DOCSLIB.ORG

A Abiogenesis, 340, 341 Absorption Lines, 7, 38 Accretion, 10, 29, 55, 58

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
A Abiogenesis, 340, 341 Absorption Lines, 7, 38 Accretion, 10, 29, 55, 58 Index A Atmosphere, 8, 13, 45, 46, 72, 73, 173–179, Abiogenesis, 340, 341 182, 187, 201, 202, 234, 271, 322, Absorption lines, 7, 38 324–328, 343, 344, 348 Accretion, 10, 29, 55, 58, 63, 95, 96, 178, 204, A-type, supergiant, 25 205, 331, 347 Auger, 14, 48–51, 70–73 Aether, 287 Australia, 37, 118, 127, 146, 152, 206, 348 Afterglow, 37, 61, 197 Axion, 9, 11, 79, 80, 82 AGASA. See Akeno Giant Air Shower Array Ayers Rock, 266 (AGASA) Airbus, 133 Air-showers, 45, 62, 70, 72, 73 B Akeno Giant Air Shower Array (AGASA), 14, Baade-Wesselink, method, 38 70, 71 Babcock, Horace, 128 Alchemist, 290 Balloon, 45, 143, 146, 148, 152, 178, 270, 324 Almagest, 303 Barnes, Julian, 268 Alpha Magnetic Spectrometer (AMS), 14, 146 Baryonic Acoustic Oscillations (BAO), 32, Aluminium, 178, 346, 347 36–37 American Museum of Natural History Becquerel, Paul, 341 (AMNH), 260, 262, 263, 265, 266 Belgium, 132 Andromeda, 23, 24, 29, 95 Bell, Jocelyn, 10 Anisotropy, 14, 15, 50–52, 54, 62, 64, 71, 80 Bell Telephone Laboratories, 126, 127, 130 Ankle, 44 BeppoSax, 37 Antimatter, 13, 14 Bernal, J. D., 343 Apollo program, 176, 322, 344 Beta decay, 17 Arc, gravitational, 271–274 Bethe, Hans, 8 Arcsecond, 174, 213 Big Bang, 6, 8, 11, 24, 30, 32, 98, 148, 164, Aristotle, 287 313, 314 Arrhenius, Svante, 341 Binary, 11, 15, 17, 28, 34, 87, 88, 90–97, 101, Asteroid, 113, 126, 175, 176, 182, 264, 335 194, 200, 202, 203, 206, 207 Astrobiology, 154, 328, 338, 340, 344 Bioastronomy, 338, 344 Astrochemistry, 154 Black hole, 12–13, 15, 17, 29, 58, 63, 90–97, Astrologer, 124, 289, 291–293, 296–299, 302, 101, 153, 164, 177, 178, 180, 234, 265, 304, 305 275, 277, 318 Astrology, 285–305 Bohr, Niels, 17 ASTRONET, 16, 134, 160–172, 246 Boksenberg, Alec, 271 Astrophysical Journal, 140, 262 Bolometer, 130 ATLAS detector, 6 Bonaparte, Napoleon, 288 J.-P. Lasota (ed.), Astronomy at the Frontiers of Science, Integrated Science 351 & Technology Program 1, DOI 10.1007/978-94-007-1658-2, © Springer Science+Business Media B.V. 2011 352 Index Brahe, Tycho, 28, 113, 170, 290 Dauvillier, A., 343 Brane, 98, 275 DAWN, 175, 179 Broadway, 261 δ Cephei, 26 Bruno, Giordano, 286, 290 Decadal survey, 16, 164, 170–172 B-type, supergiant, 25 Degeneracy, 10 Density, critical, 30 de Sitter, space-time, 311 C Detector, 6, 8, 14, 15, 22, 30, 46, 47, 56–57, Cabbala, 289, 290 59, 61, 64, 88, 89, 96, 128, 130, 177, Camera, 22, 130, 131, 142, 175, 193, 194, 184, 185 196–198, 200, 205–207, 220, 224, 225, Detonation, 34, 35 270–272, 333 2dF survey, 32 Canada-France-Hawaii Telescope (CFHT), Diffraction, 174, 213, 214, 237, 270 149, 155, 271, 272 Dirac, Paul A.M., 310 Capek, Karl, 290 Disk, accretion, 55, 63, 95, 96 Cardinal points, 293, 294, 298 Disk, galactic, 200 Caribbean, 125 Distance, 15, 21–39, 48, 50–54, 63, 73, 76, Cartography, 112, 125 80, 89, 96, 97, 101, 125, 184, 185, 195, Cassiopea, constellation, 28 202, 203, 207, 218, 219, 272, 303, 310, CCD. See Charge Coupled Device (CCD) 326, 331, 334 CEA, 130, 131, 271 Divination, 289, 292 Cepheid variable, 26 Dolfuss, Audoin, 270 CERN, 5, 6, 18, 73, 81, 134, 162, 266 Dust, 27, 36, 165, 176, 177, 322, 324, 331, Charge Coupled Device (CCD), 22, 30, 130, 333, 335 192, 193, 196–198, 200, 205, 206, 211, Dwarf white, 10, 28, 29, 34, 35 212, 225, 271, 272 China, 125, 178 CNES, 174, 179, 186, 270 Cobalt, 178 E Cobe satellite, 32 Easter Island, 266 Coleman-de Lucia tunneling, 315 Eclipse, 198, 200, 270 Colour, 30, 31, 36, 252, 254, 327 Ecliptic, 293, 294, 297 Combes, Michel, 270 E-ELT, European Extremely Large Telescope Comet, 117, 175, 176, 179, 186, 324, 332–336 (E–ELT) Committee on Space Research (COSPAR), 174 Effelsberg, 127, 153 Constant, cosmological, 32, 277, 315 Einstein, Albert, 32, 87, 265, 290 Constantine the Great, 289 Electron, 10, 29, 34, 39 Copernicus, Nicolaus, 286 Electronographic camera, 270, 271 Corona, 270 Emission lines, 36, 37, 128, 270 COROT, 174, 179, 202, 205 Energy dark, 6, 30–32, 164, 180, 186, 264, Correction, bolometric, 49, 56 273, 275, 287 Cosmic Microwave Background (CMB), 4, 13, Equivalence principle, 61, 89, 174 16, 27, 32, 48, 49, 57, 73, 78, 80, 98 Eros, 175, 192, 298 Cosmic ray, 13–15, 43–64, 70, 73, 82 ESA. See European Space Agency (ESA) COSPAR. See Committee on Space Research EUCLID, 33, 156, 180 (COSPAR) Europa, 181, 183, 184, 327, 328, 335, 336 Curator, 260, 261, 263, 266 European Extremely Large Telescope (E-ELT), Curve, rotation, 27 6, 146, 156, 171, 214, 222, 236, 237, Cycle, magnetic, 177 240, 241 European Space Agency (ESA), 4, 131–134, 139, 144, 146, 151, 155, 156, 160, 162, D 166, 172, 174, 175, 177–187, 326, 328, Danish Telescope, 1.5m, 30 333, 336 Darwin, George, 340, 341 Ewen, Harold, 127 Index 353 Expanding Photosphere, method, 38 Greisen-Zatsepin-Kuzmin (GZK), 14, 44, 48, Explorer 11, 178 49, 54–58, 64, 71–74, 78 Group, Local, 24 GZK. See Greisen-Zatsepin-Kuzmin (GZK) F Felenbok, Paul, 270 Fermi acceleration, 13 H Fermi Gamma-ray Space Telescope, 17 Haeckel, Ernst, 341 Fireball, 59–60 Haldane, J.B.S., 341, 342 Flamsteed, John, 302–304 Hanks, Tom, 262 Fluence, 55 Hayabusa, 176 Ford, Harrison, 262 Heliophysics, 177, 179, 183 Ford T, 126 Helioseismology, 177 France, 110, 113, 114, 118, 125, 128–130, 132, Heliosphere, 174, 177 155, 160, 168, 178, 179, 185 Helium, 7, 8, 14, 26, 27, 35, 132, 187, 331 Freedman, Wendy, 27 Heresy, 287 Fusion, 7–10, 146 Herschel Space Observatory, 130 Herzsprung-Russel, diagram, 347 HESS, 72, 74, 153 G Hess Victor, 13 Galactic Centre, 12, 17 Hewish, A., 10 Galaxy, 12–14, 22, 23, 27–29, 31, 35, 37, Higgs boson, 5, 18 50, 51, 72, 74–76, 81, 95, 96, 139, Hilbert, David, 315 177–179, 195, 203, 210, 250, 251, 253, Himalaya mountains, 309 257, 272–274, 297 Hoerner, Sebastian von, 127 Galaxy, elliptical, 28, 35, 36, 72, 180, 184, Horizon, 12, 13, 37, 55, 92, 93, 125, 277, 231, 257, 271 293–295, 300, 314, 315 Galaxy, spiral, 22, 23, 28, 36, 257 Horoscope, 290, 292, 293, 297–302, 304, 305 Galilei, Galileo, 125, 154, 230, 286, 291, 324, House, 127, 175, 212, 263, 290, 293, 295, 298, 328 299, 301, 302 Gamma ray, 14, 73, 78, 81, 148, 178, 179, 197, Hoyle, Fred, 8 198 Hubble, Edwin, 24, 210 Gamma ray burst (GRB), 13, 17, 36–38, 55, Hubble parameter, 17, 101 69, 72, 95, 178, 179, 197 Hubble Space Telescope (HST), 23, 24, 26, 27, Gas, 6, 7, 12, 56, 155, 165, 177, 178, 182, 274, 130, 143, 148, 152, 174, 178, 179, 187, 331 203, 212, 271, 273 Gemini, telescope, 30, 145, 153, 154, 213, 214, Hulst, Henk Van de, 127 216, 234, 296, 299 Huxley, Thomas, 341 Genesis, 176, 265, 269 Huygens, Christiaan, 125, 176, 186 Geobiology, 176 Huygens probe, 328, 344 Geodesy, 110, 112, 119, 125 Hydrocarbon, 176, 328 Geomagnetic field, 118, 176 Hypatia of Alexandria, 289 Geoscience, 176 Germs, 341 Giant planet, 331 I Giants, 25, 191, 332 ICECUBE, 15, 57–59 Giraffes, 310 Image, 15, 112, 117, 128, 129, 133, 134, 142, Goldberg, Whoopi, 262 178, 192, 202, 212, 218–220, 230–232, Grand Tour, 175 234, 235, 248–250, 254, 272, 273, 278, Gravity, 4–5, 7, 10, 11, 15, 17, 25, 30, 32, 34, 286, 317, 323, 329, 330, 333 37, 61, 70, 77, 78, 101, 127, 147, 177, Imagery, 27, 176, 262, 271 212, 216, 231, 233, 238, 274, 275, 277, Imaging, medical, 130, 271 291, 326, 331 India, 125, 178 Greenwich, 110–114, 117, 118, 125 Indonesia, 125 354 Index Infinity, 315, 316 Large Magellanic Cloud (LMC), 23, 192 Inflation, 16, 98, 316 Laser, 15, 88, 89, 99, 128, 129, 181, 214, 233, Infrared (IR), 13, 73, 78, 81, 129, 130, 132, 303 142, 144, 148, 152, 154, 162, 166, 174, Laser Interferometer Gravitational wave 177–179, 184, 186, 187, 201, 252, 324, Observatory (LIGO), 15, 88, 89, 93, 95, 332, 333 97–101, 276 In-situ, 174, 176, 182, 239, 322, 327, 335, 336 Laser-interferometer space antenna (LISA), Institute for Radio Astronomy at Millimeter 15, 88, 146, 150, 151, 153, 156, 180, wavelengths (IRAM), 127, 128, 131, 181, 275 153 La Silla, Chile, 30, 191, 232 Interferometer, 15, 88, 89, 99, 100, 128, 133, Launch, 14, 126, 132, 146, 147, 152, 178, 144, 145, 181, 184, 218, 275 180–182, 184, 185, 187, 328 Interferometry, 126, 127, 145, 146, 148, 185 Laws, 4, 5, 7, 16, 81, 180, 234, 269, 275, 286, Ireland, 128, 168 288, 291, 292, 309–316, 342, 345 Iron, 7, 46, 73, 74, 76, 178 Lense, 230 Isotopes, 33–35, 178, 183 Lensing, 5, 27, 192, 273, 274 Lequeux, James, 123–135 LETI, 130, 131 J Le Verrier, Urbain, 117, 126 Jansky, Karl, 126, 127 LHC. See Large Hadron Collider (LHC) Japan, 144–146, 178, 179 Light, speed of, 17, 22, 63, 77, 90, 91, 310 Jet, 61, 63, 72, 131 LIGO. See Laser Interferometer Gravitational John Paul II, 289 wave Observatory (LIGO) Jupiter, 111, 124, 125, 137, 175, 183, 186, 198, Loew, Judah, 290 199, 203, 206, 207, 235, 264, 287, 296, Logic, 172, 268, 269, 277, 297, 315–316 298–301, 326–332, 335 Longitude, 118, 125, 297 Lorentz, invariance, 14, 17, 61, 77–79 LSST, 33, 139, 146, 150, 151, 225, 244 K Luminosity, 8, 22, 24–33, 35–39, 54, 55, 64, Kafka, Franz, 290 71, 72, 76, 82, 89, 90, 96, 101, 195, 200 Kaon, 59, 61 Lunar, 114, 179, 292, 297, 322, 335, 348 Keck, telescope, 30, 143, 210, 216, 223, 234, Lyot, Bernard, 270 237, 239 Kelvin, Lord (William Thomson), 174, 341 Kepler, Johannes, 179, 202, 205, 208, 286–295, M 297–303, 305 Mach, Ernst, 310 Kiepenheuer, Karl Otto, 127 Machu Picchu, 266 Knee, 44 Madagascar, 125 Kodak, 129 Magnetars, 10 Kudritzki, R.-P., 25 Magnetosphere, 174, 177, 335 Maillet, Benoit de, 340 Mandatory program (ESA), 175 L Manhattan Project, 265 Laboratory, 3–18, 70, 73, 111, 114, 128, 131, Mapping, 40, 273, 324 163, 165, 166, 171, 174, 182, 183, Mariner 2, 176 269–271, 335, 336 Marlowe, Christopher, 290 Lagrange, Joseph-Louis, 288 Mars,
Load more

Recommended publications
  • Intelligent Design, Abiogenesis, and Learning from History: Dennis R
    Author Exchange Intelligent Design, Abiogenesis, and Learning from History: Dennis R. Venema A Reply to Meyer Dennis R. Venema Weizsäcker’s book The World View of Physics is still keeping me very busy. It has again brought home to me quite clearly how wrong it is to use God as a stop-gap for the incompleteness of our knowledge. If in fact the frontiers of knowledge are being pushed back (and that is bound to be the case), then God is being pushed back with them, and is therefore continually in retreat. We are to find God in what we know, not in what we don’t know; God wants us to realize his presence, not in unsolved problems but in those that are solved. Dietrich Bonhoeffer1 am thankful for this opportunity to nature, is the result of intelligence. More- reply to Stephen Meyer’s criticisms over, this assertion is proffered as the I 2 of my review of his book Signature logical basis for inferring design for the in the Cell (hereafter Signature). Meyer’s origin of biological information: if infor- critiques of my review fall into two gen- mation only ever arises from intelli- eral categories. First, he claims I mistook gence, then the mere presence of Signature for an argument against bio- information demonstrates design. A few logical evolution, rendering several of examples from Signature make the point my arguments superfluous. Secondly, easily: Meyer asserts that I have failed to refute … historical scientists can show that his thesis by not providing a “causally a presently acting cause must have adequate alternative explanation” for the been present in the past because the origin of life in that the few relevant cri- proposed candidate is the only known tiques I do provide are “deeply flawed.” cause of the effect in question.
    [Show full text]
  • GTL PI Meeting 2003 Presentation Nealson
    USCUSC Geobiology Astrobiology Ken Nealson Wrigley Professor of Geobiology USC SHEWANELLA and Genomes to Life !! THE FUTURE!! WHERE ARE WE GOING? HOW WILL WE GET THERE? WHAT ARE THE CHALLENGES AND TRAPS? USCUSC Geobiology Astrobiology Genomes to Life: Shewanella and the future !! Genomes & Genomics: For sake of this discussion, I include Genome composition, gene expression, & metabolism Genomics Physiology Ecophsyiology Ecology Predictable Community Behavior Successful Manipulation of Natural Communities USCUSC Geobiology Astrobiology Shewanella in the future: Short Term: Genomic/Proteomic/Metabolic Connections Linkage of physiology to genomic information Mid Term: Ecophysiology Questions regarding regulation of MR-1 How does the cell”work”? Linkage of laboratory to microcosm and field data Long Term: Community structure and activities Genetic variability and use of genomic approaches Predictable community ecology The “old view” of Shewanella oneidensis Gamma Purple proteobacteria MR-1; when Isolated was One of ~10, Now >50 ! USCUSC Geobiology Astrobiology The “new view” of Shewanella Now MR-1 is again one of 1, although a strain of S. benthica is almost finished by a Japanese group (JAMSTEC) USCUSC Geobiology Astrobiology Excitement of the “new view”: May be able to use this information to dissect specific aspects of both ecology and evolution: Ecology: Involved in many different redox processes Aerobic and anaerobic niches Metal cycling connected with carbon cycling Potential for dealing with many toxic metals and radionuclides Can we understand Shewanella well enough to begin to use it? what it does how it does it how it regulates how it interacts with other organisms All of this well enough to make predictions that work.
    [Show full text]
  • The Primordial Earth: Hadean and Archean Eons
    5th International Symposium on Strong Electromagnetic Fields and Neutron Stars 10 –13 of May, 2017 -Varadero, Cuba HABITABILITY OF THE MILKY WAY REVISITED Rolando Cárdenas and Rosmery Nodarse-Zulueta e-mail: [email protected] Planetary Science Laboratory Universidad Central “Marta Abreu” de Las Villas, Santa Clara, Cuba Abstract • The discoveries of the last three decades on deep sea and deep crust of planet Earth show that life can thrive in many places where solar radiation does not reach, using chemosynthesis instead of photosynthesis for primary production. • Underground life is relatively well protected from hazardous ionizing cosmic radiation, so above mentioned discoveries reopen the habitability budget of the Milky Way, turning potentially habitable even planetary bodies without atmosphere. • Considering this, in this work the habitability potential of the Milky Way is reconsidered. Energy Sources for Primary Habitability: - Photosynthesis: Electromagnetic Waves, mostly in the range 400-700 nm. Dominant in planetary surface. - Chemosynthesis: Energy released by redox chemical reactions. Dominant in deep sea and crust. Circumstellar Habitable Zone https://en.wikipedia.org/wiki/Circumstellar_habitable_zone. Accessed on 2017.04.28 Liquid water at surface: biased towards surface (photosynthetic) life Chemosynthesis: More common than previously thought… - Any redox process giving at least 20 kJ/mol of free energy can support microbial metabolism. The following gives 794 kJ/mol: Pohlman, J.: The biogeochemistry of anchialine caves:
    [Show full text]
  • Bayesian Analysis of the Astrobiological Implications of Life's
    Bayesian analysis of the astrobiological implications of life's early emergence on Earth David S. Spiegel ∗ y, Edwin L. Turner y z ∗Institute for Advanced Study, Princeton, NJ 08540,yDept. of Astrophysical Sciences, Princeton Univ., Princeton, NJ 08544, USA, and zInstitute for the Physics and Mathematics of the Universe, The Univ. of Tokyo, Kashiwa 227-8568, Japan Submitted to Proceedings of the National Academy of Sciences of the United States of America Life arose on Earth sometime in the first few hundred million years Any inferences about the probability of life arising (given after the young planet had cooled to the point that it could support the conditions present on the early Earth) must be informed water-based organisms on its surface. The early emergence of life by how long it took for the first living creatures to evolve. By on Earth has been taken as evidence that the probability of abiogen- definition, improbable events generally happen infrequently. esis is high, if starting from young-Earth-like conditions. We revisit It follows that the duration between events provides a metric this argument quantitatively in a Bayesian statistical framework. By (however imperfect) of the probability or rate of the events. constructing a simple model of the probability of abiogenesis, we calculate a Bayesian estimate of its posterior probability, given the The time-span between when Earth achieved pre-biotic condi- data that life emerged fairly early in Earth's history and that, billions tions suitable for abiogenesis plus generally habitable climatic of years later, curious creatures noted this fact and considered its conditions [5, 6, 7] and when life first arose, therefore, seems implications.
    [Show full text]
  • Thoughts in Geobiology
    Journal of Geology and Mining Research Vol. 1(8), October, 2009 Available online http://www.academicjournals.org/jgmr ISSN 2006 – 9766 © 2009 Academic Journals Editorial Thoughts in Geobiology One of the possible ways to make connection between geologists and biologists is through studying subjects related to the newly established trend “Geobiology”. In the year 1972, Sylvester-Bradley stated that the Earth sciences include not only geology, but the hybrid-sciences geophysics, geochemistry and geobiology, of which the most complex and least rigorous is geobiology. Kump (2008) simply defined geobiology as the field that has recently energized the life and Earth sciences as geologists and biologists bring new tools to collaborations addressing fundamental problems that transcend the disciplines. The book edited by Xiao and Kaufman (2007) includes a set of multidisciplinary reviews on the Neoproterozoic fossil record (animals, algae, acritarchs, protists, and trace fossils), evolutionary developmental biology of animals, molecular clock estimates of phylogenetic divergences, and Neoproterozoic chemostratigraphy and sedimentary geology. The editors of this book believe that these topics are of continuing interest to geoscientists and bioscientists who are intrigued by the deep history of the Earth and its inhabitants. Yildirim et al. (2008) believe that microbial systems in extreme environments and in the deep biosphere may be analogous to potential life on other planetary bodies and hence may be used to investigate the possibilities of extraterrestrial life. I would add that astrobiologists are working on this point through studying materials from Mars. Through geobiology we search for origins and evolution of life, atmosphere, hydrosphere, lithosphere and biosphere, reasons of mass extinctions, interactions between microbes and minerals, global changes, and other subjects of interest.
    [Show full text]
  • SIDE GROUP ADDITION to the POLYCYCLIC AROMATIC HYDROCARBON CORONENE by PROTON IRRADIATION in COSMIC ICE ANALOGS Max P
    The Astrophysical Journal, 582:L25–L29, 2003 January 1 ᭧ 2003. The American Astronomical Society. All rights reserved. Printed in U.S.A. SIDE GROUP ADDITION TO THE POLYCYCLIC AROMATIC HYDROCARBON CORONENE BY PROTON IRRADIATION IN COSMIC ICE ANALOGS Max P. Bernstein,1,2 Marla H. Moore,3 Jamie E. Elsila,4 Scott A. Sandford,2 Louis J. Allamandola,2 and Richard N. Zare4 Received 2002 July 23; accepted 2002 November 5; published 2002 December 6 ABSTRACT ∼ Ices at 15 K consisting of the polycyclic aromatic hydrocarbon coronene (C24H12) condensed either with H2O, CO2, or CO in the ratio of 1 : 100 or greater have been subjected to MeV proton bombardment from a Van de Graaff generator. The resulting reaction products have been examined by infrared transmission- reflection-transmission spectroscopy and by microprobe laser-desorption laser-ionization mass spectrometry. Just as in the case of UV photolysis, oxygen atoms are added to coronene, yielding, in the case of H2O ices, the addition of one or more alcohol (i OH) and ketone (1CuO) side chains to the coronene scaffolding. There are, however, significant differences between the products formed by proton irradiation and the products formed by UV photolysis of coronene containing CO and CO2 ices. The formation of a coronene carboxylic i acid ( COOH) by proton irradiation is facile in solid CO but not in CO2, the reverse of what was previously observed for UV photolysis under otherwise identical conditions. This work presents evidence that cosmic- ray irradiation of interstellar or cometary ices should have contributed to the formation of aromatics bearing ketone and carboxylic acid functional groups in primitive meteorites and interplanetary dust particles.
    [Show full text]
  • Rowan C. Martindale Curriculum Vitae Associate Professor (Invertebrate Paleontology) at the University of Texas at Austin
    ROWAN C. MARTINDALE CURRICULUM VITAE ASSOCIATE PROFESSOR (INVERTEBRATE PALEONTOLOGY) AT THE UNIVERSITY OF TEXAS AT AUSTIN Department of Geological Sciences E-mail: [email protected] Jackson School of Geosciences Website: www.jsg.utexas.edu/martindale/ 2275 Speedway Stop C9000 Orchid ID: 0000-0003-2681-083X Austin, TX 78712-1722 Phone: 512-475-6439 Office: JSG 3.216A RESEARCH INTERESTS The overarching theme of my work is the connection between Earth and life through time, more precisely, understanding ancient (Mesozoic and Cenozoic) ocean ecosystems and the evolutionary and environmental events that shaped them. My research is interdisciplinary, (paleontology, sedimentology, biology, geochemistry, and oceanography) and focuses on: extinctions and carbon cycle perturbation events (e.g., Oceanic Anoxic Events, acidification events); marine (paleo)ecology and reef systems; the evolution of reef builders (e.g., coral photosymbiosis); and exceptionally preserved fossil deposits (Lagerstätten). ACADEMIC APPOINTMENTS Associate Professor, University of Texas at Austin September 2020 to Present Assistant Professor, University of Texas at Austin August 2014 to August 2020 Postdoctoral Researcher, Harvard University August 2012 to July 2014 Department of Organismic and Evolutionary Biology; Mentor: Dr. Andrew H. Knoll. EDUCATION Doctorate, University of Southern California 2007 to 2012 Dissertation: “Paleoecology of Upper Triassic reef ecosystems and their demise at the Triassic-Jurassic extinction, a potential ocean acidification event”. Advisor: Dr. David J. Bottjer, degree conferred August 7th, 2012. Bachelor of Science Honors Degree, Queen’s University 2003 to 2007 Geology major with a general concentration in Biology (Geological Sciences Medal Winner). AWARDS AND RECOGNITION Awards During Tenure at UT Austin • 2019 National Science Foundation CAREER Award: Awarded to candidates who are judged to have the potential to serve as academic role models in research and education.
    [Show full text]
  • Interstellar Dust Within the Life Cycle of the Interstellar Medium K
    EPJ Web of Conferences 18, 03001 (2011) DOI: 10.1051/epjconf/20111803001 C Owned by the authors, published by EDP Sciences, 2011 Interstellar dust within the life cycle of the interstellar medium K. Demyk1,2,a 1Université de Toulouse, UPS-OMP, IRAP, Toulouse, France 2CNRS, IRAP, 9 Av. colonel Roche, BP. 44346, 31028 Toulouse Cedex 4, France Abstract. Cosmic dust is omnipresent in the Universe. Its presence influences the evolution of the astronomical objects which in turn modify its physical and chemical properties. The nature of cosmic dust, its intimate coupling with its environment, constitute a rich field of research based on observations, modelling and experimental work. This review presents the observations of the different components of interstellar dust and discusses their evolution during the life cycle of the interstellar medium. 1. INTRODUCTION Interstellar dust grains are found everywhere in the Universe: in the Solar System, around stars at all evolutionary stages, in interstellar clouds of all kind, in galaxies and in the intergalactic medium. Cosmic dust is intimately mixed with the gas-phase and represents about 1% of the gas (in mass) in our Galaxy. The interstellar extinction and the emission of diffuse interstellar clouds is reproduced by three dust components: a population of large grains, the BGs (Big Grains, ∼10–500 nm) made of silicate and a refractory mantle, a population of carbonaceous nanograins, the VSGs (Very Small Grains, 1–10 nm) and a population of macro-molecules the PAHs (Polycyclic Aromatic Hydrocarbons) [1]. These three components are more or less abundant in the diverse astrophysical environments reflecting the coupling of dust with the environment and its evolution according to the physical and dynamical conditions.
    [Show full text]
  • Dornbos.Web.CV
    Stephen Quinn Dornbos Associate Professor and Department Chair Department of Geosciences University of Wisconsin-Milwaukee Milwaukee, WI 53201-0413 Phone: (414) 229-6630 Fax: (414) 229-5452 E-mail: [email protected] http://uwm.edu/geosciences/people/dornbos-stephen/ EDUCATION 2003 Ph.D., Geological Sciences, University of Southern California, Los Angeles, CA. 1999 M.S., Geological Sciences, University of Southern California, Los Angeles, CA. 1997 B.A., Geology, The College of Wooster, Wooster, OH. ADDITIONAL EDUCATION 2002 University of Washington, Summer Marine Invertebrate Zoology Course, Friday Harbor Laboratories. 1997 Louisiana State University, Summer Field Geology Course. PROFESSIONAL EXPERIENCE 2017-Present Department Chair, Department of Geosciences, University of Wisconsin-Milwaukee. 2010-Present Associate Professor, Department of Geosciences, University of Wisconsin-Milwaukee. 2004-2010 Assistant Professor, Department of Geosciences, University of Wisconsin-Milwaukee. 2012-Present Adjunct Curator, Geology Department, Milwaukee Public Museum. 2004-Present Curator, Greene Geological Museum, University of Wisconsin- Milwaukee. 2003-2004 Postdoctoral Research Fellow, Department of Earth Sciences, University of Southern California. 2002 Research Assistant, Invertebrate Paleontology Department, Natural History Museum of Los Angeles County. EDITORIAL POSITIONS 2017-Present Editorial Board, Heliyon. 2015-Present Board of Directors, Coquina Press. 2014-Present Commentaries Editor, Palaeontologia Electronica. 2006-Present Associate Editor, Palaeontologia Electronica. Curriculum Vitae – Stephen Q. Dornbos 2 RESEARCH INTERESTS 1) Evolution and preservation of early life on Earth. 2) Evolutionary paleoecology of early animals during the Cambrian radiation. 3) Geobiology of microbial structures in Precambrian–Cambrian sedimentary rocks. 4) Cambrian reef evolution, paleoecology, and extinction. 5) Exceptional fossil preservation. HONORS AND AWARDS 2013 UWM Authors Recognition Ceremony. 2011 Full Member, Sigma Xi.
    [Show full text]
  • L115 Modeling the Unidentified Infrared Emission With
    The Astrophysical Journal, 511:L115±L119, 1999 February 1 q 1999. The American Astronomical Society. All rights reserved. Printed in U.S.A. MODELING THE UNIDENTIFIED INFRARED EMISSION WITH COMBINATIONS OF POLYCYCLIC AROMATIC HYDROCARBONS L. J. Allamandola, D. M. Hudgins, and S. A. Sandford NASA Ames Research Center, MS 245-6, Moffett Field, CA 94035 Received 1998 July 13; accepted 1998 November 24; published 1999 January 18 ABSTRACT The infrared emission band spectrum associated with many different interstellar objects can be modeled successfully by using combined laboratory spectra of neutral and positively charged polycyclic aromatic hydro- carbons (PAHs). These model spectra, shown here for the ®rst time, alleviate the principal spectroscopic criticisms previously leveled at the PAH hypothesis and demonstrate that mixtures of free molecular PAHs can indeed account for the overall appearance of the widespread interstellar infrared emission spectrum. Furthermore, these models give us insight into the structures, stabilities, abundances, and ionization balance of the interstellar PAH population. These, in turn, re¯ect conditions in the emission zones and shed light on the microscopic processes involved in the carbon nucleation, growth, and evolution in circumstellar shells and the interstellar medium. Subject headings: infrared: ISM: lines and bands Ð ISM: individual (Orion Bar, IRAS 2227215435) Ð line: formation Ð line: identi®cation Ð line: pro®les Ð molecular data Ð radiation mechanisms: nonthermal 1. INTRODUCTION resemblance of the
    [Show full text]
  • Cosmic-Ray Soil Water Monitoring: the Development, Status & Potential of the COSMOS- India Network Ross Morrison, J
    Cosmic-ray soil water monitoring: the development, status & potential of the COSMOS- India network Ross Morrison, J. G. Evans, S. S. Angadi, L. Ball, T. Chakraborty, H. Cooper, M. Fry, G. Geet, M. Goswami, N. Ganeshi, O. Hitt, S. Jain, M. Krishnan, R. Krishnan, A. Kumar, M. Mujumdar, M. Nema, G. Rees, M. Sekhar, O. Swain, R. Thayyen, S. Tripathi, D. Upadhyaya & A. Jenkins COSMOS-India: outline o Background & rationale o Basics of measurement principle o COSMOS-India network & sites o Selected results o Future work COSMOS-India: objectives o Collaborative development of soil moisture (SM) network in India using cosmic ray (COSMOS) sensors o Deliver high temporal frequency SM observations at the intermediate spatial scale in near real-time o Development of national COSMOS-India data system & near real time data portal o Integrate with Earth Observation datasets for validated SM maps of India o Empower many other applications… Acknowledgment: other COSMOS networks cosmos.hwr.arizona.edu cosmos.ceh.ac.uk Why measure soil moisture (SM)? o Controls exchanges of energy & mass between land surface & atmosphere o Hydrology: controls evapotranspiration, partitioning between runoff & infiltration, groundwater recharge o Meteorology: partitioning solar energy into sensible, latent & soil heat fluxes, surface-boundary layer interactions o Plant growth & soil biogeochemistry https://www2.ucar.edu/atmosnews/people/aiguo-dai https://nevada.usgs.gov/water/et/measured.htm Applications of soil moisture data SM observation techniques o Challenge: SM observations at spatial & temporal resolution relevant Measuringto applications soil (e.g.moisture gridded models, content field scale) o Point scale: high temporal resolution & low cost o Issues - spatial heterogeneity & sensor placement (e.g.
    [Show full text]
  • The Next Decade in Astrochemistry: an Integrated Approach
    The Next Decade in Astrochemistry: An Integrated Approach An Astro2010 Science White Paper by Lucy M. Ziurys (U. Arizona) Michael C. McCarthy (Harvard, CfA) Anthony Remijan (NRAO) DeWayne Halfen (U.Arizona) Al Wooten (NRAO) Brooks H. Pate (U.Virginia) Science Frontier Panels: Planets and Stars and Star Formation Stars and Stellar Evolution The Galactic Neighborhood 1 Introduction: The Transformational Role of Astrochemistry: Among the most fundamental questions in astronomy are those concerning the formation of stars and planets from interstellar material and the feedback mechanisms from those stars on the dynamics and chemical evolution of the ISM itself. Studies of the Milky Way and other galaxies in the Local Group have shown that massive molecular clouds are the principal sites of star formation (e.g. Rosolowsky and Blitz 2005). The resultant stars can limit the star formation process as their radiation heats and disperses the remaining cloud (e.g. Matzner 2002). Star formation itself generally proceeds through the formation of a proto-planetary disk, which in turn leads to the establishment of planetary systems (e.g. Glassgold et al. 2004) and the creation of reservoirs of icy bodies. Such reservoirs are the sources of comets, asteroids, and meteorites, which provide a continuing source of material to planets via bombardment (e.g. Mumma et al. 2003). The material in stars is subject to nuclear processing, and some of it is returned to the ISM via supernovae and mass loss from other evolved stars (Asymptotic Giant Branch (AGB), red giants and supergiants: e.g. Wilson 2000). In our galaxy, planetary nebulae, which form from AGB stars, are thought to supply almost an order of magnitude more mass to the ISM than supernovae (e.g.
    [Show full text]