鲁西南地区地下水锰的分布特征及其成因

为了解鲁西南地区地下水中锰的含量及其成因,采集并分析了276组地下水样和18组地表水样,结果表明,鲁西南平原区浅层地下水中锰含量在未检出至2.84mg/L之间,平均浓度为0.35mg/L,超标率达41%。鲁西南地区地下水中锰含量的分布与该区的工业化程度以及所处的补、径、排条件密切相关。影响地下水中锰含量分布的因素主要有表层土壤、地下水径流条件及含水层介质和地下水矿化度等。     

龙湾套铜矿岩石学特征及矿床成因

泗水县龙湾套地区发育大面积新太古代角闪辉长岩,为在该区寻找赋存在角闪辉长岩中的岩浆熔离型铜矿床,曾开展过普查工作,最终发现了一小型铜矿床。探讨该区角闪辉长岩岩石学特征,对在该区进一步寻找同类型铜矿床有重要意义。     

临沂市城区岩溶塌陷特征及成因分析

自20世纪80年代以来,临沂市城区一带发生多起岩溶塌陷,这些岩溶塌陷发生具有突发性、重复性,其分布具有一定的规律性;其形成原因一方面取决于该区具备岩溶塌陷形成的物质基础条件,另一方面取决于水动力条件的改变,而水动力条件的改变主要是由于城区地下水不合理开采造成的。     

贵州碳酸盐岩风化壳中晶体石英形成条件分析:氧同位素证据

贵州碳酸盐岩风化壳中的晶体石英具有较强的测年潜力,其成因判别是年代学研究的前提和基础。对黔北、黔东地区3个碳酸盐岩风化壳剖面中的晶体石英和圆状石英进行了研究,拟通过晶体石英的δ18O值探讨其形成条件。结果表明,晶体石英的δ18O值在17.3‰～22.7‰范围内,平均为19.8‰,与火成岩、变质岩及热水(液)沉积中高温成因石英δ18O值明显不同;与砂岩中的碎屑石英、现代海滨砂中的石英以及风成沉积物中的石英等混合来源石英的δ18O值也有差异;尽管黔东大兴剖面中晶体石英和圆状石英的δ18O值相近,但它们的硅氧同位素相关关系不同,它们具有不同的成因;晶体石英的δ18O值分布在低温成因石英δ18O值范围内,这与其中未见两相包裹体的现象一致。结合实际资料和已有认识,推断晶体石英是包气带地表温度(15～25℃)条件下缓慢生长形成的;其形成过程与碳酸盐岩风化成土的两阶段模式密切相关:酸不溶物风化形成的含硅流体向下淋滤至风化壳底部后被圈闭在已形成的孔隙、空洞中,由于蒸发作用达到过饱和而缓慢结晶形成晶体石英。     

冕环电流的成因分析

将冕环电流按成因分成三种类型：对流电流、感应电流和自举电流，并分别进行了讨论。将tokamak等离子体中的自举电流的概念引入到冕环中，初步分析表明在部分冕环中也可能产生可观的自举电流。这种电流的存在将对冕环的稳定性将产生重要的影响。     

Rebuttal to “Comment on the paper “Comparison of the composition of the Tempel 1 ejecta to the dust in Comet C/Hale-Bopp 1995 O1 and YSO HD 100546” by C.M. Lisse, K.E. Kraemer, J.A. Nuth III, A. Li, and D. Joswiak"

This response is to address the comments made by Drs. J. Crovisier and D. Bockelee-Morvan concerning the spectral analysis of Lisse et al. [Lisse, C.M., Kraemer, K.E., Nuth, J.A., Li, A., Joswiak, D., 2007. Icarus 187, 69-86] of the mid-IR ISO SWS spectrum of Comet Hale-Bopp 1995 O1 taken on October 6, 1996, and to support the conclusions made in Lisse et al. concerning the positive detection of PAHs in this comet. We also present some additional information determined from the Deep Impact and STARDUST missions, demonstrating the presence of PAHs in other comets, to support the plausibility of the Hale-Bopp PAH detection.     

IRCS/Subaru observations of water in the inner coma of Comet 73P-B/Schwassmann-Wachmann 3: Spatially resolved rotational temperatures and ortho-para ratios

Comet 73P-B/Schwassmann-Wachmann 3 was observed with IRCS/Subaru at geocentric distance of 0.074 AU on UT 10 May 2006. Multiple H₂O emission lines were detected in non-resonant fluorescence near 2.9 μm. No significant variation in total H₂O production rate was found during the (3 h) duration of our observations. H₂O rotational temperatures and ortho-to-para abundance ratios were measured for several positions in the coma. The temperatures extracted from two different time intervals show very similar spatial distributions. For both, the rotational temperature decreased from ∼110 to ∼90 K as the projected distance from the nucleus increased from ∼5 to ∼30 km. We see no evidence for OPR change in the coma. The H₂O ortho-para ratio is consistent with the statistical equilibrium value (3.0) for all spatially resolved measurements. This implies a nuclear spin temperature higher than ∼45 K.     

Activity of comets at large heliocentric distances pre-perihelion

We present observational data for two long-period and three dynamically new comets observed at heliocentric distances between 5.8 to 14.0 AU. All of the comets exhibited activity beyond the distance at which water ice sublimation can be significant. We have conducted experiments on gas-laden amorphous ice samples and show that considerable gas emission occurs when the ice is heated below the temperature of the amorphous-crystalline ice phase transition (T∼137 K). We propose that annealing of amorphous water ice is the driver of activity in comets as they first enter the inner Solar System. Experimental data show that large grains can be ejected at low velocity during annealing and that the rate of brightening of the comet should decrease as the heliocentric distance decreases. These results are consistent with both historical observations of distant comet activity and with the data presented here. If observations of the onset of activity in a dynamically new comet are ever made, the distance at which this occurs would be a sensitive indicator of the temperature at which the comet had formed or represents the maximum temperature that it has experienced. New surveys such as Pan STARRS, may be able to detect these comets while they are still inactive.     

Electric Discharges in the Protoplanetary Nebula as a Source of Impulse Magnetic Fields to Promote Dust Aggregation

Lightning discharge generated in the protoplanetary nebula is viewed as a temporally isolated surge in the flow of electrically charged particles, similar to that of terrestrial lightning. If the current is intense enough, a powerful circular impulse magnetic field is generated around the instantaneous virtual electric conductor. Such magnetic field is capable of magnetizing dust grains containing ferromagnetic components present in its vicinity to their saturation levels. As a result, dust grains attract one another, forming the aggregates. This magnetically driven attraction suggests an important process possibly operational at an early stage of the planetary accretion. Based on both a classical model for electric conductor, and the theory of Lienard–Wiechert electromagnetic potentials, our calculations show that the magnetic impulse due to a discharge channel of a few cm in diameter transferring a charge of about 10⁴ electrons reaches as high as 10 T. At these magnetic fields, the ferromagnetic dust grains, and possibly the already-formed larger aggregates as well, are easily magnetized to the saturation levels, producing compact clusters exhibiting permanent magnetic moments.