The magnetic field of saturn: pioneer 11 observations

The intrinsic magnetic field of Saturn measured by the high-field fluxgate magnetometer is much weaker than expected. An analysis of preliminary data combined with the preliminary trajectory yield a model for the main planetary field which is a simple centered dipole of moment 0.20 +/- 0.01 gauss-Rs(3) = 4.3 +/- 0.2 x 10(28) gauss-cm(3) (1 Rs = 1 Saturn radius = 60,000 km). The polarity is opposite that of Earth, and, surprisingly, the tilt is small, within 2 degrees +/- 1 degrees of the rotation axis. The equatorial field intensity at the cloud tops is 0.2 gauss, and the polar intensity is 0.56 gauss. The unique moon Titan is expected to be located within the magnetosheath of Saturn or the interplanetary medium about 50 percent of the time because the average subsolar point distance to the magnetosphere is estimated to be 20 Rs, the orbital distance to Titan.     

Magnetic field of jupiter and its interaction with the solar wind

Jupiter's magnetic field and its interaction with the magnetized solar wind were observed with the Pioneer 10 vector helium magnetometer. The magnetic dipole is directed opposite to that of the earth with a moment of 4.0 gauss R(J)(3) (R(J), Jupiter radius), and an inclination of 15 degrees lying in a system III meridian of 230 degrees . The dipole is offset about 0.1 R(J) north of the equatorial plane and about 0.2 R(J) toward longitude 170 degrees . There is severe stretching of the planetary field parallel to the equator throughout the outer magnetosphere, accompanied by a systematic departure from meridian planes. The field configuration implies substantial plasma effects inside the magnetosphere, such as thermal pressure, centrifugal forces, and differential rotation. As at the earth, the outer boundary is thin, nor diffuse, and there is a detached bow shock.     

Saturn's Magnetic Field and Magnetosphere

The Pioneer Saturn vector helium magnetometer has detected a bow shock and magnetopause at Saturn and has provided an accurate characterization of the planetary field. The equatorial surface field is 0.20 gauss, a factor of 3 to 5 times smaller than anticipated on the basis of attempted scalings from Earth and Jupiter. The tilt angle between the magnetic dipole axis and Saturn's rotation axis is < 1 degrees , a surprisingly small value. Spherical harmonic analysis of the measurements shows that the ratio of quadrupole to dipole moments is < 10 percent, indicating that the field is more uniform than those of the Earth or Jupiter and consistent with Saturn having a relatively small core. The field in the outer magnetosphere shows systematic departures from the dipole field, principally a compression of the field near noon and an equatorial orientation associated with a current sheet near dawn. A hydromagnetic wake resulting from the interaction of Titan with the rotating magnetosphere appears to have been observed.     

不同覆膜栽培方式对旱地土壤水热效应及西瓜产量的影响

【目的】西瓜是黄土高原旱地的主要经济作物之一,近年来种植面积逐年扩大。但该区域降水总量不足且时空分布不均,西瓜生产中常遭受前期干旱和后期涝害而导致减产。本研究针对黄土高原旱作区水资源缺乏的现状,采用垄沟种植,改变栽培方式和覆膜方式,探索适宜西瓜生长的集雨高产栽培模式,实现有效汇集天然降水,以改善土壤水热效应,提高西瓜产量。【方法】2011-2013在甘肃省庆阳市宁县太昌乡开展试验,研究不同覆膜栽培方式对旱地土壤水分、土壤温度和西瓜产量的影响。试验设全覆膜垄上播种（RM）、全覆膜垄上沟播（GM）、全覆膜沟播（TG）、半覆膜垄上沟播（GH）和半覆膜垄上播种（RH）5个处理,采用随机区组排列,以RH为对照,3次重复。起垄后垄宽100 cm,沟宽30 cm。垄上沟播处理中,集水沟宽20 cm,深10 cm。采用Stow Away Tidbit Temp Logger测定5、10和15 cm土层土壤温度,烘干法测定0-100 cm土层土壤含水量。种植密度为7 692株/hm²。【结果】土壤含水量的变化受集雨作用和西瓜生长影响。在幼苗期,TG、GM和GH处理0-10 cm土壤含水量分别较RH提高41.41%、37.82和32.69%。伸蔓期TG、RM和GH处理0-40 cm土层土壤含水量分别较RH提高13.91%、10.61%和6.75%,结果期GM和GH处理0-40 cm土壤含水量分别较RH提高8.50%和5.49%。成熟期GM、GH、TG和RM处理0-40 cm土壤含水量分别较RH提高10.51%、10.33%、4.98%和3.66%,土壤储水量由高到低依次为GH＞GM＞TG＞RM＞RH。不同处理的温度日变化呈“S”型负正弦曲线,随土壤深度的增加,曲线的振幅减小,相位后移,周期增长。日均温度从大到小依次为RM＞RH＞GM＞TG＞GH。土层每加深5 cm,各处理温度日变化曲线相位依次推移1 h。垄上温度均高于垄沟,垄上土壤温度以处理RM最高。不同栽培方式的保温效果从大到小依次为GM＞TG＞GH＞RH＞RM。GM处理连续两年产量最高,平均较RH提高10.34%,GH处理3年平均产量较RH提高7.66%,增产幅度依次为GM＞GH＞RM＞TG。GM和GH能够有效富集降雨,增产作用显著。【结论】3年的试验验证了不同覆膜栽培的集雨效果、土壤增温效果和西瓜增产效果,全膜和半膜覆盖垄上沟播模式能够起到集雨增温保墒的作用,可提高西瓜产量。其推广应用可有效提高该区降水资源的高效利用,实现西瓜稳产高产,可作为黄土高原旱地西瓜生产的高效栽培新模式。     

Dissection of QTLs for Yield Traits on the Short Arm of Rice Chromosome 6

This study was undertaken to dissect quantitative trait loci （QTLs） controlling yield traits on the short arm of rice chromosome 6. A residual heterozygous line that carries a heterozygous segment extending from RM587 to RM19784 on the short arm of rice chromosome 6 was selected from an F7 population of the indica rice cross Zhenshan 97B/Milyang 46. An F2：3 population consisting of 221 lines was derived and grown in two trial sites. Six yield traits including number of panicles per plant, number of filled grains per panicle, total number of spikelets per panicle, spikelet fertility, 1 000-grain weight, and grain yield per plant were measured. An SSR marker linkage map was constructed and employed to determine QTLs for yield traits with Windows QTL Cartographer 2.5. QTLs were detected in the target interval for all the traits analyzed except NP, with phenotypic variance explained by a single QTL ranging between 6.3% and 35.2%. Most of the QTLs for yield components acted as additive QTLs, while the three QTLs for grain yield had dominance degrees of 1.65, 0.84, and -0.42, respectively. It was indicated that three or more QTLs for yield traits were located in the target region. The genetic action mode, the direction of the QTL effect, and the magnitude of the QTL effect varied among different QTLs for a given trait, and among QTLs for different traits that were located in the same interval.     

稻虾共作磷素平衡特征及生态经济效益研究

为研究稻虾共作生态系统磷素平衡状况和利用效率,通过田间试验,采用投入产出法,设置3个处理:水稻单作(RM)、稻虾共作投食(RC feed 1)、稻虾共作不投食(RC feed 0),分析了稻虾共作种植模式下水稻产量、磷素平衡状况、利用效率、环境风险以及经济效益。研究结果表明:3种处理水稻产量无显著差异;农田磷平衡均表现为盈余,RC feed 0处理农田磷盈余低于RM和RC feed 1处理;与RM和RC feed 1处理相比较,RC feed 0处理水稻茎叶磷素吸收量显著增加(P0.05),磷素利用率较高。在种植前期(6—8月),RC feed 0处理较RC feed 1处理显著降低了稻田田面水总磷和溶解磷的浓度;在水稻收获时,3个处理间稻田田面水总磷和溶解磷的浓度无显著差异。与RM处理相比较,RC feed 0和RC feed 1处理净收入分别增加了54.22%和51.11%。在综合考虑水稻产量效应、磷素平衡、磷素环境风险和经济效益的条件下,稻虾共作不投食模式是一种资源利用率较高、环境风险较小、经济效益好的种养模式。     

Molecular Marker Assisted Selection for Yield-Enhancing Genes in the Progeny of Minghui63 × O.rufipogon

Two yield-enhancing genes (yldl.1 and yld2.1) are located on chromosomes 1 and 2 respectively in a weedy relative of cultivated rice, Oryza rufipogon. SSR markers RM9 and RM166 are closely linked with the two loci respectively. Minghui63 (MH63) has been a widely used restoration line in hybrid rice production in China during the past two decades. The F1 of cross "MH63 × O.rufipogon" was backcrossed with MH63 generation by generation. RM9 and RM166 were used to select the plants from the progeny of the backcross populations. The results were as follows: (1) In BC2F1 population, the percentage of the individuals which have RM9 and RM166 amplified bands simultaneously was 12.2%, while in the BC3F1 population, that was 16.3%. (2) Among 400individuals of BC3F1, four yield-promising plants were obtained, with yield being 30% more than that of MH63. (3) The products amplified by primer RM166 in O. rufipogon and MH63 were sequenced. It was found that the DNA fragment sequence amplified by RM166 from MH63 was 101 bp shorter than that from O. rufipogon. The 101 bp sequence is a part of an intron of the PCNA (proliferating cell nuclear antigen) gene.     

西北干旱灌区不同地膜覆盖利用方式对玉米水分利用的影响

【目的】资源型缺水严重制约干旱灌区的农业生产,传统玉米生产模式地膜投入量大。在极端高温和生态环境污染的挑战日益加剧的情境下,探讨通过免耕地膜重复利用维持较高水分利用的可行性,以期为构建试区地膜减量玉米高效生产技术提供理论支撑。【方法】2017—2018年,在甘肃河西绿洲灌区,设置免耕地膜重复利用（免耕覆膜,NM）、秋免耕春覆膜（少耕覆膜,RM）与传统耕作每年覆盖新膜（传统覆膜,对照,CM）3种地膜覆盖利用方式,研究其对玉米田土壤水分利用的影响,以期为优化试区玉米高产高效栽培管理技术提供理论依据。【结果】NM与RM处理较CM处理提高玉米播种时0—120 cm土层平均土壤重量含水量,分别为7.8%与5.1%,这为玉米播种创造良好的土壤水分环境。玉米播种—拔节期及吐丝—灌浆初期,NM处理较CM处理提高0—120 cm土层平均土壤重量含水量,分别为5.0%与4.7%,弥补了灌浆期玉米植株旺盛生长对土壤水分的大量需求。与CM处理相比,NM处理增加了玉米播种—大喇叭口期的耗水量,降低了玉米吐丝—灌浆初期的耗水量,增大了玉米灌浆初期—收获期的耗水量,有效协调玉米各生育阶段的水分需求关系。虽然NM处理较RM与CM处理提高了玉米吐丝期之前的棵间蒸发量,分别为11.7%与26.0%,提高棵间蒸发量占耗水量的比例（E/ET）,分别为13.4%与19.9%,但是NM处理较RM与CM处理降低了玉米吐丝期之后的棵间蒸发量,分别为9.2%与19.4%,降低E/ET,分别为9.7%与20.7%,说明NM处理有利于增强玉米吐丝期之后土壤水分的有效利用。因而,在地膜减投与免耕措施下,NM处理获得与RM及CM处理相当的籽粒产量与水分利用效率。【结论】在西北干旱灌区,应用免耕地膜重复利用并没有导致玉米产量和水分利用效率的降低,具有稳定产量及水分利用效率的作用,是玉米生产中地膜减投的可行措施。     

免耕“稻鳖鱼”共生模式的环境经济学分析

采用田间试验及环境经济学方法研究免耕"稻鳖鱼"共生模式的环境经济效益并提出相关对策。试验共设免耕稻鳖鱼(RTF),免耕稻鳖(RT)、免耕稻鱼(RF),免耕水稻单作(RM)4个处理。田间试验结果表明,RTF,RT,RF控草效果明显;孕穗期RTF病蔸率和病株率分别比RM低71.1%和56.3%。RTF固碳量比RM增加8.7%,甲烷(CH4)排放总量减少39.9%。环境经济学分析结果表明,RTF、RT、RF的财务效益,比RM分别增加了52 450、24 500、23 940元/hm~2,RTF、RT、RF和RM环境经济效益分别为53 547、25 385、24 927和559元/hm~2;研究结果表明,免耕稻鳖鱼共生模式生态和经济效益高,具有良好的发展和推广前景,可作为农业供给侧结构性改革形势下精准扶贫的新模式。     

Lunar magnetic field: permanent and induced dipole moments

Apollo 15 subsatellite magnetic field observations have been used to measure both the permanent and the induced lunar dipole moments. Although only an upper limit of 1.3 x 10(18) gauss-cubic centimeters has been determined for the permanent dipole moment in the orbital plane, there is a significant induced dipole moment which opposes the applied field, indicating the existence of a weak lunar ionosphere.     

Magnetic fields at uranus

The magnetic field experiment on the Voyager 2 spacecraft revealed a strong planetary magnetic field of Uranus and an associated magnetosphere and fully developed bipolar masnetic tail. The detached bow shock wave in the solar wind supersonic flow was observed upstream at 23.7 Uranus radii (1 R(U) = 25,600 km) and the magnetopause boundary at 18.0 R(U), near the planet-sun line. A miaximum magnetic field of 413 nanotesla was observed at 4.19 R(U ), just before closest approach. Initial analyses reveal that the planetary magnetic field is well represented by that of a dipole offset from the center of the planet by 0.3 R(U). The angle between Uranus' angular momentum vector and the dipole moment vector has the surprisingly large value of 60 degrees. Thus, in an astrophysical context, the field of Uranus may be described as that of an oblique rotator. The dipole moment of 0.23 gauss R(3)(U), combined with the large spatial offset, leads to minimum and maximum magnetic fields on the surface of the planet of approximately 0.1 and 1.1 gauss, respectively. The rotation period of the magnetic field and hence that of the interior of the planet is estimated to be 17.29+/- 0.10 hours; the magnetotail rotates about the planet-sun line with the same period. Thelarge offset and tilt lead to auroral zones far from the planetary rotation axis poles. The rings and the moons are embedded deep within the magnetosphere, and, because of the large dipole tilt, they will have a profound and diurnally varying influence as absorbers of the trapped radiation belt particles.     

多次回交水稻短根突变体RM1的农艺性状

用 射线处理水稻品种大力 ,在 M3世代中选育出短根突变体 RM1。现用回交的 RM1及原品种大力进行土培和水培试验 ,评价短根对产量及其农艺性状的影响。试验结果表明 ,回交的RMI根长、根数和根干重约为大力的 4 0 % ,14 0 %和 6 0 % ;株粒重及株高约为大力的 5 0 %及 90 %。短根形态对经济产量的影响大于对生物产量的影响。     

Magnetospheres of the galilean satellites

The plasma and field perturbations of magnetospheres that would surround magnetized galilean satellites embedded in the corotating jovian plasma differ from those produced by interaction with an unmagnetized conductor. If the intrinsic satellite dipole is antiparallel to that of Jupiter, the magnetosphere will be open. It is predicted that Io has an internal magnetic field with a dipole moment of 6.5 x 10(22) gauss-cubic centimeters antiparallel to Jupiter's, and Io's special properties can be interpreted on the basis of a reconnecting magnetosphere.     

The global magnetic field of Mercury from MESSENGER orbital observations

Magnetometer data acquired by the MESSENGER spacecraft in orbit about Mercury permit the separation of internal and external magnetic field contributions. The global planetary field is represented as a southward-directed, spin-aligned, offset dipole centered on the spin axis. Positions where the cylindrical radial magnetic field component vanishes were used to map the magnetic equator and reveal an offset of 484 ± 11 kilometers northward of the geographic equator. The magnetic axis is tilted by less than 3° from the rotation axis. A magnetopause and tail-current model was defined by using 332 magnetopause crossing locations. Residuals of the net external and offset-dipole fields from observations north of 30°N yield a best-fit planetary moment of 195 ± 10 nanotesla-R(M)(3), where R(M) is Mercury's mean radius.     

An episode of steep geomagnetic inclination 120,000 years ago

The mean inclinations of three sections of 120,000-year-old fine-grained sediments from northern California range from 62 degrees to 66 degrees . These inclinations are significantly steeper than the inclination of the geocentric axial dipole at this site. Because these sediments have probably recorded an actual episode of steep inclination lasting several thousand years, they provide new insights into the significance of mean inclinations shallower than the geocentric axial dipole. Such inclinations are characteristic of fine-grained sediments younger than 35,000 years. The results raise questions about the time-averaged geomagnetic field and about the determination of plate motions from paleomagnetic data.     

Magnetic field studies by voyager 1: preliminary results at saturn

Magnetic field studies by Voyager 1 have confirmed and refined certain general features of the Saturnian magnetosphere and planetary magnetic field established by Pioneer 11 in 1979. The main field of Saturn is well represented by a dipole of moment 0.21 +/- 0.005 gauss-R(s)(3) (where 1 Saturn radius, R(s), is 60,330 kilometers), tilted 0.7 degrees +/- 0.35 degrees from the rotation axis and located within 0.02 R(s) of the center of the planet. The radius of the magnetopause at the subsolar point was observed to be 23 R(s) on the average, rather than 17 R(s). Voyager 1 discovered a magnetic tail of Saturn with a diameter of approximately 80 R(s). This tail extends away from the Sun and is similar to type II comet tails and the terrestrial and Jovian magnetic tails. Data from the very close flyby at Titan (located within the Saturnian magnetosphere) at a local time of 1330, showed an absence of any substantial intrinsic satellite magnetic field. However, the results did indicate a very well developed, induced magnetosphere with a bipolar magnetic tail. The upper limit to any possible internal satellite magnetic moment is 5 x 10(21) gauss-cubic centimeter, equivalent to a 30-nanotesla equatorial surface field.     

Jupiter's Magnetic Field. Magnetosphere, and Interaction with the Solar Wind: Pioneer 11

The Pioneer 11 vector helium magnetometer provided precise, contititious measurements of the magnetic fields in interplanetary space, inside Jupiter's magnetosphere, and in the near vicinity of Jupiter. As with the Pioneer 10 data, evidence was seen of the dynanmic interaction of Jupiter with the solar wind which leads to a variety of phenomena (bow shock, upstream waves, nonlinear magnetosheath impulses) and to changes in the dimension of the dayside magnetosphere by as much as a factor of 2. The magnetosphere clearly appears to be blunt, not disk-shaped, with a well-defined outer boundary. In the outer magnetosphere, the magnetic field is irregular but exhibits a persistent southward component indicative of a closed magnetosphere. The data contain the first clear evidence in the dayside magnetosphere of the current sheet, apparently associated with centrifugal forces, that was a donminatnt feature of the outbound Pionieer 10 data. A modest westward spiraling of the field was again evident inbound but not outbound at higher latitudes and nearer the Sun-Jupiter direction. Measurements near periapsis, which were nearer the planet and provide better latitude and longitude coverage than Pioneer 10, have revealed a 5 percent discrepancy with the Pioneer 10 offset dipole mnodel (D(2)). A revised offset dipole (6-parameter fit) is presented as well as the results of a spherical harmonic analysis (23 parameters) consisting of an interior dipole, quadrupole, and octopole and an external dipole and quadrupole. The dipole moment and the composite field appear moderately larger than inferred from Pioneer 10. Maximum surface fields of 14 and 11 gauss in the northern and southern hemispheres are inferred. Jupiter's planetary field is found to be slightly more irregular than that of Earth.     

不同覆盖方式对辽西旱地玉米土壤温度和产量的影响

在大田试验条件下,研究了不同覆盖方式对辽西地区土壤温度和玉米产量的影响。结果表明,不同覆盖处理均可以不同程度的增加旱地玉米土壤温度,渗水地膜覆盖、普通地膜覆盖分别比常规种植（CK）高出5.4%、13.07%。其中,普通地膜的增温幅度最大,整个生育期内不同处理的土壤温度在10 cm和20 cm土层变化趋势基本一致;不同覆盖方式均能增加玉米产量,其中以渗水地膜覆盖增产效果最为明显,比常规种植增产219.19 kg/667m2,增产幅度达32.66%。说明渗水地膜覆盖方式是辽西地区提高土壤温度和玉米产量的最佳覆盖方式。     

水稻第6染色体短臂产量性状QTL簇的分解

【目的】将水稻第6染色体短臂上产量性状QTL分解到更小的区间中。【方法】从珍汕97B/密阳46重组自交系群体筛选到针对第6染色体短臂RM587-RM19784区间的剩余杂合体,衍生了一个由221个株系组成的F2:3群体,种植于海南和浙江两地,考察每株穗数、每穗实粒数、每穗总粒数、千粒重、结实率和单株产量,建立SSR标记连锁图,应用Windows QTL Cartographer 2.5检测QTL。【结果】在所分析的6个性状中,除穗数外在第6染色体短臂上的目标区间均检测到QTL,分别座落于目标区域中3个以上的不同区间中,单个QTL对群体性状表型变异的贡献率为6.3%～35.2%;控制产量构成因子的QTL基本以加性作用为主,但3个单株产量QTL的显性度分别为1.65、0.84和0.42。【结论】目标区间存在3个以上的产量性状QTL,且同一区间控制不同性状的QTL、不同区间控制同一个性状的QTL在遗传作用模式、效应方向和效应大小上存在一定差异。     

QTL Detection and Epistasis Analysis for Heading Date Using Single Segment Substitution Lines in Rice(Oryza sativa L.)

Heading date of rice is a key agronomic trait determining cultivated areas and seasons and affecting yield. In the present study, five primary single segment substitution lines with the same genetic background were used to detect quantitative trait loci(QTLs) for heading date in rice. Two QTLs, q HD3 and q HD6 on the short arm of chromosome 3 and the short arm of chromosome 6, respectively, were identified under natural long-day(NLD). Nineteen secondary single segment substitution lines(SSSLs) and seven double segments pyramiding lines were designed to map the two QTLs and to evaluate their epistatic interaction between them. By overlapping mapping, q HD3 was mapped in a 791-kb interval between SSR markers RM3894 and RM569 and q HD6 in a 1 125-kb interval between RM587 and RM225. Results revealed the existence of epistatic interaction between q HD3 and q HD6 under natural long-day(NLD). It was also found that q HD3 and q HD6 had significant effects on plant height and yield traits, indicating that both of the QTLs have pleiotropic effects.