Jani Radebaugh
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2020 Technology and Research Initiative Fund Annual Report
FISCAL YEAR 2020 TECHNOLOGY AND RESEARCH INITIATIVE FUND ABOUT THIS REPORT The fiscal year 2020 Arizona Board of Regents Technology and Research Initiative Fund filed in accordance with A.R.S. §15-1648(D) includes the prior year’s TRIF expenditures. The board adopted TRIF five-year project plans, available on the ABOR website, detailing anticipated budgets and expected outcomes. TRIF was established through Proposition 301 that increased the state’s sales tax to be dedicated to K-12, community colleges and Arizona’s public universities. Collection of the tax began on June 1, 2001, and the proposition was extended for another 20 years in 2018. Arizona law establishes TRIF using Proposition 301 sales tax revenue and gives the Arizona Board of Regents the responsibility to administer the fund. TRIF monies are continuously appropriated to ABOR and do not lapse at the end of the fiscal year. The fiscal year 2020 TRIF report details research goals, accomplishments and highlights from the universities that address challenges to the state and society as well as detailed financial information on how the funds were utilized. Through TRIF funds, the institutions are able to accomplish advances in vital research, including COVID-19 research, virus biotech detection, water resources and more. ABOUT THE ARIZONA BOARD OF REGENTS The Arizona Board of Regents is committed to ensuring access for qualified residents of Arizona to undergraduate and graduate institutions; promoting the discovery, application, and dissemination of new knowledge; extending the benefits of university activities to Arizona’s citizens outside the university; and maximizing the benefits derived from the state’s investment in education. -
Ecological Importance of Benthic Macroinvertebrates in Utah Lake
Ecological Importance of Benthic Macroinvertebrates in Utah Lake File name: Ecological Role of Benthic Macroinvertebrates in Utah Lake Focus on the Keystone Taxon Chironomidae and HABs Version 1.2 Ecological Importance of Benthic Macroinvertebrates in Utah Lake With a Focus on the Role of the Keystone Taxon Chironomidae on HABs Progress Report January 28, 2017 By: David C. Richards, Ph. D. OreoHelix Consulting Phone: 406.580.7816 Email: [email protected] and Theron Miller, Ph.D. Jordan River Farmington Bay Water Quality Council OreoHelix Consulting 1 Ecological Importance of Benthic Macroinvertebrates in Utah Lake Introduction Benthic macroinvertebrates are a critical component of the ecology and ecosystem functioning of Utah Lake. They are a major link between sediment chemistry, water column chemistry, nutrient cycling, benthic algae, phytoplankton, and Utah Lake’s food web including carp, game fish, June suckers, waterfowl, shorebirds, etc. Benthic invertebrates provide underappreciated but invaluable ecosystem services and are keystone taxa instrumental for the functioning of Utah Lake’ ecosystem. It has become clear that several dominant benthic taxa, primarily chironomids, play a key role in the timing and intensity of harmful algal blooms (HABs) in the lake. Very few studies have been conducted on the benthic invertebrate assemblages in Utah Lake (Barnes and Toole 1981, Spencer and Denton 2003, Shiozawa and Barnes 1977) and none were conducted at the level and intensity that is presently being accomplished by this group. No study has ever examined the role of benthic invertebrates on HABs in Utah Lake, this is the first. Our research is also an important element of sediment chemistry, nutrients, and food web models that are presently being conducted by us and others on Utah Lake. -
Geomorphology, Stratigraphy, and Paleohydrology of the Aeolis Dorsa Region, Mars, with Insights from Modern and Ancient Terrestrial Analogs
University of Tennessee, Knoxville TRACE: Tennessee Research and Creative Exchange Doctoral Dissertations Graduate School 12-2016 Geomorphology, Stratigraphy, and Paleohydrology of the Aeolis Dorsa region, Mars, with Insights from Modern and Ancient Terrestrial Analogs Robert Eric Jacobsen II University of Tennessee, Knoxville, [email protected] Follow this and additional works at: https://trace.tennessee.edu/utk_graddiss Part of the Geology Commons Recommended Citation Jacobsen, Robert Eric II, "Geomorphology, Stratigraphy, and Paleohydrology of the Aeolis Dorsa region, Mars, with Insights from Modern and Ancient Terrestrial Analogs. " PhD diss., University of Tennessee, 2016. https://trace.tennessee.edu/utk_graddiss/4098 This Dissertation is brought to you for free and open access by the Graduate School at TRACE: Tennessee Research and Creative Exchange. It has been accepted for inclusion in Doctoral Dissertations by an authorized administrator of TRACE: Tennessee Research and Creative Exchange. For more information, please contact [email protected]. To the Graduate Council: I am submitting herewith a dissertation written by Robert Eric Jacobsen II entitled "Geomorphology, Stratigraphy, and Paleohydrology of the Aeolis Dorsa region, Mars, with Insights from Modern and Ancient Terrestrial Analogs." I have examined the final electronic copy of this dissertation for form and content and recommend that it be accepted in partial fulfillment of the equirr ements for the degree of Doctor of Philosophy, with a major in Geology. Devon M. Burr, -
Mapping and Planetary Spatial Infrastructure Team
Mapping and Planetary Spatial Infrastructure Team INTRODUCTION SSB study on NASA PSD R&A Reorganization National Academy of Sciences, 13 May 2016 Jani Radebaugh, [email protected] Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products and associated geospatial infrastructure are integral to the success of the planetary science enterprise Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products and associated geospatial infrastructure are integral to the success of the planetary science enterprise Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products and associated geospatial infrastructure are integral to the success of the planetary science enterprise Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products and associated geospatial infrastructure are integral to the success of the planetary science enterprise Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products and associated geospatial infrastructure are integral to the success of the planetary science enterprise Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products and associated geospatial infrastructure are integral to the success of the planetary science enterprise Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products and associated geospatial infrastructure are integral to the success of the planetary science enterprise – Influence all phases of the mission lifecycle for science investigations and operations – Strategic needs must be anticipated and prioritized by the community – PSS recommended a “Cartography Research and Analysis Group” [CRAG] in Fall 2014. -
Planetary Surfaces
Chapter 4 PLANETARY SURFACES 4.1 The Absence of Bedrock A striking and obvious observation is that at full Moon, the lunar surface is bright from limb to limb, with only limited darkening toward the edges. Since this effect is not consistent with the intensity of light reflected from a smooth sphere, pre-Apollo observers concluded that the upper surface was porous on a centimeter scale and had the properties of dust. The thickness of the dust layer was a critical question for landing on the surface. The general view was that a layer a few meters thick of rubble and dust from the meteorite bombardment covered the surface. Alternative views called for kilometer thicknesses of fine dust, filling the maria. The unmanned missions, notably Surveyor, resolved questions about the nature and bearing strength of the surface. However, a somewhat surprising feature of the lunar surface was the completeness of the mantle or blanket of debris. Bedrock exposures are extremely rare, the occurrence in the wall of Hadley Rille (Fig. 6.6) being the only one which was observed closely during the Apollo missions. Fragments of rock excavated during meteorite impact are, of course, common, and provided both samples and evidence of co,mpetent rock layers at shallow levels in the mare basins. Freshly exposed surface material (e.g., bright rays from craters such as Tycho) darken with time due mainly to the production of glass during micro- meteorite impacts. Since some magnetic anomalies correlate with unusually bright regions, the solar wind bombardment (which is strongly deflected by the magnetic anomalies) may also be responsible for darkening the surface [I]. -
Planning a Mission to the Lunar South Pole
Lunar Reconnaissance Orbiter: (Diviner) Audience Planning a Mission to Grades 9-10 the Lunar South Pole Time Recommended 1-2 hours AAAS STANDARDS Learning Objectives: • 12A/H1: Exhibit traits such as curiosity, honesty, open- • Learn about recent discoveries in lunar science. ness, and skepticism when making investigations, and value those traits in others. • Deduce information from various sources of scientific data. • 12E/H4: Insist that the key assumptions and reasoning in • Use critical thinking to compare and evaluate different datasets. any argument—whether one’s own or that of others—be • Participate in team-based decision-making. made explicit; analyze the arguments for flawed assump- • Use logical arguments and supporting information to justify decisions. tions, flawed reasoning, or both; and be critical of the claims if any flaws in the argument are found. • 4A/H3: Increasingly sophisticated technology is used Preparation: to learn about the universe. Visual, radio, and X-ray See teacher procedure for any details. telescopes collect information from across the entire spectrum of electromagnetic waves; computers handle Background Information: data and complicated computations to interpret them; space probes send back data and materials from The Moon’s surface thermal environment is among the most extreme of any remote parts of the solar system; and accelerators give planetary body in the solar system. With no atmosphere to store heat or filter subatomic particles energies that simulate conditions in the Sun’s radiation, midday temperatures on the Moon’s surface can reach the stars and in the early history of the universe before 127°C (hotter than boiling water) whereas at night they can fall as low as stars formed. -
Mapping and Planetary Spatial Infrastructure Team
Mapping and Planetary Spatial Infrastructure Team Report to the Planetary Science Subcommittee March 2016 Introducing the Mapping and Planetary Spatial Infrastructure Team • Mosaics, geologic maps, derived regional and global data products, and associated geospatial infrastructure are integral to the success of the planetary science enterprise – Influences all phases of the mission lifecycle for science investigations and operations – Strategic needs must be anticipated and prioritized by the community – PSS recommended a “Cartography Research and Analysis Group” [CRAG] in Fall 2014. • A team fulfilling this role now exists in the form of MAPSIT – MAPSIT succeeds former PCGMWG and assumes strategic planning role But wait, I thought we did this already? • No, we didn’t (really!) • From 1974 to 2012: – 1974: Lunar Photography and Cartography Committee (LPACC) – 1977: Lunar and Planetary Photography and Cartography Committee (LPPACC) – 1979: Planetary Cartography Working Group (PCWG) – Produced two 10-year plans and a supplement (at right) – 1994-2012: Planetary Cartography & Geologic Mapping Working Group (PCGMWG) • PCGMWG ceased “advisory” role in ~2011 • PCGMWG disbanded 2015 with end of PGG • Looming gap for NASA long-term strategic planning and prioritization activities until addressed by MAPSIT formation 3/9/2016 3 Enabling Planetary Science • Planetary Spatial Infrastructure is the technology, policies, standards, human resources, software tools, and related activities necessary to Geographic Information Science and Technology acquire, -
The Problem of the Brisbane Tuff
50 VoL. XLV., No. 11. The Problem of the Brisbane Tuff. By PROFESSOR H. C. RICHARDS, D. Sc., and W. H. BRYAN, D. Sc. (Department of Geology, University of Queensland). PLATES IV.-VI. ( Accepted for publication by the Roya� Society of Qiu!ensland, 30th November, 1933). · 1. INTRODUCTION. The following paper recor�s an attempt to discover the ongm, and explain the mode of formation of the rock now known as the Brisbane Tuff. While the authors long ago realised that this rock possessed a number of unusual features, their doubts as to its true nature were revived and strengthened when a section showing well developed columnar structure was exposed in the municipal quarry at Windsor some three miles north of the centre of the city of Brisbane. A more detailed examination disclosed other anomalous features, but a search of the literature showed that the characters displayed by the Brisbane Tuff, although rare, were not unique but could be closely paralleled in the "Great Hot Sand Flow" of Alaska and in the "Ignimbrites " of New Zealand, while they also resembled in certain respects the " Nitees ardentes" of Mt. Pelee. In the pages which follow only those features that have a direct bearing on the origin and nature of the Eris bane Tuff will be con sidered. For a more general account the reader is referred. to the paper by Mrs. C. Briggs (1928) published in these proceedings. 2. EARLIER VIEWS AS TO ORIGIN AND MODE OF FORMATION. The rock which is now knpwn as the Eris bane Tuff was first described by Leichhardt (1855) who examined the rock on his visit to Brisbane in 1844. -
GOVERNANCE & OVERSIGHT NARRATIVE Local Authority
GOVERNANCE & OVERSIGHT NARRATIVE Local Authority: Wasatch County Instructions: In the cells below, please provide an answer/description for each question. PLEASE CHANGE THE COLOR OF SUBSTANTIVE NEW LANGUAGE INCLUDED IN YOUR PLAN THIS YEAR! 1) Access & Eligibility for Mental Health and/or Substance Abuse Clients Who is eligible to receive mental health services within your catchment area? What services (are there different services available depending on funding)? Wasatch County Family Clinic-Wasatch Behavioral Health Special Service District (WCFC-WMH) is a comprehensive community mental health center providing mental health and substance use disorder services to the residents of Wasatch County. WCFC-WBH provides a mental health and Substance Use screening to any Wasatch County resident requesting services. Based on available resources, (funding or otherwise), prospective clients will be referred to or linked with available resources. Medicaid eligible clients will be provided access to the full array of services available. Individuals who carry commercial insurance will be seen as their benefits allow. Clients with no funding may be seen on a sliding fee scale. Who is eligible to receive substance abuse services within your catchment area? What services (are there different services available depending on funding)? Identify how you manage wait lists. How do you ensure priority populations get served? WCFC-WBH provides substance abuse services to residents of Wasatch County. Medicaid and commercial insurances are also accepted and services are provided as benefits allow. WCFC-WBH provides substance abuse services as funding allows those without insurance or ability to pay. A sliding fee scale is available for these clients. Clients accepted into the drug court also have all services available and fees are also set based on the sliding scale. -
Aeolian Processes and Landforms
Aeolian Processes and Landforms Ms. Deithra L. Archie, New Mexico State University Abstract I will present an overview of Aeolian processes and landforms on Mars. The overview will consist of two components. Component one is an overview of Aeolian processes and landforms on Earth and Mars, where the two planetary bodies are shown in Figures 1a and 1b respectively The second part of this paper will consist of image comparisons using satellite and MOC (Mars Orbiter Camera) images. Figure 1a Figure 1b Introduction Understanding the aeolian activity on the planet Mars and other planets begins with the study and knowledge of similar processes on Earth. Therefore, I will discuss the following: wind, particle entrainment and landforms found in the aeolian environment. This discussion will lead into my later discussion of the Martian sand seas and sand dunes. See Table 1 for a glossary of the terms used throughout this paper. In aeolian processes, wind transports and deposits particles of sediment. Aeolian features form in areas where wind is the primary source of erosion. The particles deposited are of sand, silt and clay size (see Table 2). The particles are entrained in by one of four processes. Creep is when a particle rolls or slides across the surface. Lift is when a particle rises off the surface due to the Bernoulli effect, the same mechanism which causes aircraft to rise. If the airflow is turbulent, larger particles are trajected by a process known as saltation. Finally, impact transport occurs which one particle strikes another causing the second particle to move. Erosional Landforms Wind eroded landforms are rarely preserved on the surface of the Earth except in arid regions. -
Io Volcano Observer
EPSC Abstracts Vol. 13, EPSC-DPS2019-996-1, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Follow the Heat: Io Volcano Observer A. S. McEwen1, E. Turtle2, L. Kestay3, K. Khurana4, J. Westlake2, P. Wurz5, J. Helbert6, R. Park7, M. Bland3, D. Breuer6, L. Carter1, A. G. Davies7, C. W. Hamilton1, S. Horst8, X. Jia9, L. Jozwiak2, J. T. Keane10, K. de Kleer10, V. Lainey7, K. Mandt2, I. Matsuyama1, O. Mousis11, F. Nimmo12, C. Paranicas2, J. Perry1, A. Pommier13, J. Radebaugh14, J. Spencer15, S. Sutton1, N. Thomas5, A. Vorburger5 1LPL, University of Arizona, 2JHU APL, 3USGS, 4UCLA, 5UBE, 6DLR, 7JPL, 8JHU, 9U.Michigan, 10Caltech, 11AMU, 12UCSC, 13UCSD, 14BYU, 15SwRI. Abstract A promising avenue to address these questions is a new spacecraft mission making multiple close flybys The Io Volcano Observer (IVO) Discovery mission of Io, combined with research and analysis motivated proposal [1] has been re-focused in 2019 towards by the mission. IVO will address all of these understanding tidal heating as a fundamental questions, while still within the constraints of NASA planetary process. To “Follow the Heat”, IVO will Discovery program. IVO will characterize volcanic determine how heat is generated in Io’s interior, processes (Q1); test interior models via a set of transported to the surface, and how heat and mass are geophysical measurements (coupled with laboratory lost to space. experiments and theory; Q2 and Q3); measure the total heat flow and orbital evolution of Io (Q4); and 1. Tidal Heating analyze mass loss processes (Q5). No new technologies are required for this mission, which Tidal heating is key to the evolution and habitability leverages advances in radiation design and solar of many worlds across our Solar System and beyond. -
Testing Hypotheses for the Origin of Steep Slope of Lunar Size-Frequency Distribution for Small Craters
CORE Metadata, citation and similar papers at core.ac.uk Provided by Springer - Publisher Connector Earth Planets Space, 55, 39–51, 2003 Testing hypotheses for the origin of steep slope of lunar size-frequency distribution for small craters Noriyuki Namiki1 and Chikatoshi Honda2 1Department of Earth and Planetary Sciences, Kyushu University, Hakozaki 6-10-1, Higashi-ku, Fukuoka 812-8581, Japan 2The Institute of Space and Astronautical Science, Yoshinodai 3-1-1, Sagamihara 229-8510, Japan (Received June 13, 2001; Revised June 24, 2002; Accepted January 6, 2003) The crater size-frequency distribution of lunar maria is characterized by the change in slope of the population between 0.3 and 4 km in crater diameter. The origin of the steep segment in the distribution is not well understood. Nonetheless, craters smaller than a few km in diameter are widely used to estimate the crater retention age for areas so small that the number of larger craters is statistically insufficient. Future missions to the moon, which will obtain high resolution images, will provide a new, large data set of small craters. Thus it is important to review current hypotheses for their distributions before future missions are launched. We examine previous and new arguments and data bearing on the admixture of endogenic and secondary craters, horizontal heterogeneity of the substratum, and the size-frequency distribution of the primary production function. The endogenic crater and heterogeneous substratum hypotheses are seen to have little evidence in their favor, and can be eliminated. The primary production hypothesis fails to explain a wide variation of the size-frequency distribution of Apollo panoramic photographs.