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Glossary Glossary
Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts. -
Physical and Chemical Properties of Matrix in Primitive Chondrites Thesis
Open Research Online The Open University’s repository of research publications and other research outputs Physical and Chemical Properties of Matrix in Primitive Chondrites Thesis How to cite: Vaccaro, Epifanio (2017). Physical and Chemical Properties of Matrix in Primitive Chondrites. PhD thesis The Open University. For guidance on citations see FAQs. c 2016 The Author https://creativecommons.org/licenses/by-nc-nd/4.0/ Version: Version of Record Link(s) to article on publisher’s website: http://dx.doi.org/doi:10.21954/ou.ro.0000cc17 Copyright and Moral Rights for the articles on this site are retained by the individual authors and/or other copyright owners. For more information on Open Research Online’s data policy on reuse of materials please consult the policies page. oro.open.ac.uk Physical and chemical properties of matrix in primitive chondrites SEM element map of QUE 99177 matrix Epifanio Vaccaro (MSc Hons. Geological Sciences, Palermo University) The Open University & Natural History Museum, London Supervisors: Natalie Starkey, Ian Franchi, Sara Russell November 2017 This thesis was submitted to The Open University for the degree of Doctor of Philosophy i Abstract The origin and formation of our Solar System is an open research question, which the scientific community is trying to address. In this work was specifically investigated the fine grained matrix which is a mixture of fine-grained materials composed largely of amorphous silicate and sub-micrometre crystals forsterite and enstatite. This is thought to be the remnants of the dust and gas of the protoplanetary disk that allows us to better understand chemical and physical properties of this precursor material. -
Constraining the Evolutionary History of the Moon and the Inner Solar System: a Case for New Returned Lunar Samples
Space Sci Rev (2019) 215:54 https://doi.org/10.1007/s11214-019-0622-x Constraining the Evolutionary History of the Moon and the Inner Solar System: A Case for New Returned Lunar Samples Romain Tartèse1 · Mahesh Anand2,3 · Jérôme Gattacceca4 · Katherine H. Joy1 · James I. Mortimer2 · John F. Pernet-Fisher1 · Sara Russell3 · Joshua F. Snape5 · Benjamin P. Weiss6 Received: 23 August 2019 / Accepted: 25 November 2019 / Published online: 2 December 2019 © The Author(s) 2019 Abstract The Moon is the only planetary body other than the Earth for which samples have been collected in situ by humans and robotic missions and returned to Earth. Scien- tific investigations of the first lunar samples returned by the Apollo 11 astronauts 50 years ago transformed the way we think most planetary bodies form and evolve. Identification of anorthositic clasts in Apollo 11 samples led to the formulation of the magma ocean concept, and by extension the idea that the Moon experienced large-scale melting and differentiation. This concept of magma oceans would soon be applied to other terrestrial planets and large asteroidal bodies. Dating of basaltic fragments returned from the Moon also showed that a relatively small planetary body could sustain volcanic activity for more than a billion years after its formation. Finally, studies of the lunar regolith showed that in addition to contain- ing a treasure trove of the Moon’s history, it also provided us with a rich archive of the past 4.5 billion years of evolution of the inner Solar System. Further investigations of samples returned from the Moon over the past five decades led to many additional discoveries, but also raised new and fundamental questions that are difficult to address with currently avail- able samples, such as those related to the age of the Moon, duration of lunar volcanism, the Role of Sample Return in Addressing Major Questions in Planetary Sciences Edited by Mahesh Anand, Sara Russell, Yangting Lin, Meenakshi Wadhwa, Kuljeet Kaur Marhas and Shogo Tachibana B R. -
Supporting Information (SI) Appendix Persistence and Origin of the Lunar Core Dynamo
Supporting Information Corrected July 05, 2013 Supporting Information (SI) Appendix Persistence and origin of the lunar core dynamo Clément Suavet, Benjamin P. Weiss, William S. Cassata, David L. Shuster, Jérôme Gattacceca, Lindsey Chan, Ian Garrick-Bethell, James W. Head, Timothy L. Grove, and Michael D. Fuller 1. Previous paleomagnetic studies of high-K mare basalts During the Apollo era, paleomagnetic studies were carried out on at least six high-K basalts: 10017, 10022, 10024, 10049, 10057, and 10069. 10022 was thermally demagnetized (49), but the lack of published directional data precludes the identification of magnetization components. 10024 was found to carry an intense soft overprint and a higher coercivity component blocked from 5 to at least 50 mT, but spurious demagnetization effects prevented a detailed characterization of the latter (1). Similarly, 10057 was found to contain a soft overprint and a higher coercivity component from 9 to >18 mT, but a high-quality paleointensity value could not be obtained because the sample was not fully demagnetized (50, 51). 10069 was only demagnetized to <7 mT before thermal demagnetization was attempted, at which point the sample irreversibly altered (49). Because so many lunar rocks have poor magnetic recording properties (52), we decided to focus on two samples that appeared to be unusually well-behaved during previous AF demagnetization experiments: 10017 and 10049 (Fig. S1 and Table S6). The natural remanent magnetization (NRM) of 10017 was studied by three groups (13-16). Initial reports identified a directionally stable magnetization component during alternating field (AF) demagnetization of subsample 10017,64 up to 50 mT (13). -
Lunar Impact Basins Revealed by Gravity Recovery and Interior
Lunar impact basins revealed by Gravity Recovery and Interior Laboratory measurements Gregory Neumann, Maria Zuber, Mark Wieczorek, James Head, David Baker, Sean Solomon, David Smith, Frank Lemoine, Erwan Mazarico, Terence Sabaka, et al. To cite this version: Gregory Neumann, Maria Zuber, Mark Wieczorek, James Head, David Baker, et al.. Lunar im- pact basins revealed by Gravity Recovery and Interior Laboratory measurements. Science Advances , American Association for the Advancement of Science (AAAS), 2015, 1 (9), pp.e1500852. 10.1126/sci- adv.1500852. hal-02458613 HAL Id: hal-02458613 https://hal.archives-ouvertes.fr/hal-02458613 Submitted on 26 Jun 2020 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. RESEARCH ARTICLE PLANETARY SCIENCE 2015 © The Authors, some rights reserved; exclusive licensee American Association for the Advancement of Science. Distributed Lunar impact basins revealed by Gravity under a Creative Commons Attribution NonCommercial License 4.0 (CC BY-NC). Recovery and Interior Laboratory measurements 10.1126/sciadv.1500852 Gregory A. Neumann,1* Maria T. Zuber,2 Mark A. Wieczorek,3 James W. Head,4 David M. H. Baker,4 Sean C. Solomon,5,6 David E. Smith,2 Frank G. -
GRAIL Gravity Observations of the Transition from Complex Crater to Peak-Ring Basin on the Moon: Implications for Crustal Structure and Impact Basin Formation
Icarus 292 (2017) 54–73 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus GRAIL gravity observations of the transition from complex crater to peak-ring basin on the Moon: Implications for crustal structure and impact basin formation ∗ David M.H. Baker a,b, , James W. Head a, Roger J. Phillips c, Gregory A. Neumann b, Carver J. Bierson d, David E. Smith e, Maria T. Zuber e a Department of Geological Sciences, Brown University, Providence, RI 02912, USA b NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA c Department of Earth and Planetary Sciences and McDonnell Center for the Space Sciences, Washington University, St. Louis, MO 63130, USA d Department of Earth and Planetary Sciences, University of California, Santa Cruz, CA 95064, USA e Department of Earth, Atmospheric and Planetary Sciences, MIT, Cambridge, MA 02139, USA a r t i c l e i n f o a b s t r a c t Article history: High-resolution gravity data from the Gravity Recovery and Interior Laboratory (GRAIL) mission provide Received 14 September 2016 the opportunity to analyze the detailed gravity and crustal structure of impact features in the morpho- Revised 1 March 2017 logical transition from complex craters to peak-ring basins on the Moon. We calculate average radial Accepted 21 March 2017 profiles of free-air anomalies and Bouguer anomalies for peak-ring basins, protobasins, and the largest Available online 22 March 2017 complex craters. Complex craters and protobasins have free-air anomalies that are positively correlated with surface topography, unlike the prominent lunar mascons (positive free-air anomalies in areas of low elevation) associated with large basins. -
From the President
Supplement to Meteoritics & Planetary Science, vol. 52, no. 11 The Meteoritical Society Newsletter (November 2017) A report of the business carried out by The Society over the past year, edited by Michael K. Weisberg, Secretary. IN THIS ISSUE From the President Important reminders Annual meetings Please renew your membership before Dec From the Treasurer 15 as the society has to pay the costs of From the Endowment Committee mailing late reminders. Members renewing Publications reports after March 31 incur a $15 surcharge and MAPS GCA risk missing issues of MAPS. You can renew Elements online at From the Nomenclature Committee http://metsoc.meteoriticalsociety.net. From the Membership Committee Nominate your colleagues and students for Awards and honors awards. Nominations for Fellows will be Call for nominations New Fellows to be elected considered this year. Deadlines are in From the Secretary January. See the Awards section for details. Election of new Council Proposals to host the 2022 MetSoc meeting are due in March. Please contact the secretary for procedures. FROM THE PRESIDENT President’s Report membership, and increasingly the commitment of an individual to take ownership of running our Meeting. The annual newsletter provides the President an I can say from experience that this is a somewhat opportunity to reflect on matters of interest to Society daunting task, but for those of us who have done it, it Members. First off I would like to thank Past has been a complete privilege and the memories President Mike Zolensky for all his hard work in generated go far beyond science, but are more akin to keeping the Society moving forward. -
Science Concept 3: Key Planetary
Science Concept 6: The Moon is an Accessible Laboratory for Studying the Impact Process on Planetary Scales Science Concept 6: The Moon is an accessible laboratory for studying the impact process on planetary scales Science Goals: a. Characterize the existence and extent of melt sheet differentiation. b. Determine the structure of multi-ring impact basins. c. Quantify the effects of planetary characteristics (composition, density, impact velocities) on crater formation and morphology. d. Measure the extent of lateral and vertical mixing of local and ejecta material. INTRODUCTION Impact cratering is a fundamental geological process which is ubiquitous throughout the Solar System. Impacts have been linked with the formation of bodies (e.g. the Moon; Hartmann and Davis, 1975), terrestrial mass extinctions (e.g. the Cretaceous-Tertiary boundary extinction; Alvarez et al., 1980), and even proposed as a transfer mechanism for life between planetary bodies (Chyba et al., 1994). However, the importance of impacts and impact cratering has only been realized within the last 50 or so years. Here we briefly introduce the topic of impact cratering. The main crater types and their features are outlined as well as their formation mechanisms. Scaling laws, which attempt to link impacts at a variety of scales, are also introduced. Finally, we note the lack of extraterrestrial crater samples and how Science Concept 6 addresses this. Crater Types There are three distinct crater types: simple craters, complex craters, and multi-ring basins (Fig. 6.1). The type of crater produced in an impact is dependent upon the size, density, and speed of the impactor, as well as the strength and gravitational field of the target. -
Constraining the Evolutionary History of the Moon and the Inner Solar System: a Case for New Returned Lunar Samples
Constraining the Evolutionary History of the Moon and the Inner Solar System: A Case for New Returned Lunar Samples The MIT Faculty has made this article openly available. Please share how this access benefits you. Your story matters. Citation Tartèse, Romain, et al. "Constraining the Evolutionary History of the Moon and the Inner Solar System: A Case for New Returned Lunar Samples." Space Science Reviews, 215 (December 2019): 54. © 2019, The Author(s). As Published http://dx.doi.org/10.1007/s11214-019-0622-x Publisher Springer Science and Business Media LLC Version Final published version Citable link https://hdl.handle.net/1721.1/125329 Terms of Use Creative Commons Attribution 4.0 International license Detailed Terms https://creativecommons.org/licenses/by/4.0/ Space Sci Rev (2019) 215:54 https://doi.org/10.1007/s11214-019-0622-x Constraining the Evolutionary History of the Moon and the Inner Solar System: A Case for New Returned Lunar Samples Romain Tartèse1 · Mahesh Anand2,3 · Jérôme Gattacceca4 · Katherine H. Joy1 · James I. Mortimer2 · John F. Pernet-Fisher1 · Sara Russell3 · Joshua F. Snape5 · Benjamin P. Weiss6 Received: 23 August 2019 / Accepted: 25 November 2019 / Published online: 2 December 2019 © The Author(s) 2019 Abstract The Moon is the only planetary body other than the Earth for which samples have been collected in situ by humans and robotic missions and returned to Earth. Scien- tific investigations of the first lunar samples returned by the Apollo 11 astronauts 50 years ago transformed the way we think most planetary bodies form and evolve. Identification of anorthositic clasts in Apollo 11 samples led to the formulation of the magma ocean concept, and by extension the idea that the Moon experienced large-scale melting and differentiation. -
Exploring the Bimodal Solar System Via Sample Return from the Main Asteroid Belt: the Case for Revisiting Ceres
Space Sci Rev (2020) 216:59 https://doi.org/10.1007/s11214-020-00671-0 Exploring the Bimodal Solar System via Sample Return from the Main Asteroid Belt: The Case for Revisiting Ceres Thomas H. Burbine1 · Richard C. Greenwood2 Received: 24 July 2019 / Accepted: 7 April 2020 © The Author(s) 2020 Abstract Sample return from a main-belt asteroid has not yet been attempted, but appears technologically feasible. While the cost implications are significant, the scientific case for such a mission appears overwhelming. As suggested by the “Grand Tack” model, the struc- ture of the main belt was likely forged during the earliest stages of Solar System evolution in response to migration of the giant planets. Returning samples from the main belt has the potential to test such planet migration models and the related geochemical and isotopic concept of a bimodal Solar System. Isotopic studies demonstrate distinct compositional differences between samples be- lieved to be derived from the outer Solar System (CC or carbonaceous chondrite group) and those that are thought to be derived from the inner Solar System (NC or non-carbonaceous group). These two groups are separated on relevant isotopic variation diagrams by a clear compositional gap. The interface between these two regions appears to be broadly coinci- dent with the present location of the asteroid belt, which contains material derived from both groups. The Hayabusa mission to near-Earth asteroid (NEA) (25143) Itokawa has shown what can be learned from a sample-return mission to an asteroid, even with a very small amount of sample. One scenario for main-belt sample return involves a spacecraft launching a projec- tile that strikes an object and flying through the debris cloud, which would potentially allow multiple bodies to be sampled if a number of projectiles are used on different asteroids. -
Moon Clementine Topographic Maps
GEOLOGIC INVESTIGATIONS SERIES I–2769 U.S. DEPARTMENT OF THE INTERIOR Prepared for the LUNAR NEAR SIDE AND FAR SIDE HEMISPHERES U.S. GEOLOGICAL SURVEY NORTH NATIONAL AERONAUTICS AND SPACE ADMINISTRATION NORTH SHEET 1 OF 3 90° 90° 80° . 80° 80° 80° Peary Hermite Nansen Byrd Rozhdestvenskiy 70° 70° Near Side Far Side 70° 70° Hemisphere Hemisphere Plaskett Pascal . Petermann . Poinsot . Cremona . Scoresby v Hayn SHEET 1 . Milankovic 60° Baillaud 60° 60° Schwarzschild . Mezentsev 60° . Seares Ricco Meton Bel'kovich . Philolaus Bel'kovich . Karpinskiy . Hippocrates Barrow MARE Roberts . Poczobutt Xenophanes Pythagoras HUMBOLDTIANUM . Kirkwood Arnold West East Gamow Volta Strabo Stebbins 50° . 50° Hemisphere Hemisphere 50° Compton 50° Sommerfeld Babbage J. Herschel W. Bond . Kane De La Avogadro . South Rue Emden . Coulomb Galvani SHEET 2 Olivier Tikhov Birkhoff Endymion . MARE FR . Störmer IG O . von Rowland Harpalus R Békésy . IS Sarton 40° IS 40° 40° . Chappell . Stefan 40° . Mercurius Carnot OR Lacus North South Fabry . Millikan Wegener . Plato Tempor Hemisphere Hemisphere D'Alembert . Paraskevopoulos Bragg Ju ra . Aristoteles is Atlas . Schlesinger SINUS R s Montes . Slipher Wood te Harkhebi n Vallis Alpes . Montgolfier o SHEET 3 SINUS Lacus Hercules Landau Nernst M H. G. Campbell Mons . Bridgman Alpes Gauss Wells Rümker . Mortis INDEX . Vestine IRIDUM Eudoxus Messala . Cantor Ley Lorentz Wiener Frost 30° 30° 30° Szilard . 30° LA . Von Neumann CUS SOMNIOR . Kurchatov Charlier Hahn Maxwell . Appleton . Gadomski MARE UM Laue la Joliot o Montes Caucasus . Bartels ric . Aristillus Seyfert . Kovalevskaya . Russell Ag IMBRIUM . Posidonius tes Shayn n . Larmor o Cleomedes Plutarch . Cockcroft . M Montes . Berkner O Mare Struve er A . -
Audit Com) Hasnaa Chennaoui (Initiative for Planetary and Space Sciences in Africa)
Meteoritical Society Council Meeting Invitees Meteoritical Society Council Meeting 12:00 to 5:00 pm, Sunday, July 23, 2017 Stiha room in the La Fonda hotel Santa Fe, NM Past President Invitee Michael Zolensky Council Members Invitees Trevor Ireland (Pres.) Caroline Smith Mini Wadhwa (VP) Keiko Nakamura-Messenger Candace Kohl (Treas.) Christine Floss Mike Weisberg (Sec.) Maria Eugenia Varela Catherine Corrigan (and Elements) Francois Robert Mario Trieloff Pierre Rochette Council Member Regrets Maria Eugenia Varela Keiko Nakamura-Messenger Guests Invitees Cecile Engrand (PubCom) Tim Jull (MaPS) Lydia Hallis (MetSoc 2020 Glasgow) Fiona Sarne (Wiley) Jeff Grossman (NASA report) Karen Ziegler (MetSoc 2017) Laurence Garvie (NomCom) Marc Norman (GCA) Marina Ivanova (MetSoc 2018, Moscow) Yoshi Yurimoto (2019 meeting) Sara Russell (Leonard Medal) Liz Canuel (JPC) Tasha Dunn (McKay Award) Kate Hibbert (Elsevier) Erin Walton (Membership/Service Award) Uwe Reimold (Berlin, EC) Alex Deutsch (Barringer Award) Beda Hofmann (Audit Com) Hasnaa Chennaoui (Initiative for Planetary and Space Sciences in Africa) Guest Regrets Marc Norman (GCA) Beda Hofmann (Audit Com) Alex Deutsch (Barringer Award) Laurence Garvie (NomCom) Kate Hibbert (Elsevier) Cecile Engrand (PubCom) Lydia Hallis (MetSoc 2020 Glasgow) Liz Canuel (JPC) 1 0 Welcome and introductions Ireland 12:00 05 1. Minutes last Council Meeting Weisberg 12:05 05 2. President’s report Ireland 12:10 05 3. Secretary’s report (vote) Weisberg 12:15 05 4. Treasurer’s Report (vote) Kohl 12:20 15 5. Audit Committee 12:35 05 6. Awards 6.1 Leonard Medal (+ Nier Prize) (closed vote) Russell 12:40 10 6.2 Barringer Award (closed vote) 12:50 10 7.