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USF Board of Trustees ( March 7, 2013)
Agenda item: (to be completed by Board staff) USF Board of Trustees ( March 7, 2013) Issue: Proposed Ph.D. in Integrative Biology ________________________________________________________________ Proposed action: New Degree Program Approval ________________________________________________________________ Background information: This application for a new Ph.D is driven by a recent reorganization of the Department of Biology. The reorganization began in 2006 and was completed in 2009. The reorganization of the Department of Biology, in part, reflected the enormity of the biological sciences, and in part, different research perspectives and directions taken by the faculty in each of the respective areas of biology. Part of the reorganization was to replace the original Ph.D. in Biology with two new doctoral degrees that better serve the needs of the State and our current graduate students by enabling greater focus of the research performed to earn the Ph.D. The well-established and highly productive faculty attracts students to the Tampa Campus from all over the United States as well as from foreign countries. The resources to support the two Ph.D. programs have already been established in the Department of Biology and are sufficient to support the two new degree programs. The reorganization created two new departments; the Department of Cell Biology, Microbiology, and Molecular Biology (CMMB) and the Department of Integrative Biology (IB). This proposal addresses the creation of a new Ph.D., in Integrative Biology offered by the Department of Integrative Biology (CIP Code 26.1399). The name of the Department, Integrative Biology, reflects the belief that the study of biological processes and systems can best be accomplished by the incorporation of numerous integrated approaches Strategic Goal(s) Item Supports: The proposed program directly supports the following: Goal 1 and Goal 2 Workgroup Review: ACE March 7, 2013 Supporting Documentation: See Complete Proposal below Prepared by: Dr. -
LCROSS (Lunar Crater Observation and Sensing Satellite) Observation Campaign: Strategies, Implementation, and Lessons Learned
Space Sci Rev DOI 10.1007/s11214-011-9759-y LCROSS (Lunar Crater Observation and Sensing Satellite) Observation Campaign: Strategies, Implementation, and Lessons Learned Jennifer L. Heldmann · Anthony Colaprete · Diane H. Wooden · Robert F. Ackermann · David D. Acton · Peter R. Backus · Vanessa Bailey · Jesse G. Ball · William C. Barott · Samantha K. Blair · Marc W. Buie · Shawn Callahan · Nancy J. Chanover · Young-Jun Choi · Al Conrad · Dolores M. Coulson · Kirk B. Crawford · Russell DeHart · Imke de Pater · Michael Disanti · James R. Forster · Reiko Furusho · Tetsuharu Fuse · Tom Geballe · J. Duane Gibson · David Goldstein · Stephen A. Gregory · David J. Gutierrez · Ryan T. Hamilton · Taiga Hamura · David E. Harker · Gerry R. Harp · Junichi Haruyama · Morag Hastie · Yutaka Hayano · Phillip Hinz · Peng K. Hong · Steven P. James · Toshihiko Kadono · Hideyo Kawakita · Michael S. Kelley · Daryl L. Kim · Kosuke Kurosawa · Duk-Hang Lee · Michael Long · Paul G. Lucey · Keith Marach · Anthony C. Matulonis · Richard M. McDermid · Russet McMillan · Charles Miller · Hong-Kyu Moon · Ryosuke Nakamura · Hirotomo Noda · Natsuko Okamura · Lawrence Ong · Dallan Porter · Jeffery J. Puschell · John T. Rayner · J. Jedadiah Rembold · Katherine C. Roth · Richard J. Rudy · Ray W. Russell · Eileen V. Ryan · William H. Ryan · Tomohiko Sekiguchi · Yasuhito Sekine · Mark A. Skinner · Mitsuru Sôma · Andrew W. Stephens · Alex Storrs · Robert M. Suggs · Seiji Sugita · Eon-Chang Sung · Naruhisa Takatoh · Jill C. Tarter · Scott M. Taylor · Hiroshi Terada · Chadwick J. Trujillo · Vidhya Vaitheeswaran · Faith Vilas · Brian D. Walls · Jun-ihi Watanabe · William J. Welch · Charles E. Woodward · Hong-Suh Yim · Eliot F. Young Received: 9 October 2010 / Accepted: 8 February 2011 © The Author(s) 2011. -
Investigating Mineral Stability Under Venus Conditions: a Focus on the Venus Radar Anomalies Erika Kohler University of Arkansas, Fayetteville
University of Arkansas, Fayetteville ScholarWorks@UARK Theses and Dissertations 5-2016 Investigating Mineral Stability under Venus Conditions: A Focus on the Venus Radar Anomalies Erika Kohler University of Arkansas, Fayetteville Follow this and additional works at: http://scholarworks.uark.edu/etd Part of the Geochemistry Commons, Mineral Physics Commons, and the The unS and the Solar System Commons Recommended Citation Kohler, Erika, "Investigating Mineral Stability under Venus Conditions: A Focus on the Venus Radar Anomalies" (2016). Theses and Dissertations. 1473. http://scholarworks.uark.edu/etd/1473 This Dissertation is brought to you for free and open access by ScholarWorks@UARK. It has been accepted for inclusion in Theses and Dissertations by an authorized administrator of ScholarWorks@UARK. For more information, please contact [email protected], [email protected]. Investigating Mineral Stability under Venus Conditions: A Focus on the Venus Radar Anomalies A dissertation submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy in Space and Planetary Sciences by Erika Kohler University of Oklahoma Bachelors of Science in Meteorology, 2010 May 2016 University of Arkansas This dissertation is approved for recommendation to the Graduate Council. ____________________________ Dr. Claud H. Sandberg Lacy Dissertation Director Committee Co-Chair ____________________________ ___________________________ Dr. Vincent Chevrier Dr. Larry Roe Committee Co-chair Committee Member ____________________________ ___________________________ Dr. John Dixon Dr. Richard Ulrich Committee Member Committee Member Abstract Radar studies of the surface of Venus have identified regions with high radar reflectivity concentrated in the Venusian highlands: between 2.5 and 4.75 km above a planetary radius of 6051 km, though it varies with latitude. -
Styles of Deformation in Ishtar Terra and Their Implications
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 97, NO. El0, PAGES 16,085-16,120, OCTOBER 25, 1992 Stylesof Deformationin IshtarTerra and Their Implications Wn.T.TAMM. KAU•A,• DOAN•L. BINDSCHAD•-R,l ROBERT E. GPaM•,2'3 VICKIL. HANSEN,2KARl M. ROBERTS,4AND SUZANNE E. SMREr,AR s IshtarTerra, the highest region on Venus, appears to havecharacteristics of both plume uplifts and convergent belts.Magellan imagery over longitudes 330ø-30øE indicates a great variety of tectonicand volcanic activity, with largevariations within distances of onlya few 100km. Themost prominent terrain types are the volcanic plains of Lakshmiand the mountain belts of Maxwell,Freyja, and Danu. Thebelts appear to havemarked variations in age. Thereare also extensive regions of tesserain boththe upland and outboard plateaus, some rather featureless smoothscarps, flanking basins of complexextensional tectonics, and regions of gravitationalor impactmodifica- tion.Parts of Ishtarare the locations of contemporaryvigorous tectonics and past extensive volcanism. Ishtar appearsto be the consequence of a history of several100 m.y., in whichthere have been marked changes in kinematic patternsand in whichactivity at any stage has been strongly influenced by the past. Ishtar demonstrates three general propertiesof Venus:(1) erosionaldegradation is absent,leading to preservationof patternsresulting from past activity;(2) manysurface features are the responses ofa competentlayer less than 10 km thick to flowsof 100km orbroaderscale; and (3) thesebroader scale flows are controlled mainly by heterogeneities inthe mantle. Ishtar Terra doesnot appear to bethe result of a compressionconveyed by anEarthlike lithosphere. But there is stilldoubt as to whetherIshtar is predominantlythe consequence of a mantleupflow or downflow.Upflow is favoredby the extensivevolcanic plain of Lakshmiand the high geoid: topography ratio; downflow is favoredby the intense deformationof themountain belts and the absence of majorrifts. -
The Magellan Spacecraft at Venus by Andrew Fraknoi, Astronomical Society of the Pacific
www.astrosociety.org/uitc No. 18 - Fall 1991 © 1991, Astronomical Society of the Pacific, 390 Ashton Avenue, San Francisco, CA 94112. The Magellan Spacecraft at Venus by Andrew Fraknoi, Astronomical Society of the Pacific "Having finally penetrated below the clouds of Venus, we find its surface to be naked [not hidden], revealing the history of hundreds of millions of years of geological activity. Venus is a geologist's dream planet.'' —Astronomer David Morrison This fall, the brightest star-like object you can see in the eastern skies before dawn isn't a star at all — it's Venus, the second closest planet to the Sun. Because Venus is so similar in diameter and mass to our world, and also has a gaseous atmosphere, it has been called the Earth's "sister planet''. Many years ago, scientists expected its surface, which is perpetually hidden beneath a thick cloud layer, to look like Earth's as well. Earlier this century, some people even imagined that Venus was a hot, humid, swampy world populated by prehistoric creatures! But we now know Venus is very, very different. New radar images of Venus, just returned from NASA's Magellan spacecraft orbiting the planet, have provided astronomers the clearest view ever of its surface, revealing unique geological features, meteor impact craters, and evidence of volcanic eruptions different from any others found in the solar system. This issue of The Universe in the Classroom is devoted to what Magellan is teaching us today about our nearest neighbor, Venus. Where is Venus, and what is it like? Spacecraft exploration of Venus's surface Magellan — a "recycled'' spacecraft How does Magellan take pictures through the clouds? What has Magellan revealed about Venus? How does Venus' surface compare with Earth's? What is the next step in Magellan's mission? If Venus is such an uninviting place, why are we interested in it? Reading List Why is it so hot on Venus? Where is Venus, and what is it like? Venus orbits the Sun in a nearly circular path between Mercury and the Earth, about 3/4 as far from our star as the Earth is. -
Seasonal Melting and the Formation of Sedimentary Rocks on Mars, with Predictions for the Gale Crater Mound
Seasonal melting and the formation of sedimentary rocks on Mars, with predictions for the Gale Crater mound Edwin S. Kite a, Itay Halevy b, Melinda A. Kahre c, Michael J. Wolff d, and Michael Manga e;f aDivision of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California 91125, USA bCenter for Planetary Sciences, Weizmann Institute of Science, P.O. Box 26, Rehovot 76100, Israel cNASA Ames Research Center, Mountain View, California 94035, USA dSpace Science Institute, 4750 Walnut Street, Suite 205, Boulder, Colorado, USA eDepartment of Earth and Planetary Science, University of California Berkeley, Berkeley, California 94720, USA f Center for Integrative Planetary Science, University of California Berkeley, Berkeley, California 94720, USA arXiv:1205.6226v1 [astro-ph.EP] 28 May 2012 1 Number of pages: 60 2 Number of tables: 1 3 Number of figures: 19 Preprint submitted to Icarus 20 September 2018 4 Proposed Running Head: 5 Seasonal melting and sedimentary rocks on Mars 6 Please send Editorial Correspondence to: 7 8 Edwin S. Kite 9 Caltech, MC 150-21 10 Geological and Planetary Sciences 11 1200 E California Boulevard 12 Pasadena, CA 91125, USA. 13 14 Email: [email protected] 15 Phone: (510) 717-5205 16 2 17 ABSTRACT 18 A model for the formation and distribution of sedimentary rocks on Mars 19 is proposed. The rate{limiting step is supply of liquid water from seasonal 2 20 melting of snow or ice. The model is run for a O(10 ) mbar pure CO2 atmo- 21 sphere, dusty snow, and solar luminosity reduced by 23%. -
The Earth-Based Radar Search for Volcanic Activity on Venus
52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 2339.pdf THE EARTH-BASED RADAR SEARCH FOR VOLCANIC ACTIVITY ON VENUS. B. A. Campbell1 and D. B. Campbell2, 1Smithsonian Institution Center for Earth and Planetary Studies, MRC 315, PO Box 37012, Washington, DC 20013-7012, [email protected]; 2Cornell University, Ithaca, NY 14853. Introduction: Venus is widely expected to have geometry comes from shifts in the latitude of the sub- ongoing volcanic activity based on its similar size to radar point, which spans the range from about 8o S Earth and likely heat budget. How lithospheric (2017) to 8o N (2015). Observations in 1988, 2012, and thickness and volcanic activity have varied over the 2020 share a similar sub-radar point latitude of ~3o S. history of the planet remains uncertain. While tessera Coverage of higher northern and southern latitudes may highlands locally represent a period of thinner be obtained during favorable conjunctions (Fig. 1), but lithosphere and strong deformation, there is no current the shift in incidence angle must be recognized in means to determine whether they formed synchronously analysis of surface features over time. The 2012 data on hemispheric scales. Understanding the degree to were collected in an Arecibo-GBT bistatic geometry which mantle plumes currently thin and uplift the crust that led to poorer isolation between the hemispheres. to create deformation and effusive eruptions will better inform our understanding of the “global” versus Searching for Change. Ideally, surface change “localized” timing of heat transport. Ground-based detection could be achieved by co-registering and radar mapping of one hemisphere of Venus over the past differencing any pair of radar maps. -
Westfield Council Approves Budget (Continued from Page A-L) Sullivan Also Thanked State Two More Years," Said Echausse
Cook's walk-off homer lifts WHS past Union. Please see Sports, Page C-1. WESTFIELD SCOTCH PLAINS FANWOOD Vol. 16, No.' Friday, April 27, 2001 50 cents Aro Small businesses have a friend in county corporation By GREG MARX For loans or training, the UCEDC is there for the little guys Trustees with members from "all Tow THE RECORD-PRESS walks of life," Brown said. The Bonn! of Trustees offers guidance Westfield wel< UNION COUNTY — In mod- an important ally in the Union "our key goal is to assist smiill- under-served groups, such as on how the UCEDC can best dis- ern suburban communities, small County Economic Development and medium-size businesses in women and minority entrepre- tribute the funds it collects from TV-36broadc downtown businesses often Corporation. low- to moderate-income areas." neurs. fund-raising activities and WESTHEtti struggle to compete with huge According to Susan Brown, In more affluent areas, Brown To undertake that task, the grunts from county and federal access televisi' chain stores on regional high- director of Business said, the UCEDC seeks to help UCEDC lias a paid staff of 12 agencies. launched a new ways. But local businesses have Development for the UCEDC, individuals from historically and a volunteer Board of (Continued on page A-8) night with a ril thenewTV-36br The center is second floor of the Westfield Westfield council Municipal Building and will replace space previously occu- pied at Westfield High School. Phil Falcone, chairman of the TV- 36 Advisory Committee, said offi- approves budget cials hope the new center will enhance broadcasts over the a whole cent, according to town cable-access channel. -
Final Report Venus Exploration Targets Workshop May 19–21
Final Report Venus Exploration Targets Workshop May 19–21, 2014, Lunar and Planetary Institute, Houston, TX Conveners: Virgil (Buck) Sharpton, Larry Esposito, Christophe Sotin Breakout Group Leads Science from the Surface Larry Esposito, Univ. Colorado Science from the Atmosphere Kevin McGouldrick, Univ. Colorado Science from Orbit Lori Glaze, GSFC Science Organizing Committee: Ben Bussey, Martha Gilmore, Lori Glaze, Robert Herrick, Stephanie Johnston, Christopher Lee, Kevin McGouldrick Vision: The intent of this “living” document is to identify scientifically important Venus targets, as the knowledge base for this planet progresses, and to develop a target database (i.e., scientific significance, priority, description, coordinates, etc.) that could serve as reference for future missions to Venus. This document will be posted in the VEXAG website (http://www.lpi.usra.edu/vexag/), and it will be revised after the completion of each Venus Exploration Targets Workshop. The point of contact for this document is the current VEXAG Chair listed at ABOUT US on the VEXAG website. Venus Exploration Targets Workshop Report 1 Contents Overview ....................................................................................................................................................... 2 1. Science on the Surface .............................................................................................................................. 3 2. Science within the Atmosphere ............................................................................................................... -
Volcanology © Springer-Verlag 1992
Bull Volcanol (1992) 55:97-109 Volcanology © Springer-Verlag 1992 The caldera of Volcan Fernandina: a remote sensing study of its structure and recent activity Scott K Rowland and Duncan C Munro Planetary Geosciences, Geology and Geophysics Department, University of Hawaii at Manoa, Honolulu, Hawaii 96822 Received January 4, 1992/Accepted July 9, 1992 Abstract. Air photographs taken in 1946, 1960, and Introduction 1982, together with SPOT HVR-1 images obtained in April and October of 1988, are used to characterize re The Galapagos volcanoes have been the subject of nu cent activity in and around the caldera of Fernandina merous overview studies (e.g. Richards 1962; McBirney Volcano, West Galapagos Islands. The eruptive and col and Williams 1969; Nordlie 1973; Simkin 1984), and lapse events during this time span appear to be distri some detailed work. The geographic isolation and diffi buted in a NW-SE band across the summit and caldera. cult working conditions of these volcanoes mean that re On the flanks of the volcano, subtle topographic ridges mote-sensing studies (e.g. Chadwick and Howard 1991; indicate that this is a long-term preferred orientation of Munro et al. 1991; Munro 1992), although unable to re extra-caldera activity as well (although radial and ar place the detail available to ground observers, offer a cuate fissures are found on all sectors). The caldera is synoptic viewpoint that is useful for making inferences formed from the coalescence of multiple collapse fea about structures and processes. Both aerial photographs tures that are also distributed along a NW-SE direction, (1946, 1960, and 1982) and SPOT HRV-1 images (1988) and these give the caldera its elongate and scalloped out have been used in the present study and they provide a line. -
User Guide to the Magellan Synthetic Aperture Radar Images
https://ntrs.nasa.gov/search.jsp?R=19950018567 2020-06-16T07:22:10+00:00Z User Guide to the Magellan Synthetic Aperture Radar Images Stephen D. Wall Shannon L. McConnell Craig E. Left Richard S. Austin Kathi K. Beratan Mark J. Rokey National Aeronautics and Jet Propulsion Laboratory Space Administration California Institute of Technology Scientific and Technical Pasadena, California Information Branch NASA Reference Publication 1356 March 1995 This publication was prepared at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration. Contents Iri Introduction .................................................................................................................................................................... 1 I_1 The Spacecraft ................................................................................................................................................................ 2 IB Mission Design ................................................................................................................................................................ 4 D Experiment Description ................................................................................................................................................ 15 B Mission Operations ....................................................................................................................................................... 17 [] Notable Events and Problems ..................................................................................................................................... -
Volcanism and Tectonism in Rusalka Planitia and Atla Regio, Venus; M
LPSC xn/ 767 VOLCANISM AND TECTONISM IN RUSALKA PLANITIA AND ATLA REGIO, VENUS; M. G. Lancaster and J. E. Guest (University of London Observatory, University College London, London, NW7 2QS, U. K.). In order to investigate the relationships between volcanism and tectonism in Rusalka Planitia and Atla Regio, the geology of four adjacent Cycle 1 Magellan ClMIDRs has been mapped (C100N180, C115N180, C115N197, and C100N197). These cover nearly 12 x 106 km2 between latitudes 7.6 S and 22.6 N, and longitudes 171.4 to 206.2 E. This region was chosen because it contains nearly all the types of volcanic and tectonic features observed on Venus, and covers plains as well as highlands. The western half of the region comprises most of the volcanic plains of Rusalka Planitia, which are characterized by a large-scale pervasive fabric of NW-SE trending sinuous ridges that resemble lunar and martian wrinkle ridges [I]. A NW-SE to N-S trending deformation belt occupies the SW comer of C100N180, and contains several coronae including Eigin Corona (5.0 S, 175.0 E). The belt is the source for large, radar-bright, plains forming, flood lava flow fields. A similar collection of corona-like centers and deformation belts composed largely of ridges, is found in the NE comer of C115N197, where an extensive collection of lava flow fields is also present. Other smaller regions of radar-bright lava lie scattered across the plains. A number of N-S to NNW-SSE trending ridge belts occupy the north-central part of these plains.