Drug-Rich Phases Induced by Amorphous Solid Dispersion: Arbitrary Or Intentional Goal in Oral Drug Delivery?
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Former Astronaut Visits Stennis
Volume 7 Issue 8 www.nasa.gov/centers/stennis August 2012 Touchdown! Take it both ways – the Mars Science Laboratory rover, Curiosity, touched Sharp at a height of about 3.4 miles, taller than Mount Whitney in California. down on the surface of Mars early on the morning of Aug. 6 CDT, and the The Curiosity team hopes to drive the rover to the mountain to investigate NASA team scored a very big touchdown for space exploration. This image its lower layers, which scientists think hold clues to past environmental taken by Curiosity shows what lies ahead for the rover – its main science change. This image was captured by a rover camera shortly after it landed. target, Mount Sharp. The rover’s shadow can be seen in the foreground, It has been linearized to remove the distorted appearance that results from and the dark bands beyond are dunes. Rising up in the distance is Mount its fisheye lens. For additional coverage and photos, see pages 4-7. Page 2 LAGNIAPPE August 2012 “NASA is in a unique position to excite and inspire students about STEM education, and to help grow our technical workforce.” From the desk of Katie Wallace Director, Office of Education, Stennis Space Center he Mars Science Laboratory’s successful land- and over 8,000 students and parents. Our workshops ing on Mars early Aug. 6 was a huge engi- have a satisfaction rating of 99 percent. Tneering accomplishment! Years of research, planning, collaboration and dedication came down to In addition, we focus on student activities that enrich seven minutes. -
Imaginative Geographies of Mars: the Science and Significance of the Red Planet, 1877 - 1910
Copyright by Kristina Maria Doyle Lane 2006 The Dissertation Committee for Kristina Maria Doyle Lane Certifies that this is the approved version of the following dissertation: IMAGINATIVE GEOGRAPHIES OF MARS: THE SCIENCE AND SIGNIFICANCE OF THE RED PLANET, 1877 - 1910 Committee: Ian R. Manners, Supervisor Kelley A. Crews-Meyer Diana K. Davis Roger Hart Steven D. Hoelscher Imaginative Geographies of Mars: The Science and Significance of the Red Planet, 1877 - 1910 by Kristina Maria Doyle Lane, B.A.; M.S.C.R.P. Dissertation Presented to the Faculty of the Graduate School of The University of Texas at Austin in Partial Fulfillment of the Requirements for the Degree of Doctor of Philosophy The University of Texas at Austin August 2006 Dedication This dissertation is dedicated to Magdalena Maria Kost, who probably never would have understood why it had to be written and certainly would not have wanted to read it, but who would have been very proud nonetheless. Acknowledgments This dissertation would have been impossible without the assistance of many extremely capable and accommodating professionals. For patiently guiding me in the early research phases and then responding to countless followup email messages, I would like to thank Antoinette Beiser and Marty Hecht of the Lowell Observatory Library and Archives at Flagstaff. For introducing me to the many treasures held deep underground in our nation’s capital, I would like to thank Pam VanEe and Ed Redmond of the Geography and Map Division of the Library of Congress in Washington, D.C. For welcoming me during two brief but productive visits to the most beautiful library I have seen, I thank Brenda Corbin and Gregory Shelton of the U.S. -
Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
Bose-Einstein Condensation Measurements and Superflow in Condensed Helium
JLowTempPhys DOI 10.1007/s10909-013-0855-0 Bose-Einstein Condensation Measurements and Superflow in Condensed Helium H.R. Glyde Received: 9 November 2012 / Accepted: 18 January 2013 © Springer Science+Business Media New York 2013 Abstract We review the formulation and measurement of Bose-Einstein condensa- tion (BEC) in liquid and solid helium. BEC is defined for a Bose gas and subsequently for interacting systems via the one-body density matrix (OBDM) valid for both uni- form and non-uniform systems. The connection between the phase coherence created by BEC and superflow is made. Recent measurements show that the condensate frac- tion in liquid 4He drops from 7.25 ± 0.75 % at saturated vapor pressure (p ≈ 0) to 2.8 ± 0.2 % at pressure p = 24 bars near the solidification pressure (p = 25.3 bar). Extrapolation to solid densities suggests a condensate fraction in the solid of 1 % or less, assuming a frozen liquid structure such as an amorphous solid. Measurements in the crystalline solid have not been able to detect a condensate with an upper limit 4 set at n0 ≤ 0.3 %. Opportunities to observe BEC directly in liquid He confined in porous media, where BEC is localized to patches by disorder, and in amorphous solid helium is discussed. Keywords Solid · Liquid · Helium · BEC · OBDM · Neutron scattering 1 Introduction This article is part of a series motivated by reports of possible superfluidity in solid helium, initially in 2004 [1, 2]. Other articles in this series survey extensively the experiments and theory in this new field and the current status of the field. -
NATURE [Dec. 7, 1871
100 NATURE [Dec. 7, 1871 men is usually of the highest quality, both for carefulness evidence to prove that markings of various forms exist on the of investigation and clearness of statement ; and the great surface of the planet. I am the more particularly induced to say this by having before me upwards of sixty sketches of their appear similarity which exists b etwe~n t~e fau~as and floras ?f ance, made by experiencei ob,erven, wh J in the making of ob and of the Scandmav1an reg10n, enables th~,r our islands servations employ telescop~s of great power and excellent defioi work to be used to a certain extent as h andbooks by ti,ln. No doubt the faint cJ.rnrll 0 ke m1rkings can only be made British Naturalists. May their study lead the latter to out after attentive gazing, and then are scarcely visible, though imitate the Scandinavian mode of work! We are led to they have been distinctly ,een by many observers. It i, difficult these remarks by the receipt of the tenth and concluding to account for the fact that Mr. Dawe; could not di;fnguish volume of Prof. Thomson'::; descriptive work on the Scan them, but perhaps the reas m m1y be app.vent, if we co,isider that dinavian Coleoptera, alt~ough this cons_i~ts a lmost entirely an obJt·rver who is the mo;t succ~s;ful in the o:iservatioa of faint of corrections, emendatwns, and add,twns to the con companion; to dou':ile stars, cann') t satisfactorily observe the tents of the nine previous volumes, in which the syste faint markings with which th, plane:'s disc is diversified. -
Ensory a Teacher’S Learning Guide to Multi Sensory LEARNING Improving Literacy by Engaging the Senses
Education A Teacher’s Guide to multisensory Guide to Multi A Teacher’s LEARNING Improving Literacy by Engaging the Senses ow can teachers help students develop the literacy skills that are H necessary for learning and retaining information in any subject? Traditional memory tricks, mnemonic devices, graphic organizers, and A Teacher’s Guide to role-playing do little to turn bored or reluctant students into enthusiastic learners. In A Teacher's Guide to Multisensory Learning: Improving Literacy by Engaging the Senses, Lawrence Baines shows teachers how to engage students through hands-on, visual, auditory, and olfactory stimuli and link the activities sensory multisensory to relevant academic objectives. Throughout the book, you’ll find real classroom examples of how teachers use multisensory learning techniques to help students interact with material more intensely and retain what they learn for longer periods of time. Baines provides a wide variety of engaging Learning lesson plans to keep students motivated, such as LEARNING • Scent of my Soul—helps students learn expository writing through a Improving Literacy by Engaging the Senses series of sensory lessons and encourages them to investigate a subject of infinite interest—themselves! • Between the Ears—develops students’ ability to infer and deduce by working with their own drawings • Film Score—teaches the art of persuasive writing through the emotional appeal of music • Adagio Suite—encourages students to expand their critical thinking through sight, sound, and touch Seventeen additional lessons plans from Baines and experts in the field are complemented with practical assessments and strategies for engaging students’ sense of play. Baines For teachers who are ready to energize their classrooms, this book is an invaluable resource for expanding students' capacity to learn and helping them cultivate essential skills that will last a lifetime. -
Appendix I Lunar and Martian Nomenclature
APPENDIX I LUNAR AND MARTIAN NOMENCLATURE LUNAR AND MARTIAN NOMENCLATURE A large number of names of craters and other features on the Moon and Mars, were accepted by the IAU General Assemblies X (Moscow, 1958), XI (Berkeley, 1961), XII (Hamburg, 1964), XIV (Brighton, 1970), and XV (Sydney, 1973). The names were suggested by the appropriate IAU Commissions (16 and 17). In particular the Lunar names accepted at the XIVth and XVth General Assemblies were recommended by the 'Working Group on Lunar Nomenclature' under the Chairmanship of Dr D. H. Menzel. The Martian names were suggested by the 'Working Group on Martian Nomenclature' under the Chairmanship of Dr G. de Vaucouleurs. At the XVth General Assembly a new 'Working Group on Planetary System Nomenclature' was formed (Chairman: Dr P. M. Millman) comprising various Task Groups, one for each particular subject. For further references see: [AU Trans. X, 259-263, 1960; XIB, 236-238, 1962; Xlffi, 203-204, 1966; xnffi, 99-105, 1968; XIVB, 63, 129, 139, 1971; Space Sci. Rev. 12, 136-186, 1971. Because at the recent General Assemblies some small changes, or corrections, were made, the complete list of Lunar and Martian Topographic Features is published here. Table 1 Lunar Craters Abbe 58S,174E Balboa 19N,83W Abbot 6N,55E Baldet 54S, 151W Abel 34S,85E Balmer 20S,70E Abul Wafa 2N,ll7E Banachiewicz 5N,80E Adams 32S,69E Banting 26N,16E Aitken 17S,173E Barbier 248, 158E AI-Biruni 18N,93E Barnard 30S,86E Alden 24S, lllE Barringer 29S,151W Aldrin I.4N,22.1E Bartels 24N,90W Alekhin 68S,131W Becquerei -
Downloaded for Personal Non-Commercial Research Or Study, Without Prior Permission Or Charge
MacArtney, Adrienne (2018) Atmosphere crust coupling and carbon sequestration on early Mars. PhD thesis. http://theses.gla.ac.uk/9006/ Copyright and moral rights for this work are retained by the author A copy can be downloaded for personal non-commercial research or study, without prior permission or charge This work cannot be reproduced or quoted extensively from without first obtaining permission in writing from the author The content must not be changed in any way or sold commercially in any format or medium without the formal permission of the author When referring to this work, full bibliographic details including the author, title, awarding institution and date of the thesis must be given Enlighten:Theses http://theses.gla.ac.uk/ [email protected] ATMOSPHERE - CRUST COUPLING AND CARBON SEQUESTRATION ON EARLY MARS By Adrienne MacArtney B.Sc. (Honours) Geosciences, Open University, 2013. Submitted in partial fulfilment of the requirements for the degree of Doctor of Philosophy at the UNIVERSITY OF GLASGOW 2018 © Adrienne MacArtney All rights reserved. The author herby grants to the University of Glasgow permission to reproduce and redistribute publicly paper and electronic copies of this thesis document in whole or in any part in any medium now known or hereafter created. Signature of Author: 16th January 2018 Abstract Evidence exists for great volumes of water on early Mars. Liquid surface water requires a much denser atmosphere than modern Mars possesses, probably predominantly composed of CO2. Such significant volumes of CO2 and water in the presence of basalt should have produced vast concentrations of carbonate minerals, yet little carbonate has been discovered thus far. -
In Pdf Format
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Julie Mitchell1* and Philip Christensen1
#1624 Recurring Slope Lineae and Chlorides in the Southern Hemisphere of Mars Julie Mitchell1* and Philip Christensen1 1Arizona State University, 201 E. Orange Mall, Tempe, AZ, 85281 *[email protected] Introduction Results Conclusions • Recurring Slope Lineae (RSL): candidates for Confirmed RSL were mapped at each location listed in Table 1 and as shown in Figure 3. Palikir Crater was the most The lack of chloride signatures collocated with liquid water on the martian surface [1] distinct locale, showing local evidence of chlorides in areas where RSL were most densely located (Figure 4). This RSL in the Southern hemisphere could be the • RSL peak activity during southern summer [1, 2] locale has also shown periodic evidence of ferric iron in the near-infrared [8]. For all RSL, DCS chloride signatures result of one of three scenarios: • RSL active below H O freezing point → brine 2 did not correlate to the presence of RSL on the regional scale. In some cases, such as Triolet Crater, neither local- nor flow? 1. RSL may not contain chlorides, either because • CaCl , MgCl : most likely compounds in brine [3] regional-scale evidence of chlorides was observed (Figure 5). 2 2 they a) are not aqueous flow features or b) are The purpose of this study is to investigate the not chloride-based brines. likelihood that RSL are formed by chloride Nearest Named HiRISE ID THEMIS ID brines. Crater 2. Several locales are dominated by the distinct Palikir ESP_022267_1380 I34263004 steep-slope signature in THEMIS DCS identified by Bandfield [10]; the fact that the Tivat ESP_013624_1335 I17599005 many RSL occur on the steep crater walls Pickering (SW) ESP_022820_1415 I17966002 supports this scenario (Figure 5, right). -
This Article Appeared in a Journal Published by Elsevier. the Attached
(This is a sample cover image for this issue. The actual cover is not yet available at this time.) This article appeared in a journal published by Elsevier. The attached copy is furnished to the author for internal non-commercial research and education use, including for instruction at the authors institution and sharing with colleagues. Other uses, including reproduction and distribution, or selling or licensing copies, or posting to personal, institutional or third party websites are prohibited. In most cases authors are permitted to post their version of the article (e.g. in Word or Tex form) to their personal website or institutional repository. Authors requiring further information regarding Elsevier’s archiving and manuscript policies are encouraged to visit: http://www.elsevier.com/copyright Author's personal copy Aeolian Research 8 (2013) 29–38 Contents lists available at SciVerse ScienceDirect Aeolian Research journal homepage: www.elsevier.com/locate/aeolia Review Article Summary of the Third International Planetary Dunes Workshop: Remote Sensing and Image Analysis of Planetary Dunes, Flagstaff, Arizona, USA, June 12–15, 2012 ⇑ Lori K. Fenton a, , Rosalyn K. Hayward b, Briony H.N. Horgan c, David M. Rubin d, Timothy N. Titus b, Mark A. Bishop e,f, Devon M. Burr g, Matthew Chojnacki g, Cynthia L. Dinwiddie h, Laura Kerber i, Alice Le Gall j, Timothy I. Michaels a, Lynn D.V. Neakrase k, Claire E. Newman l, Daniela Tirsch m, Hezi Yizhaq n, James R. Zimbelman o a Carl Sagan Center at the SETI Institute, 189 Bernardo Ave., Suite 100, Mountain View, CA 94043, USA b United States Geological Survey, Astrogeology Science Center, 2255 N.