth of 10(-1.3 +/-0.3) for the Cassini division. A phase integral of 1.02 +/- 0.06 is inferred for Rhea, which agrees with values for other icy bodies in the solar system. Rhea eclipse observations indicate the presence of surface materials with both high and low thermal inertias, the former most likely a blocky component and the latter a frost.     

Understanding the infrared spectrum of bare CH5+

Protonated methane, CH5+, continues to elude definitive structural assignment, as large-amplitude vibrations and hydrogen scrambling challenge both theory and experiment. Here, the infrared spectrum of bare CH5+ is presented, as detected by reaction with carbon dioxide gas after resonant excitation by the free electron laser at the FELIX facility in the Netherlands. Comparison of the experimental spectrum at approximately 110 kelvin to finite-temperature infrared spectra, calculated by ab initio molecular dynamics, supports fluxionality of bare CH5+ under experimental conditions and provides a dynamical mechanism for exchange of hydrogens between CH3 tripod positions and the three-center bonded H2 moiety, which eventually leads to full hydrogen scrambling. The possibility of artificially freezing out scrambling and internal rotation in the simulations allowed assignment of the infrared spectrum despite this pronounced fluxionality.     

Quantum coherence in an optical modulator

Semiconductor quantum well electroabsorption modulators are widely used to modulate near-infrared (NIR) radiation at frequencies below 0.1 terahertz (THz). Here, the NIR absorption of undoped quantum wells was modulated by strong electric fields with frequencies between 1.5 and 3.9 THz. The THz field coupled two excited states (excitons) of the quantum wells, as manifested by a new THz frequency- and power-dependent NIR absorption line. Nonperturbative theory and experiment indicate that the THz field generated a coherent quantum superposition of an absorbing and a nonabsorbing exciton. This quantum coherence may yield new applications for quantum well modulators in optical communications.     

Absorption features in the x-ray spectrum of an ordinary radio pulsar

The vast majority of known nonaccreting neutron stars (NSs) are rotation-powered radio and/or γ-ray pulsars. So far, their multiwavelength spectra have all been described satisfactorily by thermal and nonthermal continuum models, with no spectral lines. Spectral features have, however, been found in a handful of exotic NSs and were thought to be a manifestation of their unique traits. Here, we report the detection of absorption features in the x-ray spectrum of an ordinary rotation-powered radio pulsar, J1740+1000. Our findings bridge the gap between the spectra of pulsars and other, more exotic, NSs, suggesting that the features are more common in the NS spectra than they have been thought so far.     

三江平原沼泽湿地不同水层下CH4、N2O的排放及影响因子

采用野外静态箱—气相色谱法,对三江平原沼泽湿地6—9月不同水层下CH4、N2O的排放进行了同步对比研究,并探讨了影响气体排放的主要影响因子。结果表明,不同水层下的CH4和N2O排放具有明显的时空变化特征。CH4排放高峰期在7、8月,N2O主要排放期在6、7月。40 cm水层下的CH4排放强度最高,平均为34.54mg.m-2.h-1;20、60 cm水层下的CH4排放强度居中,平均分别为17.18、13.02 mg.m-2.h-1;0 cm水层下的CH4排放强度最低,平均7.69 mg.m-2.h-1,N2O排放强度最高,为0.072 mg.m-2.h-1;20、40 cm水层下的N2O排放强度相似,平均分别为0.053、0.050 mg.m-2.h-1;60 cm水层下的排放强度最小,平均为0.026 mg.m-2.h-1。相关分析表明,CH4的排放通量与40 cm水深及5 cm地温呈显著或极显著正相关,与其它各土壤温度之间的相关性因水层不同有所差异;N2O排放通量与地表0、40 cm水深呈显著负相关,20 cm水层下的N2O排放通量与5 cm地温呈显著正相关。CH4、N2O的排放通量与大气温度及地表温度均不相关。     

夏玉米不同土层根系对花后植株生长及产量形成的影响

【目的】探明夏玉米不同土层根系对花后植株生长及产量形成的调控作用,为生产中塑造高产高效根群结构,提高籽粒产量提供理论依据。【方法】以高产夏玉米品种郑单958和登海661为材料,采用土柱栽培方式,设置3个处理（不断根处理：CK,地下40 cm处断根：T-40,地下80 cm处断根：T-80）,于开花期进行断根,研究不同土层根系对地上部生长及产量形成的调控作用。【结果】0—40 cm土层根系对花后氮素积累和转运量影响最大,切断40 cm以下土层根系后植株吸收氮素能力显著降低,植株营养器官氮素向籽粒库的转运量增加。花后40 cm以下土层根系对叶片保绿性和光合性能影响显著,切断深层根系后玉米单株叶面积、叶绿素含量、净光合速率(Pn)和SOD活性显著降低,MDA含量升高,光合高值持续期缩短,单株生物量和籽粒产量显著下降;0—40 cm根系对产量影响最大,40—80 cm根系对穗粒数和千粒重有显著影响,80 cm以下土层根系对千粒重影响较为显著。【结论】高产栽培中促进根系下扎,保持深层根系活力可以防止玉米早衰,提高叶片光合能力和对氮素的吸收能力,有助于提高玉米单产。     

Raman Studies of Alkali-Metal Doped AxC60 Films (A = Na, K, Rb, and Cs; x = 0, 3, and 6)

The room temperature Raman spectra of the intramolecular modes between 100 cm(-1) and 2000 cm(-1) are reported for alkali-metal doped AxC(60) films. For A = K, Rb, and Cs, phase separation is observed with the spectra of C(60), K(3)C(60), K(6)C(60), Rb(3)C(60), Rb(6)C(60), and Cs(6)C(60) phases reported. The x = 3 phases show only three Raman active modes: two of Ag symmetry and only the lowest frequency Hg mode. The other Hg modes regain intensity in the x = 6 films, with several mode splittings observed. For A = Na, such phase separation is not clearly observed, and reduced mode shifts are interpreted as due to incomplete charge transfer in these films.     

Infrared observations of the neptunian system

The infrared interferometer spectrometer on Voyager 2 obtained thermal emission spectra of Neptune with a spectral resolution of 4.3 cm(-1). Measurements of reflected solar radiation were also obtained with a broadband radiometer sensitive in the visible and near infrared. Analysis of the strong C(2)H(2) emission feature at 729 cm(-1) suggests an acetylene mole fraction in the range between 9 x 10(-8) and 9 x 10(-7). Vertical temperature profiles were derived between 30 and 1000 millibars at 70 degrees and 42 degrees S and 30 degrees N. Temperature maps of the planet between 80 degrees S and 30 degrees N were obtained for two atmospheric layers, one in the lower stratosphere between 30 and 120 millibars and the other in the troposphere between 300 and 1000 millibars. Zonal mean temperatures obtained from these maps and from latitude scans indicate a relatively warm pole and equator with cooler mid-latitudes. This is qualitatively similar to the behavior found on Uranus even though the obliquities and internal heat fluxes of the two planets are markedly different. Comparison of winds derived from images with the vertical wind shear calculated from the temperature field indicates a general decay of wind speed with height, a phenomenon also observed on the other three giant planets. Strong, wavelike longitudinal thermal structure is found, some of which appears to be associated with the Great Dark Spot. An intense, localizd cold region is seen in the lower stratosphere, which does not appear to be correlated with any visible feature. A preliminary estimate of the effective temperature of the planet yields a value of 59.3 +/- 1.0 kelvins. Measurements of Triton provide an estimate of the daytime surface temperature of 38(+3)(-4) kelvins.     

Absorption of sunlight in the atmosphere of venus

In this report the fluxes measured by the solar flux radiometer (LSFR) of the Pioneer Venus large probe are compared with calculations for model atmospheres. If the large particles of the middle and lower clouds are assumed to be sulfur, strong, short-wavelength absorption results in a net flux profile significantly different from the LSFR net flux measurements. Models in which the smallest particles are assumed to be sulfur gave flux profiles consistent with the measurements if an additional source of absorption is included in the upper cloud. The narrowband data from 0.590 to 0.665 micrometer indicate an absorption optical depth of about 0.05 below the cloud bottom. The broadband data imply that either this absorption extends over a considerable wavelength interval (as might be the case for dust) or that a very strong absorption band lies on one side of the narrowband filter (as suggested by early Venera 11 and Venera 12 reports). Thermal balance calculations based on the measured visible fluxes indicate high surface temperature for reasonable assumptions of cloud opacity and water vapor abundance. The lapse rate becomes convective within the middle cloud. For water mixing ratios of 2.0 x 10(-4) below the clouds we find a subadiabatic region extending from the cloud bottom to altitudes near 35 kilometers.     

木材远红外光谱特性

根据福建22种主要用材树种远红外吸收光谱分析,木材分子结构径向与弦向基本相同,不同树种之间也无明显差别。从木材远红外吸收光谱得到木材远红外吸收峰在波数为3400cm~(-1)、740cm~(-1)、600cm~(-1)处,在800～1500cm~(-1)处有连续吸收峰,在波数为1840cm~(-1)附近有一个透射峰。提高木材远红外干燥的效率和质量的一个重要因素是增加远红外对木材的透射深度,以增加形成“正热源”的可能性。因此本研究为木材远红外干燥提供了重要的基准和依据。