The light curve of asteroid 2867 Steins measured by VIRTIS-M during the Rosetta fly-by     

F. Tosi  A. Coradini  G. Filacchione  M.C. De Sanctis  M.A. Barucci  S. Mottola  E. Dotto  The VIRTIS Team 《Planetary and Space Science》2010,58(9):1066-1076

On 5 September 2008, the Rosetta spacecraft encountered the asteroid 2867 Steins on its way to the comet 67P/Churyumov-Gerasimenko. This was the first of two planned asteroid fly-bys performed by the probe, the second fly-by being with the much larger asteroid 21 Lutetia in July 2010. The VIRTIS imaging spectrometer (IFOV 0.250 mrad, overall spectral range 0.25-5.1 μm) onboard Rosetta acquired data of Steins already before the closest approach phase, when the target was spatially unresolved, in order to obtain a light curve of the asteroid in the infrared spectral range extending up to 5 μm, that was never explored before. The VIRTIS light curve campaign started at 11:30 UTC onboard time, when the spacecraft was about 221,377 km away from the target, and ended at 17:58 UTC, at a distance of 20,741 km away from Steins. During this timeframe, the solar phase angle of the asteroid was roughly constant, ranging from 38.2° to 36.3°.Assuming the most recent value derived for the rotational period of Steins (Lamy et al., 2008), the VIRTIS observations covered slightly more than one rotation of the asteroid. In this interval, VIRTIS collected 8 hyperspectral cubes where Steins was captured 119 times, both in the visual and in the infrared range. Given the low signal and the unresolved appearance of the source, for which the instrument was not designed, only a small subset of wavelengths turned out to be suitable to sample the light curve. Nevertheless, in both the VIS and NIR ranges we find a similar trend, with two different maxima and minima during one rotational period, and amplitudes consistent with the results in the visual range obtained in previous works, including the data set acquired by the OSIRIS camera onboard Rosetta. We also report the presence of a new broad feature centered at approximately 0.81-0.82 μm, which is seen in the visual data throughout the rotation of the asteroid.  相似文献   

Abundances of Jupiter's trace hydrocarbons from Voyager and Cassini     

C.A. Nixon  R.K. Achterberg  P.N. Romani  X. Zhang  P.G.J. Irwin 《Planetary and Space Science》2010,58(13):1667-1680

The flybys of Jupiter by the Voyager spacecraft in 1979, and over two decades later by Cassini in 2000, have provided us with unique datasets from two different epochs, allowing the investigation of seasonal change in the atmosphere. In this paper we model zonal averages of thermal infrared spectra from the two instruments, Voyager 1 IRIS and Cassini CIRS, to retrieve the vertical and meridional profiles of temperature, and the abundances of the two minor hydrocarbons, acetylene (C₂H₂) and ethane (C₂H₆). The spatial variation of these gases is controlled by both chemistry and dynamics, and therefore their observed distribution gives us an insight into both processes. We find that the two gases paint quite different pictures of seasonal change. Whilst the 2-D cross-section of C₂H₆ abundance is slightly increased and more symmetric in 2000 (northern summer solstice) compared to 1979 (northern fall equinox), the major trend of equator to pole increase remains. For C₂H₂ on the other hand, the Voyager epoch exhibits almost no latitudinal variation, whilst the Cassini era shows a marked decrease polewards in both hemispheres. At the present time, these experimental findings are in advance of interpretation, as there are no published models of 2-D Jovian seasonal chemical variation available for comparison.  相似文献   

环境因子对萱藻(Scytosiphon lomentaria) 孢子附着的影响   总被引：1，自引：0，他引：1  

张文健  宫相忠  高伟 《海洋与湖沼》2013,44(6):1661-1666

将实验室保存的萱藻丝状体经过扩增、诱导得到具有成熟孢子囊的丝状体作为实验材料, 在实验室条件下研究了光照强度[0—126?mol/(m2·s)]、温度(7—27℃)、盐度(8—56)、pH(6.7—9.7)对萱藻孢子附着的影响。结果表明: (1) 萱藻孢子附着的最适光照强度为54?mol/(m2·s), 在此光照强度下, 单位面积的孢子附着量最大; (2) 温度对萱藻孢子附着的影响显著, 19℃是萱藻孢子附着的最佳温度条件; (3) 盐度过低(≤24)或过高(≥40)都会造成孢子的死亡, 萱藻孢子附着的最适盐度为30; (4) 在设定的pH范围内, 当pH为8.2时, 最有利于萱藻孢子的附着。  相似文献   

武汉市盛夏高温气候特征和成因及预报   总被引：4，自引：0，他引：4  

贺懿华  谌伟  李才媛  王丽  顾永刚 《气象科技》2007,35(6):809-813

利用1950～2005年盛夏(7～8月)逐日武汉市最高温度、2002年和2003年6～8月T213格点风和垂直速度资料,分析了武汉盛夏高温的气候特征,研究了高温过程及西太平洋副热带高压活动特点。分析结果表明:20世纪50年代末至60年代初、60年代中期、70年代后期、90年代和2000～2005年为高温日数偏多的5个阶段。80年代高温日数偏少。对较大的时间尺度而言,强的高温集中在50年代后期至60年代以及90年代后期至2005年。强高温过程集中在7月下旬至8月上旬。西太平洋副热带高压持续稳定控制长江中下游,是造成高温及强高温过程的主要环流系统。选用ECMWF和T213温度和纬向风场预报产品,应用灰色预测方法建立了武汉市盛夏日最高温度预报模型,该模型试用于2003年和2006年盛夏高温预报,检验结果表明该模型提供的高温定量预报有一定的参考价值。  相似文献   

地面气象站环境变化对气温序列均一性影响   总被引：12，自引：3，他引：9  

吴利红  康丽莉  陈海燕  马仙妹 《气象科技》2007,35(1):152-156

为研究浙江省地面气象站环境变化对气温序列均一性的影响程度,采用测站历史沿革资料,对全省测站环境的时空演变进行了分析。采用距平累加、偏差界限值、F值检验法,对36个代表站的年平均气温序列进行均一性检验,并对非均一性产生的原因进行分析。结果表明:1971~2004年,浙江省测站的地理环境有显著改变;36站中有39%的测站为非均一性,产生非均一性的测站中,迁站原因占57%,环境恶化占36%;测站迁站引起的非均一性多发生在1980年以后;测站迁站时,新旧站址海拔高度差大且地理环境差异显著是造成气温序列非均一性的主要原因,迁站后气温序列较旧址存在偏高或偏低现象,其值对累年平均值有影响。指出了测站在迁移或环境变化过程中应注意的事项,以助于减少气温序列非均一性。  相似文献   

Seasonal oscillations in mesospheric temperatures at low-latitudes     

Y. Zhao  M.J. Taylor  H.-L. Liu  R.G. Roble 《Journal of Atmospheric and Solar》2007,69(17-18):2367

Using 3 years of high-quality temperature measurements (2002–2004) recorded from Maui, HI (20.8°N), we have investigated the characteristics of mesospheric seasonal oscillations at low-latitudes. Measurements of the near-infrared OH (6,2) and O₂ (0,1) nightglow emission layers (centered at 87 and 94 km) independently reveal a distinct semi-annual oscillation (SAO) and annual oscillation (AO) with amplitudes of 3.8 and 2.0 K, respectively. An observed asymmetry in the seasonal variation of the nocturnal mean, previously reported by Taylor et al. [2005. Characterization of the semi-annual-oscillation in mesospheric temperatures at low-latitudes. Advances in Space Research 35, doi:10.1016/j.asr.2005.05.111] from this site is shown to be due to a superposed AO of amplitude 50% of the SAO signature. Detailed investigations of the local-time variation of the SAO amplitude and phase combined with TIME-GCM simulations of the seasonal variation of the diurnal tide strongly suggest a large local-time dependence of the amplitude (but not phase) of the observed SAO. These data indicate that the true mean temperature SAO amplitude could be as high as 7 K at this latitude.  相似文献   

Gemini-N mid-IR observations of the dust properties of the ejecta excavated from Comet 9P/Tempel 1 during Deep Impact     

David E. Harker  Charles E. Woodward  R. Scott Fisher 《Icarus》2007,190(2):432-453

We present mid-infrared spectra and images from the Gemini-N (+MICHELLE) observational campaign of Comet 9P/Tempel 1 before, during, and after its encounter with Deep Impact. We use our thermal grain model to probe the 10 μm properties of the dust grains in the coma of the comet. Before impact (3 July 2005 UT), and more than 24 h after impact (5, 16, and 28 July 2005 UT), the comet dust grains were composed mostly of amorphous olivine, and were relatively large (peak of the grain size distribution ). For the night of impact, we extract spectra by centering on the nucleus, and offset 1″ from the nucleus in the direction of the impact ejecta plume. We find small dust grains (∼0.2 μm) of a diverse mineralogy (amorphous olivine, amorphous pyroxene, amorphous carbon, and crystalline olivine) populating the ejecta. The submicron sized dust grains move faster than the other, larger grains (?0.7 μm), with amorphous olivine and amorphous carbon traveling together, and amorphous pyroxene and crystalline olivine dispersing at a similar rate. Deriving a velocity law from a time-of-flight analysis, we find that the material traveled with a velocity law scaled by and with a power of p=0.5. This velocity power-law requires a sustained release of grains for the duration of 45-60 min after impact. Since the mineral species are traveling at different speeds, and there was a sustained release of grains due to a possible “gas-plume,” we conclude that the different minerals did not originate from grain aggregates destroyed by the impact, but instead arise from an inhomogeneous nucleus.  相似文献   

贵州纳雍水东铅锌矿床石英包裹体特征及成矿温度研究   总被引：4，自引：2，他引：2  

吴波  陈国勇 《贵州地质》2010,27(2):100-105

利用显微测温学的方法,对纳雍水东铅锌矿床中石英进行显微及包裹体测温研究。研究表明,石英的流体包裹体主要以气液相包裹体居多,纯液相次之。包裹体测温结果显示,成矿流体冰点温度为-12.5℃~0.1℃,均一温度变化范围为122.1℃~307.0℃,峰值范围为120℃~150℃,反映出中低温成矿的特征;流体盐度W(NaC leq)%变化范围为0.18%~16.43%,平均盐度7.05%;流体密度为0.8 g/cm3~1.02g/cm3,平均密度0.95 g/cm3;成矿压力为87.86×105Pa~351.94×105Pa,其对应的成矿深度为0.29 km~1.17 km之间,平均成矿深度为0.50 km。综合研究表明本区矿床为典型的中低温热液铅锌矿床,成矿流体呈现中低温、低盐度、中等密度、低压、浅成相的矿床成矿环境特征。  相似文献   

极干旱地区土壤与大气水分的相互影响     

李红寿  汪万福  张国彬  邱飞  詹鸿涛 《西安地质学院学报》2010,(2):183-188

基于建立在莫高窟窟顶的密闭拱棚,通过监测棚内凝结水量和空气温湿度,对极干旱地区典型极干旱气候条件下土壤与大气水分的相互影响进行综合分析。棚内凝结水量和空气温湿度的监测结果表明,在热动力作用下存在地下水分向大气输送的过程,其原因主要是在温度作用下土壤结合水分的分解蒸发与土壤盐分的吸湿吸附的交替作用。这也是形成所谓“土壤凝结水分”与“土壤水分呼吸”的根源。当温度升高时,土壤结合水分分解蒸发“呼出”水分,当温度降低时土壤盐分吸湿吸附,“吸入”大气水分,形成土壤与大气不对称水分交流。称质量实验表明：土壤水分的变化与空气温度的变化完全对应;有深层水分支持的土壤吸收大气水分的能力相对较差。极干旱地区土壤与大气水分的相互影响研究结果能为莫高窟珍贵文物的保护提供参考。  相似文献   

Review on physical models of lunar brightness temperature     

Jianqing Feng  Yongliao Zou  Wei Bian  Yongchun Zheng  Chunlai Li 《中国地球化学学报》2010,29(2):204-211

Brightness temperature is a main index to reflect the energy of microwave radiation of an object. Using lunar brightness temperature data, physical properties of lunar regolith, such as thickness, heat flow and dielectric permittivity, could be interpreted. There are two methods to study brightness temperature distribution of the moon: the first is used to measure lunar brightness temperature by radio observation or spaceborne microwave radiometers, and the second is used to simulate calculation by the physical model. On the basis of the measurements of lunar brightness temperature in the history, this study analyzed the main physical model of lunar brightness temperature, also including its theory and influence factors. The authors concluded that surface and subsurface temperatures of the moon, dielectric properties and layered structure of lunar regolith were the main factors affecting the global brightness temperature of the moon. These factors should be quantified in detail in the future research.  相似文献