Geologic Formations on which and with which Indiana's Roads are Built

Indiana Geological Survey Circular 1This publication could also be titled “Sources of aggregates and types of highway subgrades in Indiana.” Our highways are built of aggregates cemented together with one kind or another of portland cement, bituminous materials, or resinous plastics. Often engineers want to know more about the origin, extent, and mineral composition of gravels and limestones used as aggregate. Because engineers don't have this information, they experience financial loss and frustration until they find the answers. The engineers of the Highway Commission, likewise, know better than anyone else in Indiana the various types of subgrades and the characteristic behavior of each type of aggregate on which our roads are built. But the engineers would like also to know m uch more about the origin, thickness, lateral extent, mineral composition, and interrelationships of the wide variety of subgrades encountered in our highway system. To answer questions of this kind, engineers and aggregate producers, in this country and abroad, are turning increasingly to geology and mineralogy, because these sciences are proving to be the most economical and dependable methods of finding new deposits and of indicating the type and size of subgrades (terranes) that will be encountered by new highways that will cross untested areas. The greatly increased use of aggregates during the past 10 years is being intensified by the demand for aggregates to build the modern heavy duty roads of this decade. These demands already are beginning to exhaust some of our present deposits. New sources of aggregates, favorably located along the proposed routes of such new superhighways, will be expensive to find and to evaluate. Since July 1947, the Indiana Geological Survey (Patton, 1949, pp. 1-47) has studied, sampled, and mapped every operating limestone quarry in Indiana (Pl. l), and also has examined nearly 3,100 gravel pits, including the 620 that are currently operating. In addition, the Geological Survey has analyzed each type of limestone encountered in quarries, and has collected information about the composition of Indiana’s gravels and sands. This publication discusses the geology, distribution and accessibility of Indiana limestones and gravels, and also to indicate the differences in origin of the materials that make up the several kinds of subgrades which support our roads.Indiana Department of Conservatio

Turbulent Mixing in Clusters of Galaxies

We present a spherically-symmetric, steady-state model of galaxy clusters in which radiative cooling from the hot gas is balanced by heat transport through turbulent mixing. We assume that the gas is in hydrostatic equilibrium, and describe the turbulent heat diffusion by means of a mixing length prescription with a dimensionless parameter alpha_mix. Models with alpha_mix ~ 0.01-0.03 yield reasonably good fits to the observed density and temperature profiles of cooling core clusters. Making the strong simplification that alpha_mix is time-independent and that it is roughly the same in all clusters, the model reproduces remarkably well the observed scalings of X-ray luminosity, gas mass fraction and entropy with temperature. The break in the scaling relations at kT \~ 1-2 keV is explained by the break in the cooling function at around this temperature, and the entropy floor observed in galaxy groups is reproduced naturally.Comment: Accepted for publication in ApJ

Non-Thermal Emission from Relativistic Electrons in Clusters of Galaxies: A Merger Shock Acceleration Model

We have investigated evolution of non-thermal emission from relativistic electrons accelerated at around the shock fronts during merger of clusters of galaxies. We estimate synchrotron radio emission and inverse Compton scattering of cosmic microwave background photons from extreme ultraviolet (EUV) to hard X-ray range. The hard X-ray emission is most luminous in the later stage of merger. Both hard X-ray and radio emissions are luminous only while signatures of merging events are clearly seen in thermal intracluster medium (ICM). On the other hand, EUV radiation is still luminous after the system has relaxed. Propagation of shock waves and bulk-flow motion of ICM play crucial roles to extend radio halos. In the contracting phase, radio halos are located at the hot region of ICM, or between two substructures. In the expanding phase, on the other hand, radio halos are located between two ICM hot regions and shows rather diffuse distribution.Comment: 19 pages, 5 figures, accepted for publication in Ap

A Description and Stratigraphic Correlation of the Fenestellidae from the Devonian of Michigan

233-275http://deepblue.lib.umich.edu/bitstream/2027.42/48193/2/ID030.pd

Optical-fiber-microsphere for remote fluorescence correlation spectroscopy

International audienceFluorescence correlation spectroscopy (FCS) is a versatile method that would greatly benefit to remote optical-fiber fluorescence sensors. However, the current state-of-the-art struggles with high background and low detection sensitivities that prevent the extension of fiber-based FCS down to the single-molecule level. Here we report the use of an optical fiber combined with a latex microsphere to perform FCS analysis. The sensitivity of the technique is demonstrated at the single molecule level thanks to a photonic nanojet effect. This offers new opportunities for reducing the bulky microscope setup and extending FCS to remote or in vivo applications

The Energy Spectrum of Primary Cosmic Ray Electrons in Clusters of Galaxies and Inverse Compton Emission

Models for the evolution of the integrated energy spectrum of primary cosmic ray electrons in clusters of galaxies have been calculated, including the effects of losses due to inverse Compton (IC), synchrotron, and bremsstrahlung emission, and Coulomb losses to the intracluster medium (ICM). The combined time scale for these losses reaches a maximum of ~3e9 yr for electrons with a Lorentz factor ~300. Only clusters in which there has been a substantial injection of relativistic electrons since z <~ 1 will have any significant population of primary cosmic ray electrons at present. In typical models, there is a broad peak in the electron energy distribution extending to gamma~300, and a steep drop in the electron population beyond this. In clusters with current particle injection, there is a power-law tail of higher energy electrons with an abundance determined by the current rate of injection. A significant population of electrons with gamma~300, associated with the peak in the particle loss time, is a generic feature of the models. The IC and synchrotron emission from these models was calculated. In the models, EUV and soft X-ray emission are nearly ubiquitous. This emission is produced by electrons with gamma~300. The spectra are predicted to drop rapidly in going from the EUV to the X-ray band. The IC emission also extends down the UV, optical, and IR bands with a fairly flat spectrum. Hard X-ray (HXR) and diffuse radio emission due to high energy electrons (gamma~10e4) is present only in clusters which have current particle acceleration. Assuming that the electrons are accelerated in ICM shocks, one would only expect diffuse HXR/radio emission in clusters which are currently undergoing a large merger.Comment: Accepted for publication in the Astrophysical Journal, with minor revisons to wording for clarity and one additional reference. 19 pages with 16 embedded Postscript figures in emulateapj.sty. Abbreviated abstract belo

Off-Center Mergers of Clusters of Galaxies and Nonequipartition of Electrons and Ions in Intracluster Medium

We investigate the dynamical evolution of clusters of galaxies and their observational consequences during off-center mergers, explicitly considering the relaxation process between ions and electrons in intracluster medium by N-body and hydrodynamical simulations. In the contracting phase a bow shock is formed between the two subclusters. The observed temperature between two peaks in this phase depends on the viewing angle even if the geometry of the system seems to be very simple like head-on collisions. Around the most contracting epoch, when we observe merging clusters nearly along the collision axis, they look like spherical relaxed clusters with large temperature gradients. In the expanding phase, spiral bow shocks occur. As in head-on mergers, the electron temperature is significantly lower than the plasma mean one especially in the post-shock regions in the expanding phase. When the systems have relatively large angular momentum, double-peak structures in the X-ray images can survive even after the most contracting epoch. Morphological features in both X-ray images and electron temperature distribution characteristic to off-center mergers are seriously affected by the viewing angle. When the clusters are observed nearly along the collision axis, the distribution of galaxies' line-of-sight (LOS) velocities is a good indicator of mergers. In the contracting phase, an negative kurtosis and a large skewness are expected for nearly equal mass collisions and rather different mass ones, respectively. To obtain statistically significant results, about 1000 galaxies' LOS velocities are required. For nearby clusters ($z<0.05$), large redshift surveys such as 2dF will enable us to study merger dynamics.Comment: 21 pages, 7 figures. Accepted for publication in Ap

A Comparison of Radio and X-Ray Morphologies of Four Clusters of Galaxies Containing Radio Halos

Clusters of galaxies may contain cluster-wide, centrally located, diffuse radio sources, called halos. They have been found to show morphologies similar to those of the X-ray emission. To quantify this qualitative statement we performed a point-to-point comparison of the radio and the X-ray emission for four clusters of galaxies containing radio halos: Coma, Abell 2255, Abell 2319, Abell 2744. Our study leads to a linear relation between the radio and the X-ray surface brightness in two clusters, namely Abell 2255 and Abell 2744. In Coma and A2319 the radio and the X-ray brightnesses seem to be related with a sub-linear power law. Implications of these findings within simple radio halo formation models are briefly discussed.Comment: 9 pages, 13 .ps figures, accepted by A&

Oat growth under different nitrogen doses in an eucalyptus alley cropping system in subtropical Brazil.

Foi realizada uma análise de crescimento para verificar como a aveia (Avena sativa L. cv. IPR 126) cultivada para grãos responde a um sistema agroflorestal (SAF) com eucaliptos (Eucalyptus dunnii Maiden) no subtrópico brasileiro. A hipótese deste trabalho é que a resposta de crescimento da aveia não é modificada pelo nitrogênio em distâncias relativas a faixas de eucaliptos. O objetivo deste estudo foi determinar como o crescimento da aveia é influenciado por níveis de nitrogênio (12 e 80 kg ha-1 de N) em cinco posições equidistantes entre faixas de linhas duplas de eucaliptos [20 m (4 m x 3 m)] em SAF e em agricultura tradicional de plantio direto. O experimento foi em faixas no delineamento de blocos ao acaso com quatro repetições. Foram avaliadas as taxas de crescimento relativo e de assimilação líquida, fração de massa foliar e taxa de enchimento relativo da panícula. O nitrogênio alterou a resposta do crescimento diferentemente em posições relativas às faixas de árvores, portanto diferentes doses de nitrogênio devem ser utilizadas nestas posições para aumentar o crescimento da aveia