DOCSLIB.ORG

Geologic Setting of the Peña De Bernal Natural Monument, Querétaro, México: an Endogenous Volcanic Dome

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
Geologic Setting of the Peña De Bernal Natural Monument, Querétaro, México: an Endogenous Volcanic Dome Geologic setting of the Peña de Bernal Natural Monument, Querétaro, México: An endogenous volcanic dome Gerardo J. Aguirre-Díaz1,*, Alfredo Aguillón-Robles2,*, Margarito Tristán-González2, Guillermo Labarthe-Hernández2, Margarita López-Martínez3,*, Hervé Bellon4,*, and Jorge Nieto-Obregón5,* 1Centro de Geociencias, Universidad Nacional Autónoma de México, campus Juriquilla, Boulevard Juriquilla 3001, Juriquilla, Querétaro, C.P. 76230, México 2Instituto de Geología, Universidad Autónoma de San Luis Potosí, San Luis Potosí, México 3División de Ciencias de la Tierra, Centro de Investigación Científi ca y de Educación Superior de Ensenada, Carretera Ensenada- Tijuana No 3918, Zona Playitas, C.P. 22860, Ensenada, México 4European University of Brittany, 6538, Domaines Océaniques, Institut Universitaire Européen de la Mer (IUEM), Université de Bretagne Occidentale, 29280 Plouzané, France 5Facultad de Ingeniería, Universidad Nacional Autónoma de México, Ciudad Universitaria, Delegación Coyoacán, 04510, México, D.F., México ABSTRACT INTRODUCTION above sea level [masl]). Either elevation chosen from these new values shows that the Peña de Peña de Bernal is a natural monument Peña de Bernal, at 20°45′N, 99°57′W Bernal is apparently the highest monolith of located near the town of Bernal, in Queré- (Fig. 1), is a prominent peak that was declared a the world. taro State, central Mexico. It is one of natural reserve area by the State Government of Previous regional geologic mapping has con- the tallest monoliths of the world, with a Querétaro in 2007 (Fig. 2). Since 30 September sidered Peña de Bernal as a Paleocene monzo- maximum height of 433 m. Peña de Bernal 2009, it has been included in UNESCO’s Intan- granodioritic pluton (Segerstrom, 1961) or a was recently declared Intangible Cultural gible Cultural Heritage sites (UNESCO, 2009) subvolcanic Miocene felsic body (Carrillo- Heritage of Humanity Patrimony by United in order to preserve the traditions of Otomí and Martínez, 1998). However, the mechanism of Nations Educational, Scientifi c, and Cultural Chichimeca indigenous peoples as well as the emplacement has remained unknown. Before Organization (UNESCO). In spite of being Peña de Bernal itself. Furthermore, Peña de Ber- this work, there were no scientifi c studies spe- both a natural and cultural monument, nal is known as the main entrance to the Sierra cifi cally on Peña de Bernal’s geologic nature little is known about its origin, physical Gorda mountains area, a range that was declared and origin. The purpose of this study is therefore characteristics, and chemical composition. in 2001 as a Biosphere Reserve by UNESCO to provide detailed information on the geologic It is a leucocratic-igneous rock intruding (2001). In a few publications and in some web setting, including the stratigraphy, structure, marine Mesozoic sedimentary rocks and has sites, including the offi cial municipal (county) geochronology, and geochemistry, to answer been misinterpreted as a pluton of Eocene web page of the Bernal area and that of the fundamental questions of when and how Peña or older age. However, this study shows National Institute of History and Anthropology de Bernal was formed and why it is topographi- that Peña de Bernal is a dacitic dome with (INAH) of Mexico, Peña de Bernal is identifi ed cally prominent with respect to its surroundings. SiO2 = 67 wt% and an age of 8.7 ± 0.2 Ma. as one of the highest monoliths in the world, The complete Peña de Bernal body includes with monolith defi ned as a prominent and large GEOLOGY three plugs that crop out in an ~3.5 × 1.5 km monolithologic rock (Fig. 2). The exact height area elongated N40°E. Texture of the rock is of Peña de Bernal has not been well constrained, Peña de Bernal is located at the intersection porphyritic, nearly holocrystalline (80 vol% with reported heights ranging between 288 and of three major geologic provinces: the Miocene– crystals and 20 vol% glass), with a mineral 360 m (e.g., Coenraads and Koivula, 2007; Quaternary Mexican Volcanic Belt (Demant , assemblage of pyroxene, hornblende, bio- INAH, 2009; Municipio Ezequiel Montes, 1978; Aguirre-Díaz et al., 1998; Siebe et al., tite, plagioclase, and quartz, plus accessory 2009). From the topographic data of the offi - 2006), the mid-Tertiary Sierra Madre Occiden- apatite and zircon. Peña de Bernal dacite cial Mexican agency for National Geographic tal ignimbrite-dominated sequence (McDowell is a spine-type endogenous dome that was Studies and Information (Instituto Nacional de and Clabaugh, 1979; Aguirre-Díaz et al., 2008), forcefully intruded through the Mesozoic Geografía Estadística e Informática [INEGI], and the Mesozoic Sierra Madre Oriental fold- sequence practically as a solid plug. 2002) and from altimeter measurements carried thrust belt (Suter, 1987; Bartolini et al., 1999), out by us at the base and at the top of Peña de which in this area corresponds to the Sierra *Emails: Aguirre-Díaz: [email protected] Bernal, we have calculated a height of 433 m on Gorda sector (Fig. 1). A simplifi ed geologic map .mx; Aguillón-Robles: [email protected]; López- Martínez: [email protected]; Bellon: herve.bellon the northern side (Fig. 3). Height is 405 m on the of the Peña de Bernal area is shown in Figure 4. @univ-brest.fr; Nieto-Obregón: nieto@servidor southern side of Peña de Bernal with respect to The stratigraphy is briefl y described below, from .unam.mx. the plain where Bernal town lies (2049 meters the oldest to the youngest unit (Fig. 5). Geosphere; June 2013; v. 9; no. 3; p. 557–571; doi:10.1130/GES00843.1; 16 fi gures; 6 tables. Received 5 July 2012 ♦ Revision received 14 January 2013 ♦ Accepted 20 February 2013 ♦ Published online 4 April 2013 For permission to copy, contact [email protected] 557 © 2013 Geological Society of America Downloaded from http://pubs.geoscienceworld.org/gsa/geosphere/article-pdf/9/3/557/3344305/557.pdf by guest on 26 September 2021 Aguirre-Díaz et al. 100°30'W 100°00'W MEX N S I 57 E R R A G EXPLANATION O San José R Iturbide 21°00'N D Toll highway El Zamorano A Highway Volcano San Miguel Tolimán State line Tolimán Town Zamorano Study area City Colón San Martín Volcano Santa Rosa Cadereyta de Jauregui Ajuchitlán Bernal MEX 57 Ezequiel Villa Montes Progreso Apaseo El Grande Tequisquiapan QUERÉTARO 20°30'N San Pedro Escobedo 32ºN Apaseo El Alto MEX S I E R R A M A D R E O R I E N T 57 S I E R R A M A D R E O C C I D E N T A L 0510 20 U. S. A. San Juan del Río Kilometers 24ºN MESA CE Gulf Sierra NTRAMa of L AL Occidendre Mexico tal Pacific Mexican Volcanic Belt Ocean Mexico City 0 200 400 16ºN Km Guatemala 112ºW 104ºW 96ºW 88ºW Figure 1. Index map showing the position of Peña de Bernal with respect to some of the geological provinces of Mexico and the geography of the local area; the study area is highlighted in the inset. Las Trancas Formation (Jt) fi ssile shales, calcareous limonites, and dirty with minor amounts of graywackes. Bedding limestones with pyrite and minor amounts of is generally undulated, with thicknesses in the Las Trancas Formation was defined by graywackes and fl int (Segerstrom, 1961, 1962; order of tens of meters. The shales and lime- Segerstrom (1961) as a Jurassic–Early Cre- Chauve et al., 1985; Carrillo-Martínez, 1990). stones of Las Trancas Formation were inten- taceous (Kimmeridgian–Barremian) marine In the Bernal area, this unit occurs as a thinly sively deformed during the Cretaceous–Tertiary sedimentary sequence. It consists of dark-gray bedded sequence of fi ssile shales and limestones (K-T) Laramide orogeny (Chauve et al., 1985; 558 Geosphere, June 2013 Downloaded from http://pubs.geoscienceworld.org/gsa/geosphere/article-pdf/9/3/557/3344305/557.pdf by guest on 26 September 2021 Geologic setting of Peña de Bernal dome, Querétaro, México at the locality of Dedhó, and Texamites sp. in the Tolimán canyon, confi rming the Late Cretaceous epoch of this unit. Soyatal Formation is thinly to 500 km medium bedded, showing boudinage primary MEXICO bedding. It is dark gray when fresh, and light gray Peña de to white when weathered. As in Las Trancas, this N Bernal unit was folded and northeastwardly tectonically transported during the K-T Laramide orogeny Mexican (Chauve et al., 1985). Las Trancas Formation Volcanic Belt was thrusted on Soyatal Formation during this orogeny (Suter, 1987; Carrillo-Martínez, 1998), forming klippes at top of younger Soyatal. In the Bernal area, the top of Soyatal Formation is A eroded, and thus, a complete thickness estimate was not possible, but a minimum of 300 m is 0 0.5 ~1 Km NE Peña de Bernal peak Bernal town considered our best approach. San Antonio Tortuga Main plug de la Cal plug Lower Tertiary Continental Clastic Sediments (Ts) Continental detrital deposits crop out to the NW of the mapped area and nearby the town of San Martín (Fig. 1). Within the mapped area these deposits occur as small patches in the SW lower fl ank of Peña de Bernal too small to be shown in Figure 4, and to the southwest of Cerro B Azul, in the northeastern portion of the area. Thickness ranges from 0 to 20 m. Near Bernal Figure 2. (A) Panoramic view toward the north of Peña de Bernal monolith and cor- this unit consists mainly of conglomerates with responding regional index map (inset). (B) Panoramic view toward the east of Peña de clast sizes of 2–30 cm in diameter, mainly from Bernal from summit of San Martín volcano. Note the elongated shape of the main plug of shales of Las Trancas Formation and black fl int the Peña de Bernal dacitic dome and the rounded plug of Tortuga.
Load more

Recommended publications
  • JVP 26(3) September 2006—ABSTRACTS
    Neoceti Symposium, Saturday 8:45 acid-prepared osteolepiforms Medoevia and Gogonasus has offered strong support for BODY SIZE AND CRYPTIC TROPHIC SEPARATION OF GENERALIZED Jarvik’s interpretation, but Eusthenopteron itself has not been reexamined in detail. PIERCE-FEEDING CETACEANS: THE ROLE OF FEEDING DIVERSITY DUR- Uncertainty has persisted about the relationship between the large endoskeletal “fenestra ING THE RISE OF THE NEOCETI endochoanalis” and the apparently much smaller choana, and about the occlusion of upper ADAM, Peter, Univ. of California, Los Angeles, Los Angeles, CA; JETT, Kristin, Univ. of and lower jaw fangs relative to the choana. California, Davis, Davis, CA; OLSON, Joshua, Univ. of California, Los Angeles, Los A CT scan investigation of a large skull of Eusthenopteron, carried out in collaboration Angeles, CA with University of Texas and Parc de Miguasha, offers an opportunity to image and digital- Marine mammals with homodont dentition and relatively little specialization of the feeding ly “dissect” a complete three-dimensional snout region. We find that a choana is indeed apparatus are often categorized as generalist eaters of squid and fish. However, analyses of present, somewhat narrower but otherwise similar to that described by Jarvik. It does not many modern ecosystems reveal the importance of body size in determining trophic parti- receive the anterior coronoid fang, which bites mesial to the edge of the dermopalatine and tioning and diversity among predators. We established relationships between body sizes of is received by a pit in that bone. The fenestra endochoanalis is partly floored by the vomer extant cetaceans and their prey in order to infer prey size and potential trophic separation of and the dermopalatine, restricting the choana to the lateral part of the fenestra.
    [Show full text]
  • Geology of the Bernal-Jalpan Area Estado De Queretaro Mexico
    Geology of the Bernal-Jalpan Area Estado de Queretaro Mexico By KENNETH SEGERSTROM GEOLOGIC INVESTIGATIONS IN MEXICO GEOLOGICAL SURVEY BULLETIN 1104-B Prepared in cooperation with the Instituto Nacional para la Investigation de Recursos Minerales, under the auspices of the International Cooperation Admin­ istration of the Department of State UNITED STATES GOVERNMENT PRINTING OFFICE, WASHINGTON : 1961 UNITED STATES DEPARTMENT OF THE INTERIOR STEW ART L. UDALL, Secretary GEOLOGICAL SURVEY Thomas B. Nolan, Director For sale by the Superintendent of Documents, U.S. Government Printing Office Washington 25, D.C. CONTENTS Page Abstract __..---_.--___-____._-___---___.______..____._._...______ 19 Introduction __-_______--_____-_____-____-_______._____..__..__.___ 19 Location _____________________________________________________ 19 Fieldwork and acknowledgments._______________________________ 19 Geography ___________________________________________________ 2 ] Accessibility ___________________________________________ ___ 21 Topography and drainage__________________________________ 22 Climate. _--__--_-___-_--_--___._____-_ ____________.______ 24 Vegetation_ _ _______--..___.__.__________._____-_____.___ 26 Water supply and agriculture_-___-_______-__---__--_-______ 27 Archeology ---_-----_---_------_--___---____-_____--______ 29 Sedimentary, metamorphic, and volcanic rocks....____.-_____..____._. 29 Jurassic system or older.___---_-_____--___---____-__--_-_______ 30 Pre-Las Trancas rocks.____________________________________ 30 Jurassic system.
    [Show full text]
  • 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.
    [Show full text]
  • Warfare in a Fragile World: Military Impact on the Human Environment
    Recent Slprt•• books World Armaments and Disarmament: SIPRI Yearbook 1979 World Armaments and Disarmament: SIPRI Yearbooks 1968-1979, Cumulative Index Nuclear Energy and Nuclear Weapon Proliferation Other related •• 8lprt books Ecological Consequences of the Second Ihdochina War Weapons of Mass Destruction and the Environment Publish~d on behalf of SIPRI by Taylor & Francis Ltd 10-14 Macklin Street London WC2B 5NF Distributed in the USA by Crane, Russak & Company Inc 3 East 44th Street New York NY 10017 USA and in Scandinavia by Almqvist & WikseH International PO Box 62 S-101 20 Stockholm Sweden For a complete list of SIPRI publications write to SIPRI Sveavagen 166 , S-113 46 Stockholm Sweden Stoekholol International Peace Research Institute Warfare in a Fragile World Military Impact onthe Human Environment Stockholm International Peace Research Institute SIPRI is an independent institute for research into problems of peace and conflict, especially those of disarmament and arms regulation. It was established in 1966 to commemorate Sweden's 150 years of unbroken peace. The Institute is financed by the Swedish Parliament. The staff, the Governing Board and the Scientific Council are international. As a consultative body, the Scientific Council is not responsible for the views expressed in the publications of the Institute. Governing Board Dr Rolf Bjornerstedt, Chairman (Sweden) Professor Robert Neild, Vice-Chairman (United Kingdom) Mr Tim Greve (Norway) Academician Ivan M£ilek (Czechoslovakia) Professor Leo Mates (Yugoslavia) Professor
    [Show full text]
  • New Chryse and the Provinces
    New Chryse and the Provinces The city of New Chryse is actually several connected cities. The Upper City is located on a break in the crater rim, looking down past a steep rock to the Lower City. Inside the da Vinci crater rim lies the Inner City, also known as the Old City – Red Era tunnels and cave shelters, as well as several nanocomposite towers and cupolas on Mona Lys Ridge looking down on the lower parts of the city. The Lower city lies in a valley sloping down to the Harbour City, which fills a crater 20 kilometres to the East. The Harbour City crater is connected to Camiling Bay and the sea through two canyons and is very well protected from both wind and ice. South of the Lower City and Harbour City lies The Slopes, a straight slope into the sea that is covered with sprawl and slums. Mona Lys Ridge is a mixture of palatial estates surrounded by gardens, imposing official imperial buildings and towering ancient structures used by the highest ranks of the Empire. The central imperial administration and especially the Council is housed in the Deimos Needle, a diamondoid tower that together with its sibling the Phobos Needle dominate the skyline. Escalators allow swift and discreet transport down to the lower levels of the city, and can easily be defended by the police force. North of Mona Lys lies a secluded garden city for higher administrators, guild officials and lesser nobility. The Inner City is to a large extent part of Mona Lys, although most of the inhabitants of Mona Lys do not care much for the dusty old tunnels and hidden vaults – that is left to the Guild of Antiquarians who maintain and protect it.
    [Show full text]
  • Magnetized Impact Craters
    Icarus xxx (2011) xxx–xxx Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Predicted and observed magnetic signatures of martian (de)magnetized impact craters ⇑ Benoit Langlais a, , Erwan Thébault b a CNRS UMR 6112, Université de Nantes, Laboratoire de Planétologie et Géodynamique, 2 Rue de la Houssinière, F-44000 Nantes, France b CNRS UMR 7154, Institut de Physique du Globe de Paris, Équipe de Géomagnétisme, 1 Rue Cuvier, F-75005 Paris, France article info abstract Article history: The current morphology of the martian lithospheric magnetic field results from magnetization and Received 3 May 2010 demagnetization processes, both of which shaped the planet. The largest martian impact craters, Hellas, Revised 6 January 2011 Argyre, Isidis and Utopia, are not associated with intense magnetic fields at spacecraft altitude. This is Accepted 6 January 2011 usually interpreted as locally non- or de-magnetized areas, as large impactors may have reset the mag- Available online xxxx netization of the pre-impact material. We study the effects of impacts on the magnetic field. First, a care- ful analysis is performed to compute the impact demagnetization effects. We assume that the pre-impact Keywords: lithosphere acquired its magnetization while cooling in the presence of a global, centered and mainly Mars, Surface dipolar magnetic field, and that the subsequent demagnetization is restricted to the excavation area cre- Mars, Interior Impact processes ated by large craters, between 50- and 500-km diameter. Depth-to-diameter ratio of the transient craters Magnetic fields is set to 0.1, consistent with observed telluric bodies. Associated magnetic field is computed between 100- and 500-km altitude.
    [Show full text]
  • Possible Origin of Chlorobenzene Detected by SAM Instrument at Gale Crater, Mars: Synergy of Iron Oxides and Perchlorate and Consequences for Organic Matter Analysis
    Eighth International Conference on Mars (2014) 1201.pdf Possible origin of chlorobenzene detected by SAM instrument at Gale crater, Mars: synergy of iron oxides and perchlorate and consequences for organic matter analysis. P. Francois1, P. Coll1, C. Szopa2, T. Georgelin3, A. Buch4, C. Freissinet5,6, I. Belmahdi4, A. McAdam5, J. Eigenbrode5, D. Glavin5, S. Kashyap5, A. R. Navarro- Gonzalez7, P. Mahaffy5 and M. Cabane2. [email protected]. 1LISA, Univ. Paris-Est Créteil, Univ. Denis Diderot & CNRS 94010 Créteil, France 2LATMOS, Univ. Pierre et Marie Curie, Univ. Versailles Saint- Quentin & CNRS, 75005 Paris, France 3LRS, Univ. Pierre et Marie Curie, Ivry sur Seine, France 4LGPM, Ecole Centrale de Paris, 92295 Châtenay-Malabry 5NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 6NASA Postdoctoral Program Administered by Oak Ridge Associated Universities, Oak Ridge, Tennessee 37831, USA 7Universidad Nacional Autónoma de México, México, D.F. 04510, Mexico Introduction: The Sample Analysis at Mars rates [5]. Apart from an oxychlorine phase, CB sam- (SAM) instrument on the Curiosity rover is designed to ples also contain iron oxides (e.g. hematite, magnetite) determine the inventory of organic and inorganic vola- [6] which could oxidize organic compounds and cata- tiles thermally evolved from solid samples notably by lyze their decomposition leading to differences in the using a combination of evolved gas analysis (EGA) amount and/or nature of the observed pyrolysis prod- and pyrolysis gas chromatography mass spectrometry ucts [7, 8]. A synergy between oxychlorine phases and (pyr-GC-MS) [1]. Multiple portions from three solid iron oxides in the presence of a carbon source can samples have been analyzed by SAM : a scoop of ba- potentially lead to the formation of CBZ, without any saltic sand at Rocknest (RN) and two drilled samples of specific need for aromatic precursors.
    [Show full text]
  • The Structure and Mechanical Properties of Hemp Fibers-Reinforced Poly(-Caprolactone)
    applied sciences Article The Structure and Mechanical Properties of Hemp Fibers-Reinforced Poly("-Caprolactone) Composites Modified by Electron Beam Irradiation Rafał Malinowski 1,* , Aneta Raszkowska-Kaczor 1, Krzysztof Moraczewski 2 , Wojciech Głuszewski 3 , Volodymyr Krasinskyi 4 and Lauren Wedderburn 1 1 Łukasiewicz Research Network—Institute for Engineering of Polymer Materials and Dyes, 55 M. Skłodowska-Curie Street, 87-100 Toru´n,Poland; [email protected] (A.R.-K.); [email protected] (L.W.) 2 Institute of Materials Engineering, Kazimierz Wielki University, 30 Chodkiewicza Street, 85-064 Bydgoszcz, Poland; [email protected] 3 Institute of Nuclear Chemistry and Technology, 16 Dorodna Street, 03-195 Warsaw, Poland; [email protected] 4 Department of Chemical Technology of Plastics Processing, Lviv Polytechnic National University, 12 Stepan Bandera Street, 79-013 Lviv, Ukraine; [email protected] * Correspondence: [email protected]; Tel.: +48-53-060-0220 Abstract: The need for the development of new biodegradable materials and modification of the properties the current ones possess has essentially increased in recent years. The aim of this study Citation: Malinowski, R.; was the comparison of changes occurring in poly("-caprolactone) (PCL) due to its modification by Raszkowska-Kaczor, A.; high-energy electron beam derived from a linear electron accelerator, as well as the addition of natural Moraczewski, K.; Głuszewski, W.; fibers in the form of cut hemp fibers. Changes to the fibers structure in the obtained composites and Krasinskyi, V.; Wedderburn, L. The the geometrical surface structure of sample fractures with the use of scanning electron microscopy Structure and Mechanical Properties were investigated.
    [Show full text]
  • 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
    [Show full text]
  • SOTANITO D,E AHUACAYLAN Sierra Madre Oriental Jalpan
    ,. , SOTANITO D,E AHUACAYLAN Sierra Madre Oriental Jalpan Ahuacatl~n I "t J I GU [ " ,. ASSOCIATION FOR MEXICAN CAVE STUDIES ,y. CAVE REPORT SERIES Number 1 t r ~:.iffI'i"Y..)" ~, ". lioN D '" RA: j,rl , ... __ ,. I'" ~, tr " ASSOCIATION FOR MEXICAN CAVE STUDIES CAVE REPORT SERIES Number 1 SOTANITO DE AHUACATLAN Sierra Madre Oriental; Jalpan; Ahuacatlan by TERRY W. RAINES The Speleo Press • Austin • 1972 The Association for Mexican Cave Studies is a non-profit, volunteer organization whose goals are the collection and dissemination of infor­ mation concerning Mexican caves. The AMCS publishes a Newsletter, Bulletin, and Cave Report Series which are available to any sincerely interested, conservation-minded person. Prices are available by writing. Some of the persons responsible for the continued success of the Association's endeavours are the following: Publications Editor Terry W. Raines Cave Files . William H. Russell Secretary-Treasurer Jan E. Lewis Coordinating Biologist James R. Reddell Photo Editor . Carl E. Kunath Production Manager. Ronald G. Fieseler ASSOCIATlON FOR MEXICAN CAVE STUDIES P. O. Box 7672, Austin, Texas 78712 Frontispiece: Craig Sainsott views the entrance of the 288.3 m (946 ft) drop within Sotanito de Ahuacatlan. Copyright ©1972 by the Association for Mexican Cave Studies Printed in the United States of America The Spe1eo Press P. O. Box 7037 Austin, Texas 78712 ASSOCIATION FOR MEXICAN CAVE STUDIES P. O. Box 7672, University Station Austin, Texas 78712 USA Price of this issue - $2.50 US INTRODUCTION the mid 1960's this right-of-way consisted solely of a single lane road paved with cob­ Of the 18 physiographic provinces in bles which was built in 1910.
    [Show full text]
  • Hidalgo, Mexico
    Mesozoic Fishes 4 – Homology and Phylogeny, G. Arratia, H.-P. Schultze & M. V. H. Wilson (eds.): pp. 373-388, 10 figs., 2 apps. © 2008 by Verlag Dr. Friedrich Pfeil, München, Germany – ISBN 978-3-89937-080-5 A new species of Ichthyotringa from the El Doctor Formation (Cretaceous), Hidalgo, Mexico Christopher FIELITZ & Katia GONZÁLEZ RODRÍGUEZ Abstract A new species of Ichthyotringa (Teleostei: Aulopiformes), Ichthyotringa mexicana, from the Muhi quarry near the town of Zimapán, Hidalgo, México is described. Thirteen specimens were examined. Preservation of individuals is poor, however, there is one complete specimen. I. mexicana n. sp. exhibits ichthyotringid characters such as a long, tapering rostrum; unornamented dermal bones of the skull roof; long mandible with a low coronoid proc- ess; and vertebral centra that are longer than deep. It differs from other species of Ichthyotringa by having a head comprising over one-half standard length; minute, pebble-like teeth on the ectopterygoid and endopterygoid; repeating pattern of small and large teeth on the premaxilla and maxilla; a preopercle with a posterior spine; and the absence of scales. A phylogenetic analysis of I. mexicana n. sp., Apateodus striatus, Apateopholis laniatus, I. delicata, I. furcata, and Yabrudichthys striatus suggests that 1) the Ichthyotringoidei is a monophyletic group, 2) Yabrudichthys is included in the group, and 3) Ichthyotringa is not monophyletic if Apateodus is included in the phylogeny. Only larger specimens of I. mexicana n. sp. have been found. Other teleost species represented at the Muhi quarry include juvenile forms. It is possible that I. mexicana n. sp. fed on these juveniles.
    [Show full text]
  • 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.
    [Show full text]