Petrology and Geochemistry of Post-Collisional Early Miocene Volcanism in the Karacada? Area (Central Anatolia, Turkey)

Early Miocene (ca.?21–18 Ma) volcanism in the Karacada? area comprises three groups of volcanic rocks: (1) calcalkaline suite (andesitic to rhyolitic lavas and their pyroclastics), (2) mildly-alkaline suite (alkali basalt, hawaiite, mugearite, benmoreite and trachydacite), and (3) a single trachyandesitic flow unit. Field observations, 40Ar/39Ar ages and geochemical data show that there was a progressive temporal transition from group 1 to 3 in a post-collisional tectonic setting. The calcalkaline suite rocks with medium-K in composition resemble those of subduction-related lavas, whereas the mildly-alkaline suite rocks having a sodic tendency (Na2O/K2O=1.5–3.2) resemble those of within-plate lavas. Incompatible element and Sr-Nd isotopic characteristics of the suites suggest that the lithospheric mantle beneath the Karacada? area was heterogeneously enriched by two processes before collision: (1) enrichment by subduction-related processes, which is important in the genesis of the calcalkaline volcanism, (2) enrichment by small degree melts from the astenosphere, which dominates the mildly alkaline volcanism. Perturbation of the enriched lithosphere by either delamination following collision and uplift or removal of the subducted slab following subduction and collision (i.e., slab breakoff) is the likely mechanism for the initiation of the post-collision volcanism.     

3rd International Conference on Unsaturated Soils (UNSAT 2002) Recife, Brazil, 10–12 March 2002

Conference Report

3rd International Conference on Unsaturated Soils (UNSAT 2002) Recife, Brazil, 10–12 March 2002     

A chemostratigraphic method to determine the end of impact‐related sedimentation at marine‐target impact craters (Chesapeake Bay,Lockne, Tvären)

Abstract– To better understand the impact cratering process and its environmental consequences at the local to global scale, it is important to know when in the geological record of an impact crater the impact‐related processes cease. In many instances, this occurs with the end of early crater modification, leaving an obvious sedimentological boundary between impactites and secular sediments. However, in marine‐target craters the transition from early crater collapse (i.e., water resurge) to postimpact sedimentation can appear gradual. With the a priori assumption that the reworked target materials of the resurge deposits have a different chemical composition to the secular sediments we use chemostratigraphy (δ¹³C_carb, %C_org, major elements) of sediments from the Chesapeake Bay, Lockne, and Tvären craters, to define this boundary. We show that the end of impact‐related sedimentation in these cases is fairly rapid, and does not necessarily coincide with a visual boundary (e.g., grain size shift). Therefore, in some cases, the boundary is more precisely determined by chemostratigraphy, especially carbonate carbon isotope variations, rather than by visual inspection. It is also shown how chemostratigraphy can confirm the age of marine‐target craters that were previously determined by biostratigraphy; by comparing postimpact carbon isotope trends with established regional trends.     

THE SOLAR Mg II h AND k LINES – Observations and Radiative Transfer Modeling

This paper presents observations of the MgII h and k lines obtained with the UVSP instrument that flew aboard the SMM satellite. Both spatially averaged and resolved observations are compared with calculated profiles of the lines from standard, plane-parallel solar models. The radiative transfer calculations presented take full account of partial frequency redistribution and wavelength overlap of the h and k lines. A comparison between theoretical and observed wing profiles indicates that current one-dimensional models underestimate the temperature in the middle photosphere. The cores of spatially resolved dark intra-network profiles are well reproduced by the model calculations, while the spatially averaged profiles have in general broader emission peaks, indicating that the additional broadening is due to a contribution of magnetic network profiles.     

Constraint on Parameters of Inverse Compton Scattering Model for PSR B2319+60

Using the multifrequency radio profiles of pulsar PSR B2319+60, two parameters of inverse Compton scattering model, the initial Lorentz factor and the factor of energy loss of relativistic particles are constrained.     

Uv Line Profiles of Biv from a 10-Ps Krf-Laser-Produced Plasma

We use a KrF laser that generates pulses up to 8 × 10¹⁴ watt/cm² when focused onto a boron nitride target. We measured the line profile of the near UV, n = 0, n = 2 transitions of helium-like boron and we studied the triplet 1s2p³P-1s2s³S at 2825.85 (J = 1), 2821.68 (J = 2) and 2824.57 (J = 0) Å, at various positions from the target surface, in order to correlate details of this profile with the presence of self-generated magnetic fields and/or dynamic turbulence among other processes. We fitted the measured profiles to a 0-D model, that includes, Stark, Doppler, Zeeman and instrumental broadening. The effect of the magnetic field was included using an intermediate field calculations. Preliminary results of these measurements are presented and discussed.     

碧口群火山岩的时代——SHRIMP锆石U—Pb测年结果

碧口群火山岩系是从原碧口系(叶连俊等,1944,后称碧口群)中解体出来的一个岩石单元(陶洪祥等,1993)。虽经过近60年的研究,但对某些关键问题,特别是碧口群火山岩系的时代,仍存在不同认识。在早期研究阶段(20世纪40～50年代)和60～70年代的区域地质调查工作中,碧口群和横丹群被视做一个整体,并通过地层层序关系探讨其时代。如,叶连俊等(1944)提出碧口系形成于志留—泥盆纪,黄振辉(1959)则认为碧口群属寒武—志留系。80年代以来对碧口群火山岩系进行的同位素年代学和地古生物学研究给出了从新元古代(赵祥生等,1990;胡正东,1990;李耀敏,1991;秦…     

Arm and Interarm Star Formation in Spiral Galaxies

We present an outline of our study of the effects of star formation on the different components of the interstellar medium in the discs of spiral galaxies, both globally and as a function of arm and interarm environment. We are in the process of obtaining images of 57 spiral galaxies at low inclinations, and analysing them to study the distribution of recent massive star formation, old stars, young stars, gas and dust. We will dissect the images into arm and interarm regions and compare and contrast the morphology and scale lengths within these regions inH_α, HI, the near infrared, optical and (where available) CO. Modelling will show how the scale lengths are affected by star formation, how this differs between arms and interarms, and whether the Schmidt Law varies from the global values in the arm and interarm regions. This revised version was published online in July 2006 with corrections to the Cover Date.