Evidence for an Hesperian-aged South Circum-Polar Lake Margin Environment on Mars

A broad pitted plain and an elongated low rise occur near the south pole of Mars between a region of major cavi (Cavi Angusti) and a regionally smooth and broad valley (Argentea Planum). Viking, Mars Global Surveyor (MGS), and Odyssey data reveal a densely pitted plain covering ∼6750 km², and containing >300 irregularly shaped, steep-walled and flat-floored depressions with a mean diameter of ∼3.5 km. At the southernmost (poleward) extent of this plain are 12 north/south trending linear valleys that are characterized by theater-shaped heads abutting a major cavi within Cavi Angusti. The pitted plain, which abuts Cavi Angusti to the southwest, is separated from the floor of Argentea Planum by a smooth, elongated low rise that extends parallel to the plain for ∼200 km. These unusual features are all found within the Hesperian-aged circumpolar Dorsa Argentea Formation, which has been interpreted by some workers to be an ice-rich glacier-related deposit. We interpret the pitted plain to represent the maximum northern extent of the Angusti lobe ice deposit. The pits are analogous in morphology and distribution to terrestrial kettle holes, which form from the melting of isolated ice-blocks surrounded and partly buried by sediment, to leave hollows. The linear valleys are consistent with sapping valleys formed from the release of an elevated groundwater table, fed by meltwater lakes. On the basis of these characteristics, relationships and analogs, we interpret the marginal facies to represent an ice-sheet/lake contact environment that existed during Hesperian time.     

Searches for bright-rimmed clouds with IRAS point sources

We have carried out systematic surveys for small bright-rimmed clouds associated with IRAS point sources in/around HII regions. They are candidate sites for star formation due to radiation-driven implosion.     

Acoustic-Gravity Waves from Bolide Sources

We have developed a new approach to modeling the acoustic-gravity wave (AGW) radiation from bolide sources. This first effort involves entry modeling of bolide sources that have available satellite data through procedures developed in ReVelle (Earth Moon Planets 95, 441–476, 2004a; in: A. Milani, G. Valsecchi, D. Vokrouhlicky (eds) NEO Fireball Diversity: Energetics-based Entry Modeling and Analysis Techniques, Near-earth Objects: Our Celestial Neighbors (IAU S236), 2007b). Results from the entry modeling are directly coupled to AGW production through line source blast wave theory for the initial wave amplitude and period at (at 10 blast wave radii and perpendicular to the trajectory). The second effort involves the prediction of the formation and or dominance of the propagation of the atmospheric Lamb, edge-wave composite mode in a viscous fluid (Pierce, J. Acoust. Soc. Amer. 35, 1798–1807, 1963) as a function of the source energy, horizontal range and source altitude using the Lamb wave frequency that was deduced directly during the entry modeling and that is used as a surrogate for the source energy. We have also determined that Lamb wave production by bolides at close range decreases dramatically as either the source energy decreases or the source altitude increases. Finally using procedures in Gill (Atmospheric-Ocean Dynamics, 1982) and in Tolstoy (Wave Propagation, 1973), we have analyzed two simple dispersion relationships and have calculated the expected dispersion for the Lamb edge-wave mode and for the excited, propagating internal acoustic waves. Finally, we have used the above formalism to fully evaluate these techniques for four large bolides, namely: the Tunguska bolide of June 30, 1908; the Revelstoke bolide of March 31, 1965; the Crete bolide of June 6, 2002 and the Antarctic bolide of September 3, 2004. Due to page limitations, we will only present results in detail for the Revelstoke bolide.     

The DynaMICCS perspective

The DynaMICCS mission is designed to probe and understand the dynamics of crucial regions of the Sun that determine solar variability, including the previously unexplored inner core, the radiative/convective zone interface layers, the photosphere/chromosphere layers and the low corona. The mission delivers data and knowledge that no other known mission provides for understanding space weather and space climate and for advancing stellar physics (internal dynamics) and fundamental physics (neutrino properties, atomic physics, gravitational moments...). The science objectives are achieved using Doppler and magnetic measurements of the solar surface, helioseismic and coronographic measurements, solar irradiance at different wavelengths and in-situ measurements of plasma/energetic particles/magnetic fields. The DynaMICCS payload uses an original concept studied by Thalès Alenia Space in the framework of the CNES call for formation flying missions: an external occultation of the solar light is obtained by putting an occulter spacecraft 150 m (or more) in front of a second spacecraft. The occulter spacecraft, a LEO platform of the mini sat class, e.g. PROTEUS, type carries the helioseismic and irradiance instruments and the formation flying technologies. The latter spacecraft of the same type carries a visible and infrared coronagraph for a unique observation of the solar corona and instrumentation for the study of the solar wind and imagers. This mission must guarantee long (one 11-year solar cycle) and continuous observations (duty cycle > 94%) of signals that can be very weak (the gravity mode detection supposes the measurement of velocity smaller than 1 mm/s). This assumes no interruption in observation and very stable thermal conditions. The preferred orbit therefore is the L1 orbit, which fits these requirements very well and is also an attractive environment for the spacecraft due to its low radiation and low perturbation (solar pressure) environment. This mission is secured by instrumental R and D activities during the present and coming years. Some prototypes of different instruments are already built (GOLFNG, SDM) and the performances will be checked before launch on the ground or in space through planned missions of CNES and PROBA ESA missions (PICARD, LYRA, maybe ASPIICS).     

Properties of star formation in the spiral arms of barred galaxies

It is assumed that the two-fold disc-wide symmetry of spirals is caused by density waves, but also the potential of a bar component may have a significant influence on structural properties. The strength of the bar component appears to be anti-correlated with the degree of symmetry of star-forming regions in the spiral arms (Rozas et al., 1998). We present new results of R and Hα surface photometry of a sample of bright barred spirals. A photometric decompositon of the galaxy components is carried out in order to make a more accurate measurement of the strength of the bar and its interrelation to gas and stars in the disc. This revised version was published online in August 2006 with corrections to the Cover Date.     

From Local Star Formation to Global Star Formation

In this brief report we summarise the most important points raised in the course of a two-hour evening discussion session on the above topic, organised by the author. Major questions that were debated included the universality of the IMF, the history of the star formation rate in the solar neighorhood, the star formation efficiency in molecular clouds, and the role of triggered star formation. The issue of a threshold gas surface density for star formation to occur was also critically discussed. This revised version was published online in September 2006 with corrections to the Cover Date.     

喀左盆地九佛堂组露头高分辨率层序地层划分

在实测106 km剖面和对喀左盆地九佛堂组沉积特征及演化进行详细研究的基础上,依据相序关系,并结合碳酸钙、油页岩的成因意义,将九佛堂组划分了 1个长期基准面旋回和7个中期基准面旋回。在长期基准面旋回内,上升期的中期基准面旋回发育以上升半旋回为主的不完全对称型中期基准面旋回,上升与下降过渡期的中期基准面旋回,则发育近完全对称的中期基准面旋回,下降期的中期基准面旋回,则发育以下降半旋回为主的不完全对称型中期基准面旋回。经过对中期基准面旋回和短期基准面旋回发育特点和形成原因的详细研究,对代表剖面进行了中期基准面旋回对比。     

惠民凹陷大芦家地区馆陶组三段沉积微相类型及空间展布

针对惠民凹陷大芦家地区各断块地层单元划分不一致,沉积相认识存在分歧等问题,依据旋回级次、旋回性质等,将馆陶组三段划分出2个四级旋回、4个五级旋回、16个六级旋回;并以岩芯及室内分析资料、测井资料等为主要依据,综合分析岩石类型、粒度及结构特征、垂向粒序变化、层理构造类型及自然电位曲线形态等。结果表明:惠民凹陷大芦家地区馆陶组三段主要发育冲积扇及辫状河;冲积扇主要发育辫流砂岛、辫流沟道、辫流带、漫流席状砂、远端砂丘等微相;辫状河主要发育心滩,辫状河道充填,天然堤、漫滩和道间洼地沉积,泛滥平原沉积,废弃河道等微相;2个四级旋回的沉积相类型及空间展布特征相似;第Ⅰ五级旋回在研究区中偏西部属冲积扇沉积,主要发育辫流砂岛、辫流沟道、辫流带微相,在东部属扇前平原沉积;第Ⅱ五级旋回早期以辫状河沉积为主,河道规模较大,仅在第Ⅱ1六级旋回的东北部位见冲积扇的辫流砂岛及辫流沟道微相;第Ⅱ五级旋回中期属辫状河沉积,河道规模减小,2个河道群自NW向SE方向流动;第Ⅱ五级旋回晚期河道规模更小,逐渐向曲流河沉积过渡。     

新疆巴楚中—晚奥陶世牙形刺生物地层和沉积环境研究

塔里木盆地中央隆起区的中—上奥陶统灰岩相地层露头分布在巴楚良里塔格地区的一间房—唐王城。以牙形刺动物群为依据厘定3个组的时代,从下至上为一间房组(Periodus flabellum层、Pygodus serra层,属达瑞威尔阶)、吐木休克组(Pygodus anserinus层、Baltoniodus alobatus带,属桑比阶)和良里塔格组(含B.confluens动物群层,属凯迪阶下部)。一间房组的开始标志了新一期的海进,此组下段发育1期藻丘,中段发育1期藻丘、1期瓶筐石礁丘和3—4期瓶筐石—棘屑滩,上段代表了海水加深至浪基面之下的过程;吐木休克组沉积过程中达到了海进最大值,为凝缩沉积;良里塔格组代表了逐渐海退的过程,由浅滩和3期藻丘建造组成。