三塘湖盆地火山岩油气藏油气充注幕次及成藏年龄确定

油气藏油气充注幕次和成藏年龄确定一直是成藏过程研究的热点和核心问题.通过60块流体包裹体系统分析, 结合单井埋藏史投影方法, 分析了三塘湖盆地火山岩油气藏的油气充注幕次和成藏期次, 确定了其成藏年龄, 从而对其油气成藏过程进行了研究, 认为三塘湖盆地火山岩油气藏经历了石炭纪以来三期油气运聚的成藏过程.它们分别发生在259~230Ma、160~134Ma和70~0Ma, 其中早期(海西印支期)油气成藏对盆地深部油气勘探具有重要意义.      

西藏谢通门县雄村铜金矿主要地质体的40Ar/39Ar年龄及地质意义

雄村铜金矿Ⅱ号矿体在2007-2008年取得了重大的找矿突破,详细的地质编录成果表明,矿体同样受含眼球状石英斑晶的角闪石英闪长玢岩和角闪石英闪长玢岩控制.含眼球状石英斑晶的角闪石英闪长玢岩和角闪石英闪长玢岩的锆石U-Pb年龄已经确定(164～177 Ma),因此,雄村铜金矿不同地质体的云母类、长石类矿物Ar-Ar同位素年龄的测定显得尤为关键.文章通过对穿切I号矿体的黑云母花岗闪长岩、云煌岩脉的黑云母Ar-Ar同位素测年,结合其他研究者的成果,得到一组十分重要的年龄数据.穿插矿体的黑云母花岗闪长岩中的黑云母(样号6187-335)坪年龄(46.96±0.42)Ma,穿插矿体的无矿化的云煌岩(5053-324.4)(Cu含量0.0551%,Au含量0.034 g/t,Ag0.6 g/t)中的黑云母给出了一个较好的似坪年龄,加权平均年龄为(49.59±0.58)Ma.结合其他研究者测定的中侏罗世侵位的角闪石英闪长玢岩(不含矿)[锆石U-Pb年龄为(177.1±2.0)Ma]中黑云母的At-At同位素年龄为(48.57±0.31)Ma;含矿凝灰岩围岩[锆石U-Pb年龄为(176±5)Ma,MS3VD=0.63}的蚀变绢云母Ar-Ar年龄为(47.07±0.30)Ma;似伟晶岩中长石的At-At年龄为(47.62±0.7)Ma,认为不同形成时代、不同产出空间、不同矿化程度的地质体的云母类、长石类矿物的Ar-Ar同位素年龄的一致性,反映了后期岩浆热事件对中侏罗世早期形成的地质体和矿体的黑云母氩同位素体系产生了较强的扰动或置换.谢通门大岩基黑云母花岗闪长岩的侵位致使各地质体发生显著的退变质,形成典型的角岩化带,这种退变质的时限在46-48 Ma之间的始新世lutetian期,进而认为各地质体中云母类矿物的~(40)Ar/~(39)Ar同位素年龄不能作为成矿年龄.     

棉花坑铀矿床花岗质脉岩地球化学特征及其与铀成矿的关系

粤北棉花坑铀矿床矿体产于一组陡倾的、近南北向展布的构造蚀变带中,在矿体附近多见有细粒花岗质岩脉穿插,通过对该类脉岩的研究表明,其锆石 U Pb 年龄为138．6±1．3 Ma （MSWD＝0.81）,属于晚燕山期岩浆活动的产物.脉岩的硅含量高,镁、铁、钙和钛含量低, ACNK 值均＞1.1, CaO/Na2 O值＜0.3,刚玉分子数C＞1.8％,属于典型的 S型花岗岩类;脉岩中富集大离子元素K、Rb、Th而亏损Ba、Sr、Ti和P,稀土总量低,配分模式明显呈海鸥型,且表现出一定程度的“四分组效应”, Eu亏损明显.细粒花岗质脉岩的侵入作用使围岩中的铀活化、预富集,因此铀矿化与其有成因联系.     

钦杭成矿带西段罗容杂岩体岩石学、地球化学及年代学

罗容杂岩体主要由二长闪长岩、二长岩、二长正长岩和正长岩组成。岩石以富碱、富含Ba、K、Rb、Sr、Ga等大离子亲石元素(LILE)和LREE、Nb、Ta、Zr、Hf、Th、U、Y等高场强元素(HFSE)为主要特征,属钾玄岩系列。对罗容杂岩体进行了高精度的LA-ICP-MS锆石U-Pb定年,获得角闪辉石二长岩等时线年龄为163.40±0.40 Ma(MSWD=0.12)。研究认为罗容杂岩体形成于中侏罗世,属于A1亚型花岗岩,形成于燕山早期华南后造山阶段大陆地壳拉张减薄的构造环境。     

桂东北越城岭—苗儿山地区印支期成矿作用：油麻岭和界牌矿区成矿花岗岩锆石U-Pb年龄和Hf同位素制约

提要：油麻岭和界牌矿床是越城岭—苗儿山地区两个钨多金属矿床,规模均达到中型,主要矿体均产在中细粒(斑状)二长花岗岩接触带附近矽卡岩和破碎带中。本研究利用LA-MC-ICP-MS微区原位测试技术,对油麻岭矿化花岗岩和界牌内接触带花岗岩中的锆石进行了U-Th-Pb和Hf同位素分析。结果显示,油麻岭矿化花岗岩锆石U-Pb年龄为（220±1）Ma（MSWD=0.035）,界牌内接触带花岗岩锆石U-Pb年龄为（215±1）Ma（MSWD=0.055）,间接指示越城岭—苗儿山地区存在印支期成矿作用。油麻岭花岗岩样品εHf(t)值在-2.47~-6.67,界牌花岗岩样品εHf(t)值在-3.52~-6.79,表明这两个矿区花岗岩都是源于地壳物质的重熔。与南岭地区其他成钨花岗岩比较,两者源区均具有高εHf(t)值特征,可能是较多εHf(t)值＞0的新元古代新生岛弧地壳组分加入引起的。本文获得及前人发表的印支期同位素年龄表明,桂北地区经历了较强的印支期成岩成矿事件,有较好的找矿前景,今后应注意区内印支期花岗岩出露区的勘查评价工作。     

Do young martian ray craters have ages consistent with the crater count system?

McEwen et al. (McEwen, A.S., Preblich, B.S., Turtle, E.P., Artemieva, N.A., Golombek, M.P., Hurst, M., Kirk, R.L., Burr, D.M., Christensen, P. [2005]. Icarus 176, 351-381) developed a useful test for the internal consistency of crater-count chronometry systems. They argued that certain multi-kilometer, fresh-looking martian craters with prominent rays should be the youngest or near-youngest craters in their size range. The “McEwen et al. test” is that the ages determined from crater densities of the smallest superimposed craters (typically diameter D ∼ 5-20 m) should thus be comparable to the expected formation intervals of the host primary. McEwen et al. concluded from MOC data that crater chronometry failed this test by factors of 700-2000. We apply HiRISE and other imagery to eight different young craters in order to re-evaluate their arguments. We use existing crater chronology systems as well as the reported observed production rate of 16 m craters (Malin, M.C., Edgett, K., Posiolova, L., McColley, S., Noe Dobrea, E. [2006]. Science 314, 1573-1557; Hartmann, W.K., Quantin, C., Mangold, N. [2007]. Icarus 186, 11-23; Kreslavsky [2007]. Seventh International Conference on Mars, 3325). Every case passes the McEwen et al. test. We conclude that the huge inconsistencies suggested by McEwen et al. are spurious. Many of these craters show evidence of impact into ice-rich material, and appear to have ice-flow features and sublimation pits on their floors. As production rate data improve, decameter-scale craters will provide a valuable way of dating these young martian geological formations and the processes that modify them.     

UVolution: Compared photochemistry of prebiotic organic compounds in low Earth orbit and in the laboratory

Solar UV radiation is a major source of energy for chemical evolution of organic materials in the Solar System. Therefore studies on the photostability of organic compounds in extraterrestrial environments are of prime importance for the understanding of the extraterrestrial origin of organic materials on Earth. A series of organic samples have been photolysed in Earth orbit during the ESA BIOPAN 6 mission (14-26/09/2007). Their photochemical lifetime has been measured and compared to results recorded in the laboratory using a lamp that simulates the solar radiation in the VUV domain. The half-lives at a distance of 1 AU from the Sun have been measured for glycine, xanthine, hypoxanthine, adenine, guanine, urea, carbon suboxide polymer ((C₃O₂)_n) and HCN polymer. They range from a few days to a lower limit of a few tens of days for the most photoresistant (e.g. adenine, guanine, hypoxanthine). Lifetimes measured in terrestrial orbit are very different from those derived with laboratory experiments. These measurements confirm that it is difficult to simulate the solar spectrum below 200 nm in the laboratory. Results are discussed and highlight the necessity to conduct experiments in orbit, and for longer duration. It also appears that the laboratory measurements made in VUV must be extrapolated very cautiously to the different environments they are supposed to simulate.