大气CO_2浓度升高与氮肥管理对麦田土壤有效氮的影响

为了探讨全球气候变化对农田土壤氮素动态的影响,采用中国稻麦轮作系统FACE(Free-Air CO2 Enrichment)平台,开展了大气CO2浓度升高和氮肥管理对麦田土壤有效氮含量影响的研究.结果表明:在低N和常规N处理下,大气CO2浓度升高使拔节期土壤C/N分别增加了5.6%和10.2%,土壤pH分别降低了 2.4%和6.4%(p＜O.05).在小麦生育期内.低N和常规N条件下.大气CO2浓度升高降低了土壤总有效氮和NO3--N含量,相对于低N处理.常规N处理下降的趋势更为明显.在低N条件下,大气CO2浓度使拔节期和成熟期土壤中NH4+-N含量分别增加了7.4%和9.9%,而常规N处理中则表现出相反的趋势.本研究显示,大气CO2浓度升高降低了土壤有效氮含量,而施用氮肥增加了土壤有效氰含量.     

土壤含水量对硝化和反硝化过程N_2O排放及同位素特征值的影响

【目的】通过室内培养试验,研究不同含水量对北京顺义潮褐土N_2O排放及同位素特征值(δ15Nbulk,δ18O和nitrogen isotopomer site preference of N_2O,简称SP)的影响,以期获得不同水分条件下土壤N_2O产生途径及变化规律,为农田土壤N_2O减排提供理论依据。【方法】结合稳定同位素技术与乙炔抑制法,以北京顺义潮褐土为试材,设置3个含水量梯度:67%、80%和95%WFPS(土壤体积含水量与总孔隙度的百分比或实际重量含水量与饱和含水量的百分比,简称WFPS),在此基础上设置无C2H2,0.1%(V/V)C2H2和10%(V/V)C2H2处理。将土壤装入培养瓶中培养2 h,之后收集培养瓶中的气体测定N_2O浓度及同位素特征值,并采集土样测定其NH+4-N和NO-3-N的含量。利用同位素二源混合模型计算硝化和反硝化作用对土壤N_2O排放的贡献率,对N_2O产生途径进行量化分析。【结果】根据室内土壤培养测定结果,高(95%WFPS)、中(80%WFPS)和低(67%WFPS)含水量土壤N_2O加权平均排放通量分别为1.17、0.27和0.08 mg N·kg-1·d-1,高含水量土壤N_2O排放量均显著高于中、低含水量处理,中含水量处理显著高于低含水量;整个培养周期,高、中和低含水量土壤N_2O+N_2累积排放量分别为培养初期总的无机氮含量的18.05%、5.27%和1.24%(N_2O+N_2累积排放量分别为19.61、5.72和1.35 mg N·kg-1;各处理NH+4-N+NO-3-N初始含量均为108.62 mg N·kg-1);与低含水量处理相比,高、中含水量土壤的N_2O+N_2累积排放量分别增加了13.53倍和3.24倍,高含水量土壤N_2O+N_2累积排放量比中含水量高2.43倍,表现为随着含水量的增加,土壤无机氮(NH+4-N+NO-3-N)以气态氮(N_2O+N_2)形式的损失量逐渐增加。3个含水量处理N_2O的δ15Nbulk加权平均值变化范围为-42.93‰—-4.07‰,且较高含水量处理显著低于较低含水量处理;10%(V/V)C2H2抑制土壤中N_2O还原成N_2的过程,各含水量土壤中,10%(V/V)C2H2处理组其N_2O的δ18O值显著低于0.1%(V/V)C2H2处理组,且N_2O/(N_2O+N_2)比率随土壤含水量增加而降低;各处理土壤中同时存在多个N_2O产生过程,对于培养第一周,土壤产生的N_2O的SP值于培养前4 d呈逐渐增加的趋势,之后又逐渐降低,低含水量土壤在第1—2天产生的N_2O的SP值为6.74‰—12.04‰,反硝化作用对土壤N_2O排放的贡献率为56.36%—66.15%,此培养阶段表现为土壤主要通过反硝化作用产生N_2O,之后,硝化作用贡献率(55.78%—100%)增强;中含水量土壤N_2O的SP加权平均值为10.26‰,该土壤中反硝化作用(40.90%—74.04%)占据主导地位;加10%(V/V)C2H2的高含水量处理,在整个培养第一周均具有较高的SP值,变化范围为7.61‰—21.11‰;与0.1%(V/V)C2H2处理组相比,10%(V/V)C2H2处理的高、中和低含水量土壤排放N_2O的SP加权平均值分别降低了0.10倍、0.33倍和0.06倍。【结论】土壤含水量增加促进N_2O排放,高含水量处理中N_2O排放量最高。67%WFPS处理中,N_2O排放前期以反硝化作用为主,后期以硝化作用为主;80%WFPS处理中,N_2O主要由反硝化过程产生;95%WFPS处理中,N_2O排放以硝化作用为主。     

冬小麦旺盛生长期CO_2浓度升高对土壤呼吸的影响

土壤呼吸是全球碳循环的一个重要组成部分、土壤碳库的主要输出途径和大气CO2重要的源。利用FACE（free-air CO2 enrichment）技术平台，采用LI6400红外气体分析仪（IRGA）-田间原位测定的方法，研究了大气CO2浓度升高和不同氮肥水平对水稻/小麦轮作制中冬小麦生长期间土壤呼吸的影响。结果表明，在整个测定期间，CO2浓度升高均增强了土壤呼吸的排放速率和释放量，增幅随着氮肥施用量的增加而增大，土壤呼吸在孕穗-抽穗期达到最大值。土壤呼吸同土壤温度呈极显著的指数相关;随施氮量从112.5kg·hm^-2增加到2255kg·hm^-2，FACE处理的Q10值从2.98增大为3.26，但比相应的Ambient（对照浓度）处理的Q10值下降了6.3%和18.3%，显然CO2浓度升高降低了土壤呼吸对温度增加的敏感性。总之，大气CO2浓度升高将加快土壤向大气的CO2排放，将有助于评价未来高CO2浓度环境对农田生态系统土壤碳循环的影响。     

水稻秸秆还田对稻田土壤N_2O排放的影响

以湖北省两种典型水稻土壤[咸宁水旱轮作土壤(简称XR)与潜江冬泡土壤(简称QF)]为研究对象,室内培养模拟水稻秸秆还田对土壤N_2O排放的影响。设置了淹水(土水比为1∶1)和土壤充水孔隙度为80%(简称80%WFPS)2种水分条件以及添加1%水稻秸秆(简称S)、1%水稻秸秆+50 mg(N)/kg尿素(简称S+U)和空白对照(CK)3种处理,25℃恒温培养60 d。结果表明,XR土样中,淹水条件下CK、S以及S+U处理后N_2O累积排放通量分别为1.80、0.15和0.42 mg(N)/kg,而80%WFPS条件下相同处理后的N_2O累积排放通量分别为0.065、0.040和0.160 mg(N)/kg;QF土样中,淹水条件下CK、S以及S+U处理后N_2O累积排放通量分别为3.42、0.09和0.22 mg(N)/kg,而80%WFPS条件下相同处理的N_2O累积排放通量分别为4.58、1.55和5.28 mg(N)/kg。土壤轮作模式、水分和秸秆添加方式均导致了不同土壤间N_2O排放的差异,但主要受土壤氧化还原电位(Eh)的影响,其排放通量与Eh呈显著负相关。这表明土壤Eh可能是调节土壤N循环过程的关键因子。     

改性尿素对土壤N2O排放的影响

通过室内培养试验,研究5种改性尿素对土壤N2O排放的效果,结果表明:当旱田土壤含水量较低(23%)时,NI(尿素 硝化抑制剂)处理的土壤NO排放效果最好,其次为FL(尿素 1.0?D 0.3%HQ)。当旱田土壤含水量较高(34%)时,FL处理的土壤N2O排放效果最好,其次为处理NI;当稻田土壤处于淹水状态时,Meister(包被尿素)处理的土壤N2O排放效果最好,其次为处理FL。该试验结果对于选取优良改性尿素进行田间试验、进一步探讨改良尿素对土壤N2O的排放效果具有指导意义。     

氧气对水稻土N2O排放和narG型反硝化微生物的短期影响

选取第四纪红土发育水稻土,在0%(厌氧)、10%(兼性厌氧)和21%(好氧)等3个O2体积分数及40%和60% 2种土壤含水量条件下进行室内培养,探讨O2含量对土壤N2O排放及narG型反硝化微生物种群丰度和群落组成的影响。结果表明：40%和60% 2种土壤含水量条件下,厌氧处理的N2O排放通量均最高,且60%土壤含水量处理下的N2O排放通量略高于40%土壤含水量处理的;方差分析表明,相比于土壤含水量,O2含量是制约土壤中N2O排放更关键的因子;微生物narG基因丰度与O2含量呈极显著(P<0.01)负相关,与N2O排放通量和土壤NO3––N消耗质量分数呈极显著(P<0.01)正相关,与土壤含水量呈正相关,但不显著;O2含量和含水量均会造成土壤narG型反硝化微生物群落组成差异,40%土壤含水量处理,OTU1882(Pseudolabrys)、OTU1510(分枝杆菌属)的占比较大,60%土壤含水量处理,OTU1593(地杆菌属)的占比较大,当土壤含水量一定时,同一培养时间厌氧处理的优势OTU1882和OTU1510相对丰度偏低,且变化幅度较大,其相对丰度与N2O排放通量呈负相关,其中OTU1882的影响显著(P<0.05)。可见,土壤O2含量通过调控土壤微生物的narG基因丰度和群落组成而调控N2O的排放。     

大气CO_2浓度升高对稻季耕层土壤溶液中Ca、Mg浓度的影响

【目的】研究稻田生态系统中土壤钙、镁元素生物地球化学循环对长期大气CO2浓度升高的响应。【方法】利用中国稻田FACE(free air carbon-dioxide enrichment)试验平台,包括Ambient(对照,自由大气CO2浓度约为370μmol·mol-1)和FACE(比对照大气CO2浓度高200μmol·mol-1)2个试验处理,在2004、2005和2007年稻季不同生育期原位采集5cm和15cm处土壤溶液并测定其中Ca、Mg浓度。【结果】在2004、2005和2007年,FACE处理5cm处土壤溶液Ca浓度分别是对照处理的125%、106%和72%,Mg浓度分别是对照处理的115%、104%和75%;FACE处理15cm处与5cm处土壤溶液Ca浓度的比值在2004、2005和2007年分别是对照处理的71%、114%和180%,Mg的比值分别是对照的74%、104%和159%;2007年FACE处理0-15cm耕层土壤溶液Ca、Mg浓度分别比对照处理低6.8%和4.6%。【结论】连续大气CO2浓度升高可改变土壤溶液中Ca、Mg元素在不同深度耕层的分布,提高15cm处与5cm处土壤溶液Ca、Mg浓度的比值,且这种影响存在一定的累积效应。稻田生态系统Ca、Mg循环对长期大气CO2浓度升高的响应值得深入研究。     

模拟N/S沉降对米槠天然林土壤N净转化速率和N_2O排放的影响

[目的]研究N/S沉降对中亚热带米槠天然林土壤硝化作用和N2O排放的影响。[方法]室内用NH4NO3/K2SO4模拟N/S沉降,在30℃和60%WHC水分条件下,恒温培养15 d。在培养的第1、5、10和15天测定土壤NH+4-N、NO-3-N和pH,在培养的第3、4、5和10天采集气体样品测定N2O浓度。[结果]N沉降和NS复合沉降在0.05水平显著促进土壤的矿化和硝化,且促进效果随沉降强度或NS复合沉降中N的比例增大而增大,但S沉降的促进作用不显著;土壤净矿化速率和净硝化速率与土壤pH具有极显著的负相关性。土壤在自然状态和N/S沉降的影响下,有机氮净矿化速率与净硝化速率之间均存在显著相关性,且矿化速率大于硝化速率。N沉降和NS复合沉降显著提高土壤的硝化率在N/S沉降下,该区土壤中的无机氮仍以NH+4-N为主,硝化作用弱,铵态氮的供给不成为土壤硝化作用的限制因素。NS复合沉降促进土壤N2O的排放,具体机理有待进一步揭示。[结论]N沉降和NS复合沉降明显促进土壤的矿化和硝化作用,S沉降对土壤的矿化和硝化作用的影响不大;NS复合沉降影响土壤的N2O排放,且其影响效应与沉降中N、S的比例相关,在有关酸沉降对土壤N2O排放的影响方面,S沉降应受到关注。     

FACE环境下不同秸秆与氮肥管理对稻田土壤产甲烷菌的影响

产甲烷菌是土壤中与甲烷产生和碳素循环有关的微生物菌群,大气CO2浓度升高可能对它们的数量产生影响。利用江都市小记镇的稻-麦轮作FACE平台,采用最大可能(MPN)法,在2004年水稻生长季研究了不同施肥情况(施常规氮量和低氮量)、不同秸秆还田情况(秸秆全还田、秸秆半还田、秸秆不还田)下,土壤中的产甲烷菌数量在大气CO2浓度升高条件下随时间的变化情况。结果表明,大气CO2浓度升高在秸秆全还田情况下对产甲烷菌数有明显的促进作用,在其他2种秸秆还田情况下,FACE与对照差异不显著。常氮处理仅在水稻生长初期促进产甲烷菌数,而在其他生长季不同氮肥处理之间无明显差异。总之,常氮处理产甲烷菌数量FACE比对照平均高104%～116%,低氮处理平均高101%～126%,进一步证实大气CO2浓度升高会促进稻田CH4的排放。     

大气CO2浓度升高和施氮对麦季土壤有效态微量元素含量的影响

利用中国的稻/麦轮作FACE(Free Air Carbon-dioxide Enrichment)平台技术,研究大气CO2浓度升高(比周围大气高200μmol·mol-1)和不同施N水平(常氮,250kg N·hm-2;低氮,150kg N·hm-2)对麦田土壤微量元素有效性的影响.结果表明,CO2:浓度升高在一定程度上增加了土壤有效态微量元素含量,其中对DTPA-Cu和Zn的增加趋势尤为明显;常规施氮水平下土壤有效态微量元素含量高于低氮水平.对CO2浓度升高增加了土壤微量元素有效性的原因做了初步分析,并指出大气CO2浓度增加可能会影响到农业生态系统中土壤微量元素的地球化学循环.     

Early meteorological results from the viking 2 lander

Early results from the meteorological instruments on the Viking 2 lander are presented. As on lander 1, the daily patterns of temperature, wind, and pressure have been highly repetitive during the early summer period. The average daily maximum temperature was 241 degrees K and the diurnal minimum was 191 degrees K. The wind has a vector mean of 0.7 meter per second from the southeast with a diurnal amplitude of 3 meters per second. Pressure exhibits both diurnal and semidiurnal oscillations, although of substantially smaller amplitude than those of lander 1. Departures from the repetitive diurnal patterns begin to appear on sol 37.     

Infrared observations of the saturnian system from voyager 2

During the passage of Voyager 2 through the Saturn system, infrared spectral and radiometric data were obtained for Saturn, Titan, Enceladus, Tethys, Iapetus, and the rings. Combined Voyager 1 and Voyager 2 observations of temperatures in the upper troposphere of Saturn indicate a seasonal asymmetry between the northern and southern hemispheres, with superposed small-scale meridional gradients. Comparison of high spatial resolution data from the two hemispheres poleward of 60 degrees latitude suggests an approximate symmetry in the small-scale structure, consistent with the extension of a symmetric system of zonal jets into the polar regions. Longitudinal variations of 1 to 2 K are observed. Disk- averaged infrared spectra of Titan show little change over the 9-month interval between Voyager encounters. By combining Voyager 2 temperature measurements with ground-based geometric albedo determinations, phase integrals of 0.91 +/- 0.13 and 0.89 +/- 0.09 were derived for Tethys and Enceladus, respectively. The subsolar point temperature of dark material on Iapetus must exceed 110 K. Temperatures (and infrared optical depths) for the A and C rings and for the Cassini division are 69 +/- 1 K (0.40 +/- 0.05), 85 +/- 1 K (0.10 +/- 0.03), and 85 +/- 2 K (0.07 +/- 0.04), respectively.     

Infrared observations of the jovian system from voyager 2

Infrared spectra obtainedfrom Voyager 2 have provided additional data on the Jovian system, complementing those obtained from Voyager 1. The abundance ratio of ethane to acetylene in Jupiter's atmosphere appears to be about three times larger in the polar regions than at lower latitudes. A decidedly hemispherical asymmetry exists, with somewhat higher ratios prevailing in northern latitudes. An overall increase in the abundance ratio by a factor of about 1.7 appears to have occurred between the Voyager 1 and 2 encounters. Global brightness temperature maps of Jupiter at 226 and 602 cm(-1) exhibit a large amount of local- and planetary-scale structure, as well as temporal variability. Although heterogeneous cloud structure and ammonia concentration in the lower troposphere may contribute to the appearance of the 226-cm(-1) map, the detail in the 602-cm(-1) maps probably represents the actual horizontal thermal structure near the tropopause and suggests that dynamical heating and cooling processes are important. Low-latitude surface temperatures on the Galilean satellites rangefrom approximately 80 K on the dark sides to 155 K at the subsolar point on Callisto. Below a thin insulating layer, the thermal inertia of Callisto is somewhat greater than that of Earth's moon. Upper limits on the infrared optical depth of the Jovian ring rangingfrom approximately 3 x 10(-4) at 250 cm(-1) to 3 x 10(-3) at 600 cm(-1) have been found.     

Extreme ultraviolet observations from the voyager 2 encounter with saturn

Combined analysis of helium (584 angstroms) airglow and the atmospheric occultations of the star delta Scorpii imply a vertical mixing parameter in Saturn's upper atmosphere of K (eddy diffusion coefficient) approximately 8 x 10(7) square centimeters per second, an order of magnitude more vigorous than mixing in Jupiter's upper atmosphere. Atmospheric H(2) band absorption of starlight yields a preliminary temperature of 400 K in the exosphere and a temperature near the homopause of approximately 200 K. The energy source for the mid-latitude H(2) band emission still remains a puzzle. Certain auroral emissions can be fully explained in terms of electron impact on H(2), and auroral morphology suggests a link between the aurora and the Saturn kilometric radiation. Absolute optical depths have been determined for the entire C ring andparts of the A and B rings. A new eccentric ringlet has been detected in the C ring. The extreme ultraviolet reflectance of the rings is fairly uniform at 3.5 to 5 percent. Collisions may control the distribution of H in Titan's H torus, which has a total vertical extent of approximately 14 Saturn radii normal to the orbit plane.     

The surface of Mars: the view from the viking 2 lander

Viking 2 lander began imaging the surface of Mars at Utopia Planitia on 3 September 1976. The surface is a boulder-strewn reddish desert cut by troughs that probably form a polygonal network. A plateau can be seen to the east of the spacecraft, which for the most probable lander location is approximately the direction of a tongue of ejecta from the crater Mie. Boulders at the lander 2 site are generally more vesicular than those near lander i. Fines at both lander sites appear to be very fine-grained and to be bound in a duricrust. The pinkish color of the sky, similar to that observed at the lander I site, indicates suspension of surface material. However, the atmospheric optical depth is less than that at the lander I site. After dissipation of a cloud of dust stirred during landing, no changes other than those stemming from sampling activities have been detected in the landscape. No signs of large organisms are apparent at either landing site.     

蔬菜根际细菌R2–2的鉴定及其抑菌活性

从云南昆明市郊蔬菜根际分离细菌,经平板对峙培养筛选出1株抑菌能力较强的菌株R2-2,通过对其进行形态观察、Biolog微生物自动鉴定系鉴定和16S rDNA序列测定及其系统发育学分析,鉴定为甲基营养型芽孢杆菌(Bacillus methylotrophicus)。对R2-2与植物病原细菌(甘蓝黑腐病菌、魔芋细菌性软腐病菌、海棠斑点病菌、水稻白叶枯病菌、水稻细菌性条斑病菌)和病原真菌(疫霉菌、尖镰孢菌、茄镰孢菌、立枯丝核菌)进行对峙试验,结果显示,R2-2对水稻白叶枯病菌和水稻条斑病菌有较强的抑菌效果,抑菌圈直径分别达6.83 cm和7.03 cm。该菌株的16S rDNA序列已在GenBank中注册,登录号为JN648098。     

超临界CO_2萃取昆虫水虻油脂的实验研究

应用超临界流体技术萃取昆虫水虻油脂成分．采用二因素三水平正交试验方案,考察温度、压力等参数对油脂萃取量的影响．结果表明,萃取压力２５ＭＰａ、温度４０℃、时间３ｈ及体积流量（２６±３）Ｌｈ－１为本试验最佳参数组合,油脂萃取量最多．影响油脂萃取量的主要因素是压力．     

Photometry from voyager 2: initial results from the uranian atmosphere, satellites, and rings

The Voyager 2 photopolarimeter successfully completed the Uranus encounter, acquiring new data on the planet's atmosphere, its principal satellites, and its ring system. Spatially resolved photometry of the atmosphere at 0.27 micrometer shows no enhancement in absorption toward the pole, unlike the case for Jupiter and Saturn. Stellar occultation measurements indicate the temperature at the 1-millibar level over the north pole is near 90 kelvins. The geometric albedos of the five large satellites of Uranus were measured at 0.27 and 0.75 micrometer and indicate the presence of low albedo, spetrally flat absorbing material. Titania seems to have a fluffy surface, as indicated by its phase curve. The nine ground-based rings were detected, and their internal structure, optical depths, and positions were determined. The sharp edges of the in ring made it possible to measure its edge thickness (less than 150 meters) and particle sizes (less than 30 meters); little or no dust was detcted. New narrow rings and partial rings (arcs) were measured, and the narrow component of the eta ring was found to be discontinuous.     

Photometry from voyager 2: initial results from the neptunian atmosphere, satellites, and rings

The Voyager photopolarimeter successfully accomplished its objectives for the Neptune encounter, performing measurements on the planet, several of its satellites, and its ring system. A photometric map of Neptune at 0.26 micrometer (microm) shows the planet to be bland, with no obvious contrast features. No polar haze was observed. At 0.75 microm, contrast features are observed, with the Great Dark Spot appearing as a low-albedo region and the bright companion as being substantially brighter than its surroundings, implying it to be at a higher altitude than the Great Dark Spot. Triton's linear phase coefficients of 0.011 magnitudes per degree at 0.26 microm and 0.013 magnitudes per degree at 0.75 microm are consistent with a solid-surface object possessing high reflectivity. Preliminary geometric albedos for Triton, Nereid, and 1989N2 were obtained at 0.26 and 0.75 microm. Triton's rotational phase curve shows evidence of two major compositional units on its surface. A single stellar occultation of the Neptune ring system elucidated an internal structure in 1989N1R, in the approximately 50-kilometer region of modest optical depth. 1989N2R may have been detected. The deficiency of material in the Neptune ring system, when compared to Uranus', may imply the lack of a "recent" moon-shattering event.     

利用Na_2S_2O_3溶液萃取和回收污染土壤中的重金属

通过对比试验研究了Na2S2O3萃取液中重金属的分离效果并将其应用于修复土壤污染。结果表明,Na2S2O3溶液能有效地萃取土壤中重金属,Na2S能沉淀分离Na2S2O3溶液中的Cu、Hg,其效率均达99%以上。连续萃取能提高污染土壤中重金属的去除率,回收的Na2S2O3连续使用6次,损失约6%,土壤中Cu和Hg累积去除率分别达64.6%、75.1%。得到的硫化物沉淀含有很高的重金属,能很方便地处理或回收。