DOCSLIB.ORG

M E T E O R I T O S 05. Septiembre 2017. 1 MUSEO CANARIO DE

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
M E T E O R I T O S 05. Septiembre 2017. 1 MUSEO CANARIO DE See discussions, stats, and author profiles for this publication at: https://www.researchgate.net/publication/346699613 METEORITOS num. 5. Septiembre-octubre 2017. Book · December 2020 CITATIONS READS 0 32 1 author: José García LPMCM METEORITES LAB 34 PUBLICATIONS 0 CITATIONS SEE PROFILE Some of the authors of this publication are also working on these related projects: Revista METEORITOS (ISSN 2605-2946) View project Cuando tocamos la Luna (When we touch the Moon) View project All content following this page was uploaded by José García on 08 December 2020. The user has requested enhancement of the downloaded file. M E T E O R I T O S 05. Septiembre 2017. 1 MUSEO CANARIO DE METEORITOS M E T E O R I T O S 05. Septiembre 2017. AVISO LEGAL; Museo Canario de Meteoritos no se Rogamos a nuestros lectores y colaboradores, que para acelerar la posible responsabiliza de la opinión ni de los contenidos de publicación de los trabajos que nos deseen hacer llegar, pueden enviarlos a los artículos firmados, ni mantiene correspondencia la dirección del MCM a través del correo electrónico que aparece en los sobre los artículos no solicitados. contactos; [email protected] Museo Canario de Meteoritos se reserva todos los Todos los trabajos serán revisados por el equipo técnico, pero no se derechos de reproducción total o parcial por modificará su contenido, salvo autorización expresa de su autor. cualquier medio gráfico o electrónico del contenido Más información, suscripciones, colaboración, etc, en nuestra página web de METEORITOS. Impreso en Holanda, Printed in The www.museocanariodemeteoritos.com o a través de las redes sociales en Netherlands. © MCM, 2017. www.facebook.com/museocanariodemeteoritos Revista bimensual editada por el Museo Canario de Meteoritos. P.O. Box 3. Agüimes 35260. Las Palmas, España. Dirección técnica; José García. ISSN 2605-2946 Depósito Legal; No necesario. Política de Publicidad; Si desea que su empresa aparezca en esta publicación, como anunciante o como patrocinador, puede ponerse en contacto con nosotros. El alcance medio de la edición digital oscila entre 4000 y 6000 lectores de todo el mundo y habla hispana. Puede solicitar condiciones para su publicidad a nuestro correo electrónico. Todas las ediciones están disponibles en todo momento a través de nuestra página web. Números anteriores 2 MUSEO CANARIO DE METEORITOS M E T E O R I T O S 05. Septiembre 2017. EDITORIAL; NWA 11397 NUEVO METEORITO DEL MCM. Encaramos el número 5 de la revista, y con Museo Canario de Meteoritos, además de ello entramos de pleno en la recta final de las ser una entidad dedicada a la investigación y publicaciones para este año. Septiembre da inicio al protección de rocas del espacio, también alberga nuevo curso, y por supuesto desde el Museo una importante colección de fósiles de diferentes comenzamos otro año más la labor divulgativa de la eras geológicas, por ello en este número, les ciencia, y lo hacemos además con importantes presentamos un artículo especial dedicado a los novedades. Después de un verano repleto de fósiles que se conservan en las colecciones. actividades, es momento de retomar las agendas para el curso que empieza. Éstos mismos fósiles son los que en muchas ocasiones visitan los centros escolares con motivo Julio y Agosto han sido meses interesantes, de diversas actividades relacionadas con el tema. entre otras cosas porque llevamos a cabo por tercer Los alumnos disfrutan sobremanera observando de año consecutivo la Expedición Sáhara (Edición cerca estas piezas, y conociendo cuándo vivieron, 2017), una expedición que probablemente se cuándo se extinguieron y a qué nuevas especies completará con próximas actividades anexas. dieron origen. En este número de METEORITOS les De nuevo continuamos ofreciéndoles la contaremos cómo ha sido el desarrollo de la primera cuarta parte del dossier “Meteoritos en España”, de quedada astronómica organizada por el museo para nuestro compañero Victoriano Canales, en el que la observación de las Perseidas desde la Isla de estamos ofreciendo la información sobre los Gran Canaria. Un evento multitudinario que meteoritos que han tocado suelo en nuestro país. lanzamos como experiencia piloto. Y es que la Estamos deseando de corazón que el número famosa lluvia de estrellas del verano ha sido todo un 5 de la revista sea del agrado de todos vosotros. acontecimiento que se unió a la observación lunar levantando sobre el horizonte del mar. La investigación científica de meteoritos ha avanzado, como no podía ser de otra forma, por lo que les traemos algunas novedades acaecidas, ya que en julio se presentó a The Meteoritical Society José García. Director del MCM. un nuevo meteorito, que ha sido clasificado como NWA 11397, una eucrita polimíctica. 3 MUSEO CANARIO DE METEORITOS M E T E O R I T O S 05. Septiembre 2017. CONTENIDOS Editorial; NWA 11397 3 Expedición SAHARA 2017 5 Meteoritos y análogos terrestres 11 Retorno al pasado, el legado de las 12 especies extintas. NWA 11397. Nuevo meteorito 20 clasificado por el Museo. MPOD de Agosto. 31 Certificado de Excelencia TripAdvisor 32 para las actividades del MCM. Eclipse Solar 2017. 34 Museo Canario de Meteoritos dispone de servicio de La colección del MCM; Gold Basin. 35 Listado meteoritos recuperados en 2016 37 estudio de meteoritos por técnica petrográfica de luz Tienda del Museo. 51 polarizada. Acoge muestras de rocas encontradas por buscadores que deseen conocer la compatibilidad con meteoritos. M U S E O C A N A R I O D E M E T E O R I T O S www.museocanariodemeteoritos.com Síguenos en Facebook; www.facebook.com/museocanariodemeteoritos TIENDA DE METEORITOS DEL MUSEO; www.tiendameteoritos.blogspot.com Dirección; José García. Apdo Correos 3. Agüimes, 35260 (Las Palmas) España. Miembro de ICOM Museos del Mundo y The Meteoritical Society 4 MUSEO CANARIO DE METEORITOS M E T E O R I T O S 05. Septiembre 2017. EXPEDICIÓN SÁHARA CRÓNICA DE LA EDICIÓN 2017, TERCERA DEL MCM J. García. Director del MCM. de actividades viable, un calendario viable, y se dio luz verde a la publicidad del evento. En honor a la verdad Por tercer año consecutivo, el Museo Canario hay que decir que aunque la acogida de dicha de Meteoritos organiza una nueva edición de la publicidad fue muy positiva, finalmente el equipo Expedición Sáhara. Recordarán que en el número conformado fue reducido, conforme a lo esperado anterior de la revista adelantábamos un completo (personalmente agradezco los grupos no muy artículo sobre las ediciones anteriores, y ahora es numerosos), y dimos comienzo a la etapa de tiempo de contarles cómo ha sido el desarrollo de la formalización de la Expedición. nueva edición. Tuvo lugar la reunión informativa previa la tarde Partió la comitiva al desierto el pasado 13 de del día 30 de junio, en el Cruce de Arinaga, donde nos julio, desde el Aeropuerto de Las Palmas, compuesta reunimos para exponer los pormenores del viaje y las por 9 personas que durante cuatro días dedicaron su condiciones aproximadas en las que se desarrollaría. tiempo al estudio y observación del Sol, astronomía Digo aproximadas porque viajar a Marruecos es toda nocturna y búsqueda de fósiles y meteoritos. una aventura, en la que garantizar al 100% el desarrollo Como todas las ediciones anteriores, de una actividad bajo previa programación, se hace aparecieron escollos desde el principio. Lo típico, que si 100% imposible, y esa sí que es una garantía exacta. hay que variar la fecha o la hora de salida, porque que En el desierto, las cosas van a otro ritmo distinto si ya no hay pasajes suficientes para todo el grupo… al que los occidentales estamos acostumbrados. Y ello Finalmente todo se resolvió favorablemente y partimos. ha quedado patente en todos y cada uno de nosotros al Llegaba nuestro avión al Aeropuerto término de esta experiencia. Internacional Hassan I, de la antigua ciudad española Finalmente, a fecha 4 de julio ya estaba de El Aaiún. Eran las 13:15 horas. Nuestros coches nos conformado todo el equipo, todos estábamos esperaban desde hacía unos minutos, para coordinados gracias a la tecnología, y comenzó la fase trasladarnos en un trip por la ciudad, en la que de reservas. pasaríamos gran parte de la tarde en algunas visitas a antiguos lugares. Establecimos una vez más nuestra base en el Hotel Canalina (www.tarfayahotelcanalina.com), sito en Después de numerosos contratiempos, como Tarfaya, y propiedad de Javier J. Franco, quien también ya es habitual cada vez que se programa una formaba parte de la expedición y fue responsable de la expedición, finalmente pudo establecerse un programa 5 MUSEO CANARIO DE METEORITOS M E T E O R I T O S 05. Septiembre 2017. logística, comidas, permisos y otros asuntos unos días donde el calor y la calima hacían acto de relacionados. Un trabajo meritorio y de agradecer, ya presencia con fuerza. En el mismo disfrutamos de un té que bregar con las gentes del desierto a veces se al tiempo que nos encontramos, unos minutos más convierte en una labor suicida. tarde, con Hamid y Fnidou, que como cada vez que vamos, nos aguardan con interesantes tesoros Llegado el día de partir, nos encontramos todos recuperados de las arenas del desierto. en el Aeropuerto de Gran Canaria a las 11.00 de la mañana del día 13 de julio. Puntuales a la cita, todos Caía la tarde, el calor se iba disipando los miembros del grupo fuimos apareciendo. A título lentamente al ritmo que el Sol caía sobre la costa, personal, el sabor de boca inicial al primer encuentro envuelto en calima. Tomamos rumbo a Tarfaya por la debo decir que fue muy positivo. carretera nacional I. 75 minutos de viaje más tarde, arribábamos a nuestro destino, con un apetito voraz, y Puntual nuestro avión despegó y puntual también deseando de vivir nuevas experiencias.
Load more

Recommended publications
  • New Major and Trace Element Data from Acapulcoite-Lodranite Clan
    52nd Lunar and Planetary Science Conference 2021 (LPI Contrib. No. 2548) 1307.pdf New Major and Trace Element Data from Acapulcoite-Lodranite Clan Meteorites: Evidence for Melt-Rock Reaction Events and Early Collisional Fragmentation of the Parent Body Michael P. Lucas1, Nick Dygert1, Nathaniel R. Miller2, and Harry Y. McSween1, 1Department of Earth & Planetary Sciences, University of Tennessee, Knoxville, [email protected], 2Department of Geological Sciences, Univer- sity of Texas at Austin. Introduction: New major and trace element data illumi- patterns exhibit negative Eu anomalies. REE patterns are nate the magmatic and thermal evolution of the acapul- generally consistent among the three groups, however coite-lodranite parent body (ALPB). We observe major comparison of calculated equilibrium melts for acapulco- and trace element disequilibrium in the acapulcoite and ite and transitional cpx and opx demonstrates disequilib- transitional groups that provide evidence for melt infil- rium partitioning in those samples, especially for light- tration and melt-rock reaction processes. In lodranites, REEs in cpx. In contrast, lodranites are in apparent trace which represent sources of the infiltrating melts, we ob- element equilibrium (Fig 1b). They are depleted in serve rapid cooling from high temperatures (hereafter REE+Y relative to acapulcoite-transitional samples in temps), consistent with collisional fragmentation of the cpx (Fig. 1a), and display consistent REE abundances parent body during differentiation. except NWA 5488, which
    [Show full text]
  • Hf–W Thermochronometry: II. Accretion and Thermal History of the Acapulcoite–Lodranite Parent Body
    Earth and Planetary Science Letters 284 (2009) 168–178 Contents lists available at ScienceDirect Earth and Planetary Science Letters journal homepage: www.elsevier.com/locate/epsl Hf–W thermochronometry: II. Accretion and thermal history of the acapulcoite–lodranite parent body Mathieu Touboul a,⁎, Thorsten Kleine a, Bernard Bourdon a, James A. Van Orman b, Colin Maden a, Jutta Zipfel c a Institute of Isotope Geochemistry and Mineral Resources, ETH Zurich, Clausiusstrasse 25, 8092 Zurich, Switzerland b Department of Geological Sciences, Case Western Reserve University, Cleveland, OH, USA c Forschungsinstitut und Naturmuseum Senckenberg, Frankfurt am Main, Germany article info abstract Article history: Acapulcoites and lodranites are highly metamorphosed to partially molten meteorites with mineral and bulk Received 11 November 2008 compositions similar to those of ordinary chondrites. These properties place the acapulcoites and lodranites Received in revised form 8 April 2009 between the unmelted chondrites and the differentiated meteorites and as such acapulcoites–lodranites are Accepted 9 April 2009 of special interest for understanding the initial stages of asteroid differentiation as well as the role of 26Al Available online 3 June 2009 heating in the thermal history of asteroids. To constrain the accretion timescale and thermal history of the Editor: R.W. Carlson acapulcoite–lodranite parent body, and to compare these results to the thermal histories of other meteorite parent bodies, the Hf–W system was applied to several acapulcoites and lodranites. Acapulcoites Dhofar 125 Keywords: – Δ chronology and NWA 2775 and lodranite NWA 2627 have indistinguishable Hf W ages of tCAI =5.2±0.9 Ma and Δ isochron tCAI =5.7±1.0 Ma, corresponding to absolute ages of 4563.1±0.8 Ma and 4562.6±0.9 Ma.
    [Show full text]
  • Chondrule Sizes, We Have Compiled and Provide Commentary on Available Chondrule Dimension Literature Data
    Invited review Chondrule size and related physical properties: a compilation and evaluation of current data across all meteorite groups. Jon M. Friedricha,b,*, Michael K. Weisbergb,c,d, Denton S. Ebelb,d,e, Alison E. Biltzf, Bernadette M. Corbettf, Ivan V. Iotzovf, Wajiha S. Khanf, Matthew D. Wolmanf a Department of Chemistry, Fordham University, Bronx, NY 10458 USA b Department of Earth and Planetary Sciences, American Museum of Natural History, New York, NY 10024 USA c Department of Physical Sciences, Kingsborough College of the City University of New York, Brooklyn, NY 11235, USA d Graduate Center of the City University of New York, 365 5th Ave, New York, NY 10016 USA e Lamont-Doherty Earth Observatory, Columbia University, Palisades, New York 10964 USA f Fordham College at Rose Hill, Fordham University, Bronx, NY 10458 USA In press in Chemie der Erde – Geochemistry 21 August 2014 *Corresponding Author. Tel: +718 817 4446; fax: +718 817 4432. E-mail address: [email protected] 2 ABSTRACT The examination of the physical properties of chondrules has generally received less emphasis than other properties of meteorites such as their mineralogy, petrology, and chemical and isotopic compositions. Among the various physical properties of chondrules, chondrule size is especially important for the classification of chondrites into chemical groups, since each chemical group possesses a distinct size-frequency distribution of chondrules. Knowledge of the physical properties of chondrules is also vital for the development of astrophysical models for chondrule formation, and for understanding how to utilize asteroidal resources in space exploration. To examine our current knowledge of chondrule sizes, we have compiled and provide commentary on available chondrule dimension literature data.
    [Show full text]
  • Petrogenesis of Acapulcoites and Lodranites: a Shock-Melting Model
    Geochimica et Cosmochimica Acta 71 (2007) 2383–2401 www.elsevier.com/locate/gca Petrogenesis of acapulcoites and lodranites: A shock-melting model Alan E. Rubin * Institute of Geophysics and Planetary Physics, University of California, Los Angeles, CA 90095-1567, USA Received 31 May 2006; accepted in revised form 20 February 2007; available online 23 February 2007 Abstract Acapulcoites are modeled as having formed by shock melting CR-like carbonaceous chondrite precursors; the degree of melting of some acapulcoites was low enough to allow the preservation of 3–6 vol % relict chondrules. Shock effects in aca- pulcoites include veins of metallic Fe–Ni and troilite, polycrystalline kamacite, fine-grained metal–troilite assemblages, metal- lic Cu, and irregularly shaped troilite grains within metallic Fe–Ni. While at elevated temperatures, acapulcoites experienced appreciable reduction. Because graphite is present in some acapulcoites and lodranites, it seems likely that carbon was the principal reducing agent. Reduction is responsible for the low contents of olivine Fa (4–14 mol %) and low-Ca pyroxene Fs (3–13 mol %) in the acapulcoites, the observation that, in more than two-thirds of the acapulcoites, the Fa value is lower than the Fs value (in contrast to the case for equilibrated ordinary chondrites), the low FeO/MnO ratios in acapulcoite olivine (16–18, compared to 32–38 in equilibrated H chondrites), the relatively high modal orthopyroxene/olivine ratios (e.g., 1.7 in Monument Draw compared to 0.74 in H chondrites), and reverse zoning in some mafic silicate grains. Lodranites formed in a similar manner to acapulcoites but suffered more extensive heating, loss of plagioclase, and loss of an Fe–Ni–S melt.
    [Show full text]
  • Frontier Mountain Meteorite Specimens of the Acapulcoite-Lodranite Clan: Petrography, Pairing, and Parent-Rock Lithology of an Unusual Intrusive Rock
    Meteoritics & Planetary Science 43, Nr 4, 731–744 (2008) Abstract available online at http://meteoritics.org Frontier Mountain meteorite specimens of the acapulcoite-lodranite clan: Petrography, pairing, and parent-rock lithology of an unusual intrusive rock Alessandro BURRONI and Luigi FOLCO* Museo Nazionale dell’Antartide, Università di Siena, Via Laterina 8, I-53100 Siena, Italy *Corresponding author. E-mail: [email protected] (Received 31 January 2007; revision accepted 10 October 2007) Abstract–In this paper we reconstruct the heterogeneous lithology of an unusual intrusive rock from the acapulcoite-lodranite (AL) parent asteroid on the basis of the petrographic analysis of 5 small (<8.3 g) meteorite specimens from the Frontier Mountain ice field (Antarctica). Although these individual specimens may not be representative of the parent-rock lithology due to their relatively large grain size, by putting together evidence from various thin sections and literature data we conclude that Frontier Mountain (FRO) 90011, FRO 93001, FRO 99030, and FRO 03001 are paired fragments of a medium- to coarse-grained igneous rock which intrudes a lodranite and entrains xenoliths. The igneous matrix is composed of enstatite (Fs13.3 ± 0.4 Wo3.1 ± 0.2), Cr-rich augite (Fs6.1 ± 0.7 Wo42.3 ± 0.9), and oligoclase (Ab80.5 ± 3.3 Or3.2 ± 0.6). The lodranitic xenoliths show a fine-grained (average grain size 488 ± 201 µm) granoblastic texture and consist of olivine Fa9.5 ± 0.4 and Fe,Ni metal and minor amounts of enstatite Fs12.7 ± 0.4 Wo1.8 ± 0.1, troilite, chromite, schreibersite, and Ca-phosphates. Crystals of the igneous matrix and lodranitic xenoliths are devoid of shock features down to the scanning electron microscope scale.
    [Show full text]
  • UNIVERSITY of CALIFORNIA, SAN DIEGO Primitive and Differentiated
    UNIVERSITY OF CALIFORNIA, SAN DIEGO Primitive and differentiated achondrite meteorites and partial melting in the early Solar System A Thesis submitted in partial satisfaction of the requirements for the degree Master of Science in Earth Sciences By Christopher Andrew Corder Committee in charge: Professor James M. D. Day, Chair Professor Geoffrey W. Cook Professor David R. Stegman 2015 © Christopher Andrew Corder, 2015 All rights reserved. The Thesis of Christopher Corder is approved and it is acceptable in quality and form for publication on microfilm and electronically: Chair University of California, San Diego 2015 iii Dedication This manuscript would be far from complete without thanking those who helped set the stage for the many hours of work it documents, and those thank-yous would be far from complete without recognizing my parents and their unwavering support throughout years of study. I know I was the one in the lab, but I never would have made it there, or to my defense, or through any of the long days and nights if it weren’t for you both. Thank you, so much. I’d love to thank my entire family, especially Stephen. You’re a brother Stephen, and you encourage me more than you know. Whenever it seemed like research was going nowhere, you were there to remind me why science is always a worthwhile endeavor. Even more importantly you remind me, by example, that there are exceptional people in this world. Many thanks are due to the lab group I worked with and other smart folks at SIO. First of all, thank you James for trusting this intriguing suite of meteorites to my care.
    [Show full text]
  • Acapulcoite-Lodranite Meteorites: Ultramafic Asteroidal Partial Melt
    G Model CHEMER-25432; No. of Pages 51 ARTICLE IN PRESS Chemie der Erde xxx (2017) xxx–xxx Contents lists available at ScienceDirect Chemie der Erde j ournal homepage: www.elsevier.de/chemer Invited review Acapulcoite-lodranite meteorites: Ultramafic asteroidal partial melt residues a,∗ b Klaus Keil , Timothy J. McCoy a Hawai’i Institute of Geophysics and Planetology, School of Ocean and Earth Science and Technology, University of Hawai’i at Manoa, Honolulu, HI 96822, USA b Department of Mineral Sciences, National Museum of Natural History, Smithsonian Institution, Washington, DC 20560-0119, USA a r t i c l e i n f o a b s t r a c t Article history: Acapulcoites (most ancient Hf-W ages are 4,563.1 ± 0.8 Ma), lodranites (most ancient Hf-W ages are Received 13 February 2017 4,562.6 ± 0.9 Ma) and rocks transitional between them are ancient residues of different degrees of partial Received in revised form 3 April 2017 melting of a chondritic source lithology (e.g., as indicated by the occurrence of relict chondrules in 9 Accepted 21 April 2017 acapulcoites), although the precise chondrite type is unknown. Acapulcoites are relatively fine- grained ∼ ( 150–230 ␮m) rocks with equigranular, achondritic textures and consist of olivine, orthopyroxene, Ca- Keywords: rich clinopyroxene, plagioclase, metallic Fe,Ni, troilite, chromite and phosphates. Lodranites are coarser Partial melting grained (540–700 ␮m), with similar equigranular, recrystallized textures, mineral compositions and con- Age tents, although some are significantly depleted in eutectic Fe,Ni-FeS and plagioclase- clinopyroxene Chondritic composition Origin partial melts.
    [Show full text]
  • 105. Titanium Stable Isotopic Variations in Chondrites
    Available online at www.sciencedirect.com ScienceDirect Geochimica et Cosmochimica Acta 213 (2017) 534–552 www.elsevier.com/locate/gca Titanium stable isotopic variations in chondrites, achondrites and lunar rocks Nicolas D. Greber a,⇑, Nicolas Dauphas a, Igor S. Puchtel b, Beda A. Hofmann c, Nicholas T. Arndt d a Origins Laboratory, Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, 5734 South Ellis Avenue, Chicago, IL 60615, USA b Department of Geology, University of Maryland, College Park, MD 20742, USA c Naturhistorisches Museum der Burgergemeinde Bern, Bernastrasse 15, Bern, Switzerland d Universite´ Grenoble Alpes, Institute Science de la Terre (ISTerre), CNRS, F-38041 Grenoble, France Received 22 December 2016; accepted in revised form 21 June 2017; Available online 30 June 2017 Abstract Titanium isotopes are potential tracers of processes of evaporation/condensation in the solar nebula and magmatic differ- entiation in planetary bodies. To gain new insights into the processes that control Ti isotopic variations in planetary materials, 25 komatiites, 15 chondrites, 11 HED-clan meteorites, 5 angrites, 6 aubrites, a martian shergottite, and a KREEP-rich impact melt breccia have been analyzed for their mass-dependent Ti isotopic compositions, presented using the d49Ti notation (devi- ation in permil of the 49Ti/47Ti ratio relative to the OL-Ti standard). No significant variation in d49Ti is found among ordi- nary, enstatite, and carbonaceous chondrites, and the average chondritic d49Ti value of +0.004 ± 0.010‰ is in excellent agreement with the published estimate for the bulk silicate Earth, the Moon, Mars, and the HED and angrite parent- bodies.
    [Show full text]
  • Chondrules Reveal Large-Scale Outward Transport of Inner Solar System Materials in the Protoplanetary Disk
    Chondrules reveal large-scale outward transport of inner Solar System materials in the protoplanetary disk Curtis D. Williamsa,1, Matthew E. Sanborna, Céline Defouilloyb,2, Qing-Zhu Yina,1, Noriko T. Kitab, Denton S. Ebelc, Akane Yamakawaa,3, and Katsuyuki Yamashitad aDepartment of Earth and Planetary Sciences, University of California, Davis, CA 95616; bWiscSIMS, Department of Geoscience, University of Wisconsin–Madison, Madison, WI 53706; cDepartment of Earth and Planetary Sciences, American Museum of Natural History, New York, NY 10024; and dGraduate School of Natural Science and Technology, Okayama University, Kita-ku, 700-8530 Okayama, Japan Edited by H. J. Melosh, Purdue University, West Lafayette, IN, and approved August 9, 2020 (received for review March 19, 2020) Dynamic models of the protoplanetary disk indicate there should actually be composed of solids with diverse formation histories be large-scale material transport in and out of the inner Solar Sys- and, thus, distinct isotope signatures, which can only be revealed tem, but direct evidence for such transport is scarce. Here we show by studying individual components in primitive chondritic me- that the e50Ti-e54Cr-Δ17O systematics of large individual chon- teorites (e.g., chondrules). Chondrules are millimeter-sized drules, which typically formed 2 to 3 My after the formation of spherules that evolved as free-floating objects processed by the first solids in the Solar System, indicate certain meteorites (CV transient heating in the protoplanetary disk (1) and represent a and CK chondrites) that formed in the outer Solar System accreted major solid component (by volume) of the disk that is accreted an assortment of both inner and outer Solar System materials, as into most chondrites.
    [Show full text]
  • Partial Melting and Melt Migration in the Acapulcoite-Lodranite Parent Body
    Geochimica et Cosmochimica Acta, Vol. 61. No. 3, pp. 639-650, 1997 Copyright 0 1997 Elsevier Science Ltd Pergamon Printed in the USA. All rights reserved 0016-7037/97 $17.00 + .OO PI1 SOO16-7037(96)00365-l Partial melting and melt migration in the acapulcoite-lodranite parent body T. J. McCoy,‘.‘.* K. I&IL,‘.+ D. W. MuENow,‘.~.+ and L. WILSON’.“.’ ‘Hawai’i Institute of Geophysics and Planetology, School of Ocean and Earth Science and Technology, University of Hawai’i at Manoa, Honolulu, Hawai’i 96822, USA ‘Code SN4, NASA/Johnson Space Center, Houston, Texas 77058, USA 3Chemistry Department, University of Hawai’i at Manoa, Honolulu, Hawai’i 96822, USA 4Environmental Science Division, Institute of Environmental and Biological Sciences, Lancaster University, Lancaster LA1 4YQ. UK (Received October 10, 1995; accepted in revised form October 21, 1996) Abstract-We review petrologic evidence that the acapulcoites and lodranites formed by < 1 ~01% to probably >20 ~01% whole rock partial melting of a chondritic precursor material. At low degrees of partial melting, only Fe,Ni-FeS cotectic melting occurred. Migration distances for partial melts were short, resulting in the formation of acapulcoites with essentially chondritic troilite and plagioclase contents, but achondritic textures. At high degrees of partial melting, both Fe,Ni-FeS and basaltic (plagioclase-pyroxene) partial melts formed, and the melts may have migrated out of the source rock. The partial melt residues, which are more or less depleted in Fe,Ni-FeS and plagioclase, are the lodranites. Melt migration was complex: most acapulcoites, which experienced relatively low degrees of partial melting, lost little if any of the partial melt.
    [Show full text]
  • Petrologic and Minerochemical Trends of Acapulcoites, Winonaites and Lodranites: New Evidence from Image Analysis and EMPA Investigations †
    Geosciences 2015, 5, 222-242; doi:10.3390/geosciences5030222 OPEN ACCESS geosciences ISSN 2076-3263 www.mdpi.com/journal/geosciences Article Petrologic and Minerochemical Trends of Acapulcoites, Winonaites and Lodranites: New Evidence from Image † Analysis and EMPA Investigations Vanni Moggi Cecchi 1,‡,* and Stefano Caporali 2,3,‡ 1 Dipartimento di Scienze della Terra, Università degli Studi di Firenze, Via La Pira 4, 50121 Florence, Italy 2 Dipartimento di Chimica, Università degli Studi di Firenze, Via della Lastruccia 3, 50019 Sesto Fiorentino, Italy 3 Consorzio INSTM, Via Giusti 9, 50121 Florence, Italy; E-Mail: [email protected] † This paper is an extended version of our paper published in the 42nd Lunar and Planetary Science Conference, The Woodlands, TX, USA, 7–11 March 2011. ‡ These authors contributed equally to this work. * Author to whom correspondence should be addressed; E-Mail: [email protected]; Tel.: +39-055-275-7456; Fax: +39-055-275-6322. Academic Editor: Jesus Martinez-Frias Received: 1 April 2015 / Accepted: 23 June 2015 / Published: 2 July 2015 Abstract: A comprehensive classification of primitive achondrites is difficult due to the high compositional and textural variability and the low number of samples available. Besides oxygen isotopic analysis, other minerochemical and textural parameters may provide a useful tool to solve taxonomic and genetic problems related to these achondrites. The results of a detailed modal, textural and minerochemical analysis of a set of primitive achondrites are presented and compared with literature data. All the samples show an extremely variable modal composition among both silicate and opaque phases. A general trend of troilite depletion vs.
    [Show full text]
  • Programme Book
    EPSC2018 European Planetary Science Congress 2018 16–21 September 2018 TU Berlin | Berlin | Germany Programme Book © TU Berlin/Dahl access to access to cafeteria area first floor area Information & registration Jupiter room Ground floor area H0104 Ground floor area EPSCEuropean Planetary Science Congress Mars Venus Saturn Uranus Neptune room room room room room H0112 H0111 H0110 H0107 H0106 access to ground floor area Cafeteria area Cafeteria area EPSCEuropean Planetary Science Congress Mercury Press conference Press room room room H2035 H2036 H2037 Second floor area Second floor area EPSCEuropean Planetary Science Congress EEuropeaPn PlanetarSy Science CCongress Table of contents 1 Welcome …………………………………2 General information …………………………………4 Exhibitors, Community events …………………………………6 Splinter meetings & workshops .………………………….….…7 Session overview ……………………………..….8 Monday – Oral programme ..……………………………….9 Tuesday – Oral programme ……………………………….19 Tuesday – Poster programme .………………………………30 Wednesday – Oral programme .……….…………………..…42 Wednesday – Poster programme .………………………………51 Thursday – Oral programme ……………………………….60 Thursday – Poster programme ……………………………….71 Friday – Oral programme ……………………………….81 Author index ……………………………….91 European Planetary Science Congress 2018 2 Welcome Message from the Organizers amateur astronomers, policy makers, the next generation of scientists and engineers, and On behalf of the Executive Committee, the planetary scientists around the world. Scientific Organizing Committee and the Local Organizing Committee, welcome
    [Show full text]