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Olivine and Pyroxene from the Mantle of Asteroid 4 Vesta ∗ Nicole G
Earth and Planetary Science Letters 418 (2015) 126–135 Contents lists available at ScienceDirect Earth and Planetary Science Letters www.elsevier.com/locate/epsl Olivine and pyroxene from the mantle of asteroid 4 Vesta ∗ Nicole G. Lunning a, , Harry Y. McSween Jr. a,1, Travis J. Tenner b,2, Noriko T. Kita b,3, Robert J. Bodnar c,4 a Department of Earth and Planetary Sciences and Planetary Geosciences Institute, University of Tennessee, Knoxville, TN 37996, USA b Department of Geosciences, University of Wisconsin, Madison, WI 53706, USA c Department of Geosciences, Virginia Tech, Blacksburg, VA 24061, USA a r t i c l e i n f o a b s t r a c t Article history: A number of meteorites contain evidence that rocky bodies formed and differentiated early in our solar Received 25 September 2014 system’s history, and similar bodies likely contributed material to form the planets. These differentiated Received in revised form 25 February 2015 rocky bodies are expected to have mantles dominated by Mg-rich olivine, but direct evidence for such Accepted 25 February 2015 mantles beyond our own planet has been elusive. Here, we identify olivine fragments (Mg# = 80–92) in Available online 17 March 2015 howardite meteorites. These Mg-rich olivine fragments do not correspond to an established lithology Editor: T. Mather in the howardite–eucrite–diogenite (HED) meteorites, which are thought to be from the asteroid 4 Keywords: Vesta; their occurrence in howardite breccias, combined with diagnostic oxygen three-isotope signatures planetary formation and minor element chemistry, indicates they are vestan. -
Assessment of the Mesosiderite-Diogenite Connection and an Impact Model for the Genesis of Mesosiderites
45th Lunar and Planetary Science Conference (2014) 2554.pdf ASSESSMENT OF THE MESOSIDERITE-DIOGENITE CONNECTION AND AN IMPACT MODEL FOR THE GENESIS OF MESOSIDERITES. T. E. Bunch1,3, A. J. Irving2,3, P. H. Schultz4, J. H. Wittke1, S. M. Ku- ehner2, J. I. Goldstein5 and P. P. Sipiera3,6 1Dept. of Geology, SESES, Northern Arizona University, Flagstaff, AZ 86011 ([email protected]), 2Dept. of Earth & Space Sciences, University of Washington, Seattle, WA, 3Planetary Studies Foundation, Galena, IL, 4Dept. of Geological Sciences, Brown University, Providence, RI, 5Dept. of Geolo- gy, University of Massachusetts, Amherts, MA, 6Field Museum of Natural History, Chicago, IL. Introduction: Among well-recognized meteorite 34) is the most abundant silicate mineral and in some classes, the mesosiderites are perhaps the most com- clasts contains inclusions of FeS, tetrataenite, merrillite plex and petrogenetically least understood. Previous and silica. Three of the ten norite clasts contain a few workers have contributed important information about tiny grains of olivine (Fa24-32). A single, fine-grained “classic” falls and Antarctic finds, and have proposed breccia clast was found in NWA 5312 (see Figure 2). several different models for mesosiderite genesis [1]. Unlike the case of pallasites, the co-occurrence of met- al and silicates (predominantly orthopyroxene and cal- cic plagioclase) in mesosiderites is inconsistent with a single-stage “igneous” history, and instead seems to demand admixture of at least two separate compo- nents. Here we review the models in light of detailed ex- amination of multiple specimens from a very large mesosiderite strewnfield in Northwest Africa. Many specimens (totaling at least 80 kilograms) from this area (probably in Algeria) have been classified sepa- rately by us and others; however, in most cases the Figure 1. -
Meteorite Dunite Breccia Mil 03443: a Probable Crustal Cumulate Closely Related to Diogenites from the Hed Parent Asteroid
METEORITE DUNITE BRECCIA MIL 03443: A PROBABLE CRUSTAL CUMULATE CLOSELY RELATED TO DIOGENITES FROM THE HED PARENT ASTEROID. David W Mittlefehldt, Astromateri- als Research Office, NASA/Johnson Space Center, Houston, Texas, USA, ([email protected]). Introduction: There are numerous types of differ- Metal is very rare, and occurs as grains a few microns entiated meteorites, but most represent either the crusts in size associated with troilite. or cores of their parent asteroids. Ureilites, olivine- pyroxene-graphite rocks, are exceptions; they are man- tle restites [1]. Dunite is expected to be a common mantle lithology in differentiated asteroids. In particu- lar, models of the eucrite parent asteroid contain large volumes of dunite mantle [2-4]. Yet dunites are very rare among meteorites, and none are known associated with the howardite, eucrite, diogenite (HED) suite. Spectroscopic measurements of 4 Vesta, the probable HED parent asteroid, show one region with an olivine signature [5] although the surface is dominated by ba- saltic and orthopyroxenitic material equated with eucrites and diogenites [6]. One might expect that a small number of dunitic or olivine-rich meteorites might be delivered along with the HED suite. The 46 gram meteoritic dunite MIL 03443 (Fig. 1) Figure 2. BSE image of MIL 03443 showing its gen- was recovered from the Miller Range ice field of Ant- eral fragmental breccia texture, and primary texture arctica. This meteorite was tentatively classified as a between olivine, orthopyroxene and chromite. mesosiderite because large, dunitic clasts are found in this type of meteorite, but it was noted that MIL 03443 could represent a dunite sample of the HED suite [7]. -
JEM-EUSO: Meteor and Nuclearite Observations
Exp Astron DOI 10.1007/s10686-014-9375-4 ORIGINAL ARTICLE JEM-EUSO: Meteor and nuclearite observations M. Bertaina A. Cellino F. Ronga The JEM-EUSO· Collaboration· · Received: 22 August 2013 / Accepted: 24 February 2014 ©SpringerScience+BusinessMediaDordrecht2014 Abstract Meteor and fireball observations are key to the derivation of both the inven- tory and physical characterization of small solar system bodies orbiting in the vicinity of the Earth. For several decades, observation of these phenomena has only been possible via ground-based instruments. The proposed JEM-EUSO mission has the potential to become the first operational space-based platform to share this capabil- ity. In comparison to the observation of extremely energetic cosmic ray events, which is the primary objective of JEM-EUSO, meteor phenomena are very slow, since their typical speeds are of the order of a few tens of km/sec (whereas cosmic rays travel at light speed). The observing strategy developed to detect meteors may also be applied to the detection of nuclearites, which have higher velocities, a wider range of possible trajectories, but move well below the speed of light and can therefore be considered as slow events for JEM-EUSO. The possible detection of nuclearites greatly enhances the scientific rationale behind the JEM-EUSO mission. Keywords Meteors Nuclearites JEM-EUSO Space detectors · · · M. Bertaina (!) Dipartimento di Fisica, Universit`adiTorino,INFNTorino,viaP.Giuria1,10125Torino,Italy e-mail: [email protected] A. Cellino (!) INAF-Osservatorio Astrofisico di Torino, Strada Osservatorio 20, 10025 Pino Torinese (TO), Italy e-mail: [email protected] F. Ronga (!) Istituto Nazionale di Fisica Nucleare - Laboratori Nazionali di Frascati, Via E. -
Hydrated Minerals and Carbonaceous Chondrite Fragments in Lohawat Howardite: Astrobiological Implications: M
Astrobiology Science Conference 2015 (2015) 7069.pdf HYDRATED MINERALS AND CARBONACEOUS CHONDRITE FRAGMENTS IN LOHAWAT HOWARDITE: ASTROBIOLOGICAL IMPLICATIONS: M. S. Sisodia, A. Basu Sarbadhikari and R. R. Maha- jan. PLANEX, Physical Reasearch Laboratory, Ahmedabad, India (E-mail: [email protected]; [email protected]) Introduction: Presence of hydrated minerals on nebula caused initial melting and subsequent gradual asteroids, which are remnants of the blocks that formed differentiation of these early accreting bodies into the planets of the solar system has great importance for crust, mantle and core [4]. Dawn’s results confirm that deducing the origin of Earth’s water. Asteroid 4 Vesta Vesta is a differentiated protoplanet and that it is a is the parent body of the howardite-eucrite-diogenite parent body of HED meteorites [5]. The presence of (HED) family of the meteorites that have fallen on hydrated minerals on vesta as revealed by Lohawt Earth [1]. Lohawat howardite that fell in India in the howardite is very significant. Howardites originate year 1994 is a heterogeneous breccia composed of va- from the surface of Vesta nad constitute representative riety of mineral and lithic fragments [2]. We report samples from its crust, mantle and core. The low gravi- here optical study of hydrated minerals that we found ty of Vesta induce lower velocities to the impactors in Lohawat howardite and then discuss their astrobio- resulting into incomplete melting of impacting carbo- logical implications. naceous chondrites [6]. Whether these hydrated miner- Petrography of Lohawat howardite: Lohawat als were contributed on the surface of Vesta by carbo- howardite is an assortment of different minerals and naceous chondrites will be revealed by isotope study clasts. -
Howardite-Eucrite-Diogenite) Title PARENT BODY -PARTIAL MELT EXPERIMENTS on DIFFERENTIATION PROCESSES-( Dissertation 全文 )
EVOLUTION OF THE HED (Howardite-Eucrite-Diogenite) Title PARENT BODY -PARTIAL MELT EXPERIMENTS ON DIFFERENTIATION PROCESSES-( Dissertation_全文 ) Author(s) Isobe, Hiroshi Citation Kyoto University (京都大学) Issue Date 1991-03-23 URL http://dx.doi.org/10.11501/3053044 Right Type Thesis or Dissertation Textversion author Kyoto University 学位 申請論文 磯部博志 EVOLUTION OF THE HED (howardite-eucrite-diogenite) PARENT BODY -PARTIAL MELT EXPERIMENTS ON DIFFERENTIATION PROCESSES- Hiroshi ISOBE Department of Environmental Safety Research Japan Atomic Energy Research Institute Tokai, Ibaraki, 319-11, JAPAN CONTENTS Abstract 1 Introduction1 2 Experiments —starting materials and procedures13 2-1 Composition of the starting materials13 2-2 Experimental procedures19 3 Results and interpretation25 3-1 Mineral assemblages of the run products25 3-2 Composition of the melts and minerals34 4 Discussion60 4-1 Melting relations on the 'pseudo-liquidus' diagrams 60 4-2 Fractionation sequence71 4-3 Physical conditions of the solid-liquid separations 78 4-4 Summary of the present evolution model of HEDP-PB96 Acknowledgments98 References99 Appendix 1 Chemistry of HED and pallasite meteorites106 Appendix 2 Tables of compositions of run products116 Abstract Three series of melting experiments with a chondritic material, a eucrite-diogenite mixture, and a eucritic material were carried out using a one atmosphere gas mixing furnace to illustrate liquidus phase relation and chemical compositions of the phases. Locations of an olivine control line, olivine-pyroxene phase boundary -
Carbonaceous Chondrite-Rich Howardites; the Potential for Hydrous Lithologies on the Hed Parent
CARBONACEOUS CHONDRITE-RICH HOWARDITES; THE POTENTIAL FOR HYDROUS LITHOLOGIES ON THE HED PARENT. J. S. Herrin 1,2 , M. E. Zolensky 2, J. A. Cartwright 3, D. W. Mittle- fehldt 2, and D. K. Ross 1,2 . 1ESCG Astromaterials Research Group, Houston, Texas, USA ( [email protected] ), 2NASA Johnson Space Center, Houston, Texas, USA, 3Max Planck Institut für Chemie, Mainz, Germany. Introduction: Howardites, eucrites, and dioge- clasts texturally resembling CM2 up to 7mm occupy- nites, collectively referred to as the “HED’s”, are a ing nearly half of the sample area accompanied 1-5 clan of meteorites thought to represent three different mm subangular impact melt clasts containing relict lithologies from a common parent body. Collectively eucritic fragments. The remaining medium and fine they are the most abundant type of achondrites in terre- fraction of the specimen consists of mm-to-sub-mm strial collections [1]. Eucrites are crustal basalts and angular-to-subrounded eucritic, diogenitic, carbona- gabbros, diogenites are mostly orthopyroxenites and ceous chondrite clasts set in a medium-to-coarse angu- are taken to represent lower crust or upper mantle ma- lar matrix of same materials. The eucrite/diogenite terials, and howardites are mixed breccias containing ratio of identifiable clasts is approximately 50/50. The both lithologies and are generally regarded as derived total modal abundance of visible carbonaceous chon- from the regolith or near-surface. drite fragments is ~60%. The presence of exogenous chondritic material in PRA 04402 is a howardite breccia consisting of howardite breccias has long been recognized [2,3]. As mm-to-sub-mm subrounded-to-subangular diogenite a group, howardites exhibit divergence in bulk chemi- and eucritic clasts in roughly equal proportions set in a stry from what would be produced by mixing of dioge- medium-to-coarse matrix. -
Map of Monuments and Architecture
1 Prague is renowned for its towers, winding streets and buildings from nearly The Loreto Treasure houses a rare collection of liturgical objects from the 16th – 18th home to hidden architectural treasures including the rare Romanesque rotunda 31. Danube House – Karolinská 1, Prague 8, www.danube.cz every period of architecture – from Romanesque rotundas and Gothic cathedrals centuries, the most famous of which is the ”Prague Sun”, a monstrance encrusted with of St. Martin; the neo-Gothic Church of Sts. Peter and Paul, built on medieval Prague’s Karlin district is one of the city’s fastest growing urban areas. Danube to Baroque and Renaissance palaces, to progressive and global award-winning 6,222 diamonds. foundations; the national cemetery, where Antonín Dvořák and other notable House is the first building in the emerging River City neighborhood. The building, modern architecture. personalities were laid to rest; and underground casemates housing the originals with its triangular footprint, resembles a giant ship; also of special note is its 10. Strahov Monastery (Strahovský klášter) – Strahovské nádvoří 1, Prague 1, of some Baroque statues from the Charles Bridge. monumental glass atrium. The design for the project came from the American Our map offers a selection of the most interesting architectural sights in Prague. www.strahovskyklaster.cz studio Kohn Pedersen Fox. sale for Not This Premonstratensian monastery was founded in 1140. The complex includes 21 Church of the Most Sacred Heart of Our Lord (Kostel Nejsvětějšího Srdce edition First Total cost: 500,000 pcs 500,000 cost: Total Plan your route according to your mood and discover Prague today – beautiful, the Church of the Assumption of the Blessed Virgin Mary (1743 – 1752); the rare Páně) – náměstí Jiřího z Poděbrad, Prague 3, www.srdcepane.cz 32 Mainpoint Karlín – Pobřežní 21, Prague 8, www.mainpointkarlin.cz 2014 Prague seductive, magical.. -
Fr. Arturo Sosa Superior General Father Arturo Sosa
Fr. Arturo Sosa SUPERIOR GENERAL Father Arturo Sosa Father Arturo Sosa was born in 31 Caracas, Venezuela on 12 Novem- ber 1948. Until his election, Fa- ther Sosa was Delegate for Inter- provincial Houses of the Society in Rome, as well as serving on the General Council as a Counsellor. He obtained a licentiate in philo- sophy from the Andrés Bello Ca- tholic University in 1972. He later obtained a doctorate in Political Science from the Central Univer- sity of Venezuela, in 1990. Father Sosa speaks Spanish, Ita- lian, English, and understands French. In 2008, during General Congregation 35, Father General Adolfo Nicolás appointed FFather Arturo Sosa as General Counsellor, based in Venezuela. In 2014, Father Sosa joi- ned the General Curia community and took on the role of Delegate for Interprovincial Roman Houses of the Society of Jesus in Rome, which include the Pontifical Gregorian University, the Pontifical Biblical Institute, the Pontifical Oriental Institute, the Vatican Observatory, Civiltà Cattolica, as well as international Jesuit colleges in Rome. Between 1996 and 2004, Father Sosa was provincial superior of the Jesuits in Venezuela. Before that, he was the province coordinator for the social apostolate, during which time he was also director of Gumilla Social Center, a center for research and social action for the Jesuits in Venezuela. Father Arturo Sosa has dedicated a large part of his life to research and teaching. He has held different positions in academia. He has been a professor and member of the Council of the Andrés Bello Catholic Foundation and Rector of the Catholic University of Táchira. -
1950 Da, 205, 269 1979 Va, 230 1991 Ry16, 183 1992 Kd, 61 1992
Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. Burbine Index More Information 356 Index 1950 DA, 205, 269 single scattering, 142, 143, 144, 145 1979 VA, 230 visual Bond, 7 1991 RY16, 183 visual geometric, 7, 27, 28, 163, 185, 189, 190, 1992 KD, 61 191, 192, 192, 253 1992 QB1, 233, 234 Alexandra, 59 1993 FW, 234 altitude, 49 1994 JR1, 239, 275 Alvarez, Luis, 258 1999 JU3, 61 Alvarez, Walter, 258 1999 RL95, 183 amino acid, 81 1999 RQ36, 61 ammonia, 223, 301 2000 DP107, 274, 304 amoeboid olivine aggregate, 83 2000 GD65, 205 Amor, 251 2001 QR322, 232 Amor group, 251 2003 EH1, 107 Anacostia, 179 2007 PA8, 207 Anand, Viswanathan, 62 2008 TC3, 264, 265 Angelina, 175 2010 JL88, 205 angrite, 87, 101, 110, 126, 168 2010 TK7, 231 Annefrank, 274, 275, 289 2011 QF99, 232 Antarctic Search for Meteorites (ANSMET), 71 2012 DA14, 108 Antarctica, 69–71 2012 VP113, 233, 244 aphelion, 30, 251 2013 TX68, 64 APL, 275, 292 2014 AA, 264, 265 Apohele group, 251 2014 RC, 205 Apollo, 179, 180, 251 Apollo group, 230, 251 absorption band, 135–6, 137–40, 145–50, Apollo mission, 129, 262, 299 163, 184 Apophis, 20, 269, 270 acapulcoite/ lodranite, 87, 90, 103, 110, 168, 285 Aquitania, 179 Achilles, 232 Arecibo Observatory, 206 achondrite, 84, 86, 116, 187 Aristarchus, 29 primitive, 84, 86, 103–4, 287 Asporina, 177 Adamcarolla, 62 asteroid chronology function, 262 Adeona family, 198 Asteroid Zoo, 54 Aeternitas, 177 Astraea, 53 Agnia family, 170, 198 Astronautica, 61 AKARI satellite, 192 Aten, 251 alabandite, 76, 101 Aten group, 251 Alauda family, 198 Atira, 251 albedo, 7, 21, 27, 185–6 Atira group, 251 Bond, 7, 8, 9, 28, 189 atmosphere, 1, 3, 8, 43, 66, 68, 265 geometric, 7 A- type, 163, 165, 167, 169, 170, 177–8, 192 356 © in this web service Cambridge University Press www.cambridge.org Cambridge University Press 978-1-107-09684-4 — Asteroids Thomas H. -
Ludmila Mašková Et Al., (Presented by Jiří Smolík), Institute of Chemical
BEHAVIOUR OF INDOOR COARSE PARTICLES IN THE LIBRARY Ludmila Mašková, Jiří Smolík, Tereza Trávníčková, Jaromír Hlavica Institute of Chemical Process Fundamentals of the CAS INTRODUCTION In the period 2008-2010 we performed detailed indoor air quality measurements in an old Baroque Library Hall (BLH), located in Clementinum historical complex in Prague. INTRODUCTION Founded in 1232, the Clementinum is one of the largest building complexes in Europe. Since 1930 it is currently in use as the National Library of the Czech Republic. BAROQUE LIBRARY HALL • 21 000 books • 100 – 200 visitors • Naturally ventilated • Area 430 m2 • Volume 4500 m3 KEY QUESTION Effect of visitors on the indoor air quality? MEASUREMENTS 1 week 2008 3 intensive campaigns: spring, summer, winter 2009 Indoor and outdoor • Airborne particulate matter (PM) • Determination of chemical composition • Temporal variation • Spatial variation of indoor PM • Gaseous pollutants • Climatic parameters MEASUREMENTS PREVIOUS ANALYSIS ) 3 400 350 Winter indoor APS 300 Winter outdoor APS 250 200 150 100 50 Numberconcentration (#/cm 0 24.11.2009 26.11.2009 27.11.2009 28.11.2009 30.11.2009 01.12.2009 Date ) 3 25000 Winter indoor SMPS 20000 Winter outdoor SMPS 15000 10000 5000 Numberconcentration (#/cm 0 24.11.2009 26.11.2009 27.11.2009 28.11.2009 30.11.2009 01.12.2009 Date Similar behaviour found in all 3 periods DYNAMIC MASS BALANCE MODEL dC S in PaC aC kC dt out in in V -3 Cin indoor particle concentration (cm ) -3 Cout outdoor particle concentration (cm ) t time (min-1) V volume -
Citizen Science with the Desert Fireball Network
EPSC Abstracts Vol. 13, EPSC-DPS2019-1178-2, 2019 EPSC-DPS Joint Meeting 2019 c Author(s) 2019. CC Attribution 4.0 license. Fireballs in the Sky: Citizen Science with the Desert Fireball Network Brian Day (1), Phil Bland (2), Renae Sayers (2) (1) NASA Solar System Exploration Research Virtual Institute. NASA Ames Research Center. Moffett Field, CA, USA. ([email protected]) (2) Curtin University. Perth, WA, Australia. ([email protected]) ([email protected]) Abstract Curtin University in Western Australia. It is led by Phil Bland of Curtin University. Fireballs in the Sky is an innovative Australian citizen science program that connects the public with 2. Observatory Design and Network the research of the Desert Fireball Network (DFN). The observatories are fully autonomous intelligent This research aims to understand the early workings imaging systems, capable of operating for 12 months of the solar system, and Fireballs in the Sky invites in a harsh environment without maintenance, and people around the world to learn about this science, storing all imagery collected over that period. Each contributing fireball sightings via a user-friendly observatory uses a 36MP consumer DSLR camera augmented reality mobile app. Tens of thousands of equipped with a fisheye lens providing spatial people have downloaded the app world-wide and precision of approximately one arcminute. The participated in the science of meteoritics. The DSLR is modified with a liquid crystal (LC) shutter. Fireballs in the Sky app allows users to get involved The LC shutter is used to break the fire-ball trail into with the Desert Fireball Network research, dashes for velocity calculation, after triangulation.