Comet nuclei: Morphology and implied processes of surface modification     

A.T. Basilevsky  H.U. Keller 《Planetary and Space Science》2006,54(8):808-829

Surface morphology and related issues for nuclei of three comets: Halley, Borrelly and Wild 2, are considered in the paper. Joint consideration of publications and results of our analysis of the comets’ images led to conclusions, partly new, partly repeating conclusions published by other researchers. It was found that typical for all three nuclei is the presence of rather flat areas: floors of craters and other depressions, mesas and terraces. This implies that flattening surfaces or planation is a process typical for the comet nuclei. Planation seems to work through the sublimation-driven slope collapse and retreat. This requires effective sublimation so this process should work only when a comet is close to the Sun and if on the nucleus there are starting slopes, steep and high enough to support the “long-distance” avalanching of the collapsing material. If the surface had no starting slopes, then instead of planation, the formation of pitted-and-hilly surfaces should occur. An example of this could be the mottled terrain of the Borelly nucleus. Both ways of the sublimational evolution on the nucleus surface should lead to accumulation of cometary regolith. The thickness of the degassed regolith is not known, but it is obvious that in surface depressions, including the flat-floor ones, it should be larger compared with nondepression areas. This may have implications for the in situ study of comets by the Deep Impact and Rosetta missions.Our morphological analysis puts constraints on the applicability of the popular “rubble-pile comet nucleus” hypothesis (Weissman, 1986. Are cometery nuclei primordial rubble piles? Nature 320, 242-244.). We believe that the rubble pile hypothesis can be applicable to the blocky Halley nucleus. The Borelly and Wild 2 nuclei also could be rubble piles. But in these cases the “rubbles” have to be either smaller than 30-50 m (a requirement to keep lineament geometry close to ideal), or larger than 1-2 km (a requirement to form the rather extended smooth, flat surfaces of mesa tops and crater floors). Another option is that the Borelly and Wild 2 nuclei are not rubble piles.In relation to surface morphology we suggest that three end-member types of the comet nuclei may exist: (1) impact cratered “pristine” bodies, (2) non-cratered fragments of catastrophic disruption, and (3) highly Sun-ablated bodies. In this threefold classification, the Wild 2 nucleus is partially ablated primarily cratered body. Borrelly is significantly ablated and could be either primarily cratered or not-cratered fragment. Halley is certainly partially ablated but with the available images it is difficult to say if remnants of impact craters do exist on it.Recently published observations and early results of analysis of the Tempel 1 nucleus images taken by Deep Impact mission are in agreement with our conclusions on the processes responsible for the Halley, Borrelly and Wild 2 nuclei morphologies. In particular, we have now more grounds to suggest that decrease in crater numbers and increase of the role of smooth flat surfaces in the sequence Wild 2?Tempel 1?Borelli reflects a progress in the sublimational degradation of the nucleus surface during comet passages close to the Sun.  相似文献   

由对FRⅡ射电星系的X射线观测试预言射电噪活动星系核的X射线喷流     

白金明 《天文研究与技术》2003,(1):19-25

在早期的文章中,基于耀变体(Blazar)的知识,我们预言了在射电噪活动星系核(AGN)中心10 kpc范围内X射线喷流的存在.钱得拉(Chandra)卫星最近对低功率射电星系的X射线观测与我们的预言相一致.在本文中我们研究了kpc尺度喷流中的电子加速,并建议通过对强的FR Ⅱ射电星系中所预言的X射线喷流的钱得拉卫星的X射线的观测,来研究红的耀变体中的康普顿冷却以及在内部致密喷流和大尺度延伸喷流间环境的不同.以上的研究可以进一步检验我们的关于射电噪活动星系核中kpc尺度X射线喷流的模型.  相似文献   

云凝结核浓度对南京地区一次冰雹云过程影响的数值研究          下载免费PDF全文

刘晓莉  朱煜  孟翠丽  屈家安 《大气科学学报》2019,42(6):936-943

采用WRF模式与包含了云凝结核(Cloud Condensation Nuclei,CCN)浓度和霰雹密度预报的NSSL(National Severe Storm Laboratory,国家强风暴实验室)微物理方案,模拟不同CCN初始浓度条件下南京地区的一次冰雹云过程,分析不同CCN初始浓度影响下冰雹云过程的宏微观演变特征,以及对流发展不同阶段的水凝物粒子及流场、温度场的垂直分布特征。研究发现:1)较大的CCN初始浓度虽然抑制了前期对流降水,但对后期对流降水的产生有促进作用;2)CCN初始浓度的增加使得模拟雷达回波的强回波区域(大于40 dBz)缩小,中等强度区域(小于40 dBz)扩张。3)CCN初始浓度增大不利于对流发展初期云雨自动转化过程的发生,但是促进了冰晶与雪的产生,使得冰雹含量峰值出现的时间推迟。4)CCN浓度增大抑制了雨水产生,间接使得霰粒子更倾向于干增长,平均密度更小;5)较大的CCN浓度促使冰雹云单体的发展时间增长。  相似文献   

庐山变质核杂岩构造的初步研究   总被引：12，自引：2，他引：12  

项新葵  许建华 《华东地质学院学报》1994,17(1):11-17

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关于地球磁场极性反转机制的思索     

杨合群 《西北地质》2002,35(3):126-130

地球磁场极性在地质历史中发生过相当频繁的倒转。作者将地球内部划分为岩石圈－软流圈－中圈－液圈－固核等5个动力学圈层，认为中圈与固核间可异步旋转；地球偶极磁场由中圈与固核异步旋转时所驱动的液圈中的封闭涡流与系磁场作用产生；该偶极子场极性由地球所通过的银道面上侧或下侧磁场方向及液圈涡流的方向共同决定，二者之一反向，极性发生倒转。  相似文献   

西沙群岛大气中海盐粒子的分布特征   总被引：9，自引：1，他引：9  

吴兑  游积平  关越坚 《热带气象学报》1996,12(2):122-129

分析了在西沙永兴岛观测的Ｃｌ＾－海盐核资料，主要结果有：（１）东北季风期干直径大于２μｍ的Ｃｌ＾－核平均浓度８７８个／Ｌ，平均含盐量１０５．４μｇ／ｍ＾３，其中干直径大于４μｍ的特大核平均为１９０个／Ｌ，最大间观测到干直径５７μｍ的Ｃｌ＾－粒子，均较该地在１９８７年５月西南季风盛行期的观测值高。谱型呈准单调下降的幂函数递减谱。（２）随距海面高度增加海盐粒子浓度与含盐量均有所减小。（３）Ｃｌ＾－粒子  相似文献   

大气冰核浓度对对流云降水过程影响的数值模拟     

王梦旖  师正  谭涌波  刘俊  于梦颖  郑天雪 《气象科技》2020,48(2):220-228

在已有的三维对流云模式的基础上新植入了同质冻结和异质核化方案,结合一次山地雷暴个例,通过敏感性试验来探讨大气冰核浓度对对流云微物理过程和降水的影响。模拟结果表明:①冰核浓度的改变会对对流云的动力场及各水成物粒子产生明显作用。增加冰核浓度,冰相粒子的数浓度随之增加;同时,凝华过程中释放大量潜热导致云中上升气流增强。由于水汽含量一定,各水成物粒子"争夺"水汽,使得云滴、冰晶和霰的增长均受到抑制,难以成为较大尺寸的降水粒子。②冰核浓度的增加,"贝吉龙效应"导致云滴的尺度减小,削弱了云-雨转化过程。雨滴、云滴混合比的减小抑制了雨滴对云滴的收集。同时,小尺度的霰粒子削弱了霰融化为雨滴的物理过程,最终导致地面累积降雨量降低。  相似文献   

是地层单元还是构造单元？   总被引：6，自引：0，他引：6       下载免费PDF全文

王仁民  倪志耀童　英 《中国地质》2002,29(3):281-285

古大陆边缘变质地质体性质的确定对于探讨大地构造演化具有十分重要的意义。由于后期变形变质作用的影响,原先不同的构造单元往往被改造成看似完整的一套地层单元,但在同位素年龄、变质程度、岩浆活动与地层的专属组合及其空间延伸等方面则变化很大,这在华北古陆北缘的单塔子群和南缘的太华群中最为典型。因此,笔者建议用“构造－岩相杂岩体带”填图法来取代以地层为骨架的变质岩区地质制图,这有助于确定该地区的大地构造演化进程。  相似文献   

Mkn501长期光变性质     

杨江河  樊军辉  刘怡  王永祥  杨如曙 《天文学报》2007,48(4):407-417

在R和I波段对Mkn 501进行了测光观测,并结合历史文献得到Mkn 501在近30年间的光学、红外和射电等多个波段的光变曲线;讨论了光变与色指数之间的关系,发现色指数(B—V)与(B—R)之间有强相关,相关系数r=0.73.利用DCF方法分析了多波段光变的相关性,发现B波段与4.8GHz和红外波段的光变存在一定的正相关,利用CLEANest方法对B波段的光变曲线进行频谱分析,结果表明Mkn 501的光变曲线存在2个可能的周期,即(10.06±0.04)年和(21.60±0.17)年.  相似文献   

Searching for the Deep Impact crater on Comet 9P/Tempel 1 using image processing techniques     

I. Busko  D. Lindler  R.L. White 《Icarus》2007,187(1):56-68

In this work we attempt to obtain direct images of the crater associated with the impact of the Deep Impact impactor spacecraft on the nucleus of Comet 9P/Tempel 1 on July 4, 2005. The impact generated a large and bright ejecta cloud that hampers the clear view of the post-impact nucleus surface. We used image restoration techniques to enhance spatial resolution and contrast on a subset of selected post-impact high resolution images. No unambiguous evidence for the crater can be found; however, indirect evidence is consistent with a crater size in the 150-200 m range.  相似文献