Volume of Abstracts

Total Page:16

File Type:pdf, Size:1020Kb

Volume of Abstracts Volume of Abstracts Indian Planetary Science Conference-2021 25-26 February 2021 Physical Research Laboratory ORAL Presentations No Details Speaker Page No The Impact of Stealth CMEs on Martian Topside 1 Smitha Thampi, SPL 1 Ionosphere Spatio-temporal characteristics of the He bulge in the 2 Neha Gupta, NARL 2 Martian Upper Atmosphere 3 Recurrent Space Weather Events at Mars C Krishnaprasad, SPL 3 How do we understand dust in the Martian 4 Varun Sheel, PRL 4 atmosphere? Response of the Martian ionospheric peak to the 5 Vrinda Mukundan, NCESS 5 Planet Encircling Dust Event of June 2018 MOM and MAVEN Observations of the Effects of Venkateswara Rao Narukull, 6 the 2018 Planet‐Encircling Dust Event on the Martian 6 NARL Thermospheric Densities Water ice clouds observations over Olympus Mons 7 using the Mars Color Camera and Mars Climate Jagabandhu Panda, NIT, Rourkela 7 Sounder Variation of composition of Martian atmosphere Nagaraja Kamsali, Bangalore 8 8 during solar quiet and disturbed periods University A study on the characteristic features of the V1 layer 9 of the Venus ionosphere using Akatsuki Ambili K M, SPL 9 measurements. Dinesh Kumar V. R., BITS Pilani, 10 Current Status of Venus Lightning Research 10 Hyderabad Analogue research in Astrobiology: Implications for 11 Sudha Rajamani, IISER Pune 11 delineating prebiotically relevant processes 12 Graphene in Titan Rahul Kumar Kushwaha, PRL 12 Isita, SRM Institute of Science & 13 Violacein: a Bio-pigment Exploited in Mars 13 Technology, Tamil Nadu Complex structures in the ejecta of hypervelocity 14 Surendra Singh, PRL 14 impacts on icy mixtures of amino acids Ranjan Sarkar, Max Planck The origin of Juventae Chasma, Mars, and the light- 15 Institute for Solar System 15 toned sedimentary rock occurrences within it Research, Germany New insights into the glacial activity within Erebus 16 Rishitosh Sinha, PRL 16 Montes, Mars Impact craters with fan deposits in southern 17 highlands of Mars: Insights into their hydrological Tuhi Saumya, Anna University 17 history Formation of Theater-headed valleys in the Valles 18 Pragya Singh, IIT Bombay 18 Marineris region SHARAD detection of subsurface reflection near 19 Rajiv Ranjan Bharti, PRL 19 Mangala Fossa, Mars Spectral Parameters for Orbital identification of Sandeepan Dhoundiyal, IIT 20 20 Martian Phyllosilicates Bombay No Details Speaker Page No Synthesis of chemical provinces on Mars with the 21 latest geochemical maps and implications for Alka Rani, PRL 21 geologic interpretations Hyperspectral analysis for studying temporal 22 variations of dry and water ice in Korolev and Louth Sehajpal Singh, IIRS 22 Crater on Mars Olivine-Serpentine-Magnesite Association in Salem Ultramafic Complex, Southern India: A Potential Asif Iqbal, Govt. College, 23 23 Terrestrial Analogue Site for Comparable Kasaragod Occurrences On Mars Vigneshwaran K, Govt. Arts 24 Kunnam formation - Potential Martian analogue site 24 College, Salem Emissivity and compositional Variation of Venus 25 Highlands with Ovda Regio: Insights into Venusian Nithin Mohan, NISER 25 surface processes Solar Wind Ion Spectrometer (SWIS): A subsystem 26 Prashant Kumar, PRL 26 of ASPEX on-board Aditya-L1 mission Solar Coronal Dynamics investigated using radio sounding experiment conducted on Indian Mars 27 Richa Naja Jain, SPL 27 Orbiter Mission (MOM) during 2015 solar conjunction event Proposed measurements of supra-thermal and 28 energetic particles from the Sun-Earth L1 point and Shiv Kumar Goyal, PRL 28 Martian orbit Probing the magnetic field of coronal loops using Sneha Chaudhari, Kadi Sarva 29 microwave and hard X-ray emissions during flare 29 Vishwavidhyalaya observed by SOXS mission Modelling the Impact of Magnetic Storms on 30 Souvik Roy, IISER, Kolkata 30 Planetary Environments Study of Phase Relationship of Sunspot Numbers Satish Kumar Kasde, Govt. 31 with F 10.7 cm Solar Radio-Fluxand Coronal Index 31 College Bhainsdehi, M.P. using Wavelet-Transform Technique Polarimetric Analysis of South polar crater of the 32 Lunar Surface using L-band SAR data of Shashi Kumar, IIRS 32 Chandrayaan-2 Mare Tranquillitatis region observed by CLASS on 33 Netra Pillai, URSC 33 board Chandrayaan-2 Estimation of Lunar Dielectric Constant from 34 Chandrayaan-1 and Chandrayaan-2 Hybrid-pol Inderkumar Kochar, IIT Roorkee 34 Datasets Hematite detection in the high latitudes of the Moon 35 Neha Panwar, PRL 35 using Chandrayaan-1 HySI data Compositional Variability Mapping of Transition zone between Serenitatis and Tranquillitatis Basin Abinandhan Sivakumar, 36 36 using Moon Minerology Mapper (M3) of Bharathidasan University Chandrayaan-1 & Clementine UVVIS Data Lunar Surface Thermophysical Behaviour – Present 37 Durga Prasad Karanam, PRL 37 Understanding and Future Implications Multiple Evidences for Modification of Central Peaks 38 in Lunar Complex Craters: Implications for Deepak Dhingra, IIT Kanpur 38 Determining the Subsurface Mineralogy First results of polarimetric observations of the 39 Reiner Gamma swirl using EMPOL of Mount Abu Megha Bhatt, PRL 39 observatory No Details Speaker Page No Role of impact-induced heating in early lunar-core 40 Vishal Goyal, Panjab University 40 formation Machine learning based distinction between primary 41 Suchit Purohit, Gujarat University 41 and secondary craters 42 Highly Siderophile Element conundrum of the Moon Yash Srivastava, PRL 42 Comparative Chemical and Spectral Characterization Deepchand V, University of 43 of Chromites in Nuggihalli Schist Belt, Western 43 Kerala Dharwar Craton (Southern India). Ion density distribution in the inner coma of peculiar 44 Susarla Raghuram, PRL 44 compositional comet C/2016 R2 (Pan-STARRS) Multi-fluid modelling of comets with varying parent 45 Sana Ahmed, PRL 45 volatile compositions The evolution of the Galactic dust in the Solar 46 Anuj Gupta, Panjab University 46 neighborhood Cometary Dust Particles: reliable relics from the 47 Prithish Halder, PRL 47 Solar Protoplanetary phase Status of IDP flux models and observations in the 48 Jayesh Pabari, PRL 48 inner solar system High Resolution Mg and Si Isotopic Measurements 49 of Presolar Silicates: Insights into diverse stellar Manish Sanghani, PRL 49 origins and the Galactic Chemical Evolution (GCE) Short-Lived Radionuclides (SLRs) in the Early Solar 50 Tejpreet Kaur, Panjab University 50 System Tushar Bhatt, Kadi Sarva 51 Solar wind interaction with magnosheath of Saturn 51 Vishwavidualaya NAVA payload: Identification of the array detector 52 and recent developments on front-end and processing Rahul Pathak, PRL 52 electronics Development of Langmuir Probe Electronics for 53 Chandan Kumar, PRL 53 LPEX payload for future Mars mission Development of In-situ Measurement Technique for 54 Sanjeev Mishra, PRL 54 Water Ice Detection for Planetary Applications Design and Testing of X-Band Radio Occultation 55 Sonam Jitarwal, PRL 55 Transmitter and Receiver for future Mars Mission Development of Dynamic Feedback Instrumentation 56 for Optimizing Drilling Performance on Lunar South Nilay Awasthi, Amity University 56 Pole Terrain with varying Slope Review of sublimation rates, thermal modeling, and 57 design factors for integrated heat probe lunar drill for Vedanth Sharma, IIT Bombay 57 the sampling of subsurface ice in the lunar south pole Quantitative Assessment of Errors in the Radio 58 Keshav Ram Tripathi, SPL 58 Occultation profiling Laser-induced breakdown spectroscopy (LIBS) study Abhishek Rai, University of 59 of impactites and related rocks from Lonar Crater, 59 Allahabad India - An Ideal terrestrial analogue Spacecraft Autonomous Navigation with Space 60 Arpana Aravindakshan, LEOS 60 bodies as targets for planetary missions No Details Speaker Page No Analysis of Optimal Interplanetary Transfers using 61 Suchismita Choudhury, VSSC 61 Solar-Electric Propulsion Cosmogenic radioisotopes in surface dust collected Narendra Bhandari, Science & 62 62 from asteroids Spirituality Research Institute Dwarf planet Ceres: Inner or outer solar system 63 Guneshwar Thangjam, NISER 63 origin? Anatomy of Iron meteorite: Understanding core of a 64 Dwijesh Ray, PRL 64 differentiated asteroid Aqueous alteration in CM2 chondrite Jbilet 65 Winselwan as analog of alteration processes on Rahul Das Gupta, NISER 65 asteroid Ceres Alteration of Fe-Ni-S metal phase in Mukundpura 66 Dipak Panda, PRL 66 meteorite. Mössbauer Spectroscopic study of Mukundpura CM2 67 Ambesh Dixit, IIT Jodhpur 67 carbonaceous Chondrite at 30 K Fine-grained rims (FGRs) in Mukundpura CM2: 68 Shivani Baliyan, PRL 68 Implications for in situ parent body alteration Shribharath Balakrishnan, IIT 69 Formation and evolution of rings around small bodies 69 Kanpur K. Balasubramanian, Mepco Raman Spectroscopic Study on Silicon Carbide 70 Schlenk Engineering College, 70 Polytype Distribution in Circumstellar Condition Tamil Nadu Basement deep impact event as evidenced from a Saranya R Chandran, University 71 71 melt rock at Lonar Impact Crater, Central India of Kerala The origin of Insoluble organic matter in meteorites: 72 Shreeya Natrajan, PRL 72 A Multi-technique study 73 Indian Sample curation and processing facility Ramakant Mahajan, PRL 73 POSTER Presentation Simulations of the solar wind crafted Martian 1 Arnab Basak, IISER 74 environment Dust distribution within a vortex and its significance 2 Shefali Uttam, PRL 75 for Mars 3 Mathematical Modelling of Martian Dust Storm Foram Joshi, G.H. Patel College 76 Modelling of CO (a3π) Cameron bands in the 4 Masoom Jethwa, PRL 77 Martian atmosphere A universal tool to retrieve
Recommended publications
  • 10Great Features for Moon Watchers
    Sinus Aestuum is a lava pond hemming the Imbrium debris. Mare Orientale is another of the Moon’s large impact basins, Beginning observing On its eastern edge, dark volcanic material erupted explosively and possibly the youngest. Lunar scientists think it formed 170 along a rille. Although this region at first appears featureless, million years after Mare Imbrium. And although “Mare Orien- observe it at several different lunar phases and you’ll see the tale” translates to “Eastern Sea,” in 1961, the International dark area grow more apparent as the Sun climbs higher. Astronomical Union changed the way astronomers denote great features for Occupying a region below and a bit left of the Moon’s dead lunar directions. The result is that Mare Orientale now sits on center, Mare Nubium lies far from many lunar showpiece sites. the Moon’s western limb. From Earth we never see most of it. Look for it as the dark region above magnificent Tycho Crater. When you observe the Cauchy Domes, you’ll be looking at Yet this small region, where lava plains meet highlands, con- shield volcanoes that erupted from lunar vents. The lava cooled Moon watchers tains a variety of interesting geologic features — impact craters, slowly, so it had a chance to spread and form gentle slopes. 10Our natural satellite offers plenty of targets you can spot through any size telescope. lava-flooded plains, tectonic faulting, and debris from distant In a geologic sense, our Moon is now quiet. The only events by Michael E. Bakich impacts — that are great for telescopic exploring.
    [Show full text]
  • 2D Mercury Crater Wordsearch V2
    3/24/2019 Word Search Generator :: Create your own printable word find worksheets @ A to Z Teacher Stuff MAKE YOUR OWN WORKSHEETS ONLINE @ WWW.ATOZTEACHERSTUFF.COM NAME:_______________________________ DATE:_____________ Craters on Mercury SICINIMODFIQPVMRQSLJ BEETHOVEN MICHELANGELO BLTVPTSDUOMRCIPDRAEN BYRON RAPHAEL YAPVWYPXSEHAUEHSEVDI CUNNINGHAM SAVAGE RRZAYRKFJROGNIGSNAIA DAMER SHAKESPEARE ORTNPIVOCDTJNRRSKGSW DOMINICI SVEINSDOTTIR NOMGETIKLKEUIAAGLEYT DRISCOLL TOLSTOI PCLOLTVLOEPSNDPNUMQK ELLINGTON VANGOGH YHEGLOAAEIGEGAHQAPRR FAULKNER VIEIRADASILVA NANHIDLNTNNNHSAOFVLA HEMINGWAY VIVALDI VDGYNSDGGMNGAIEDMRAM HOLST GALQGNIEBIMOMLLCNEZG HOMER VMESTIWWKWCANVEKLVRU IMHOTEP ZELTOEPSBOAWMAUHKCIS IZQUIERDO JRQGNVMODREIUQZICDTH JOPLIN SHAKESPEARETOLSTOIOX KIPLING BBCZWAQSZRSLPKOJHLMA LANGE SFRLLOCSIRDIYGSSSTQT LARROCHA FKUIDTISIYYFAIITRODE LENGLE NILPOJHEMINGWAYEGXLM LENNON BEETHOVENRYSKIPLINGV MARKTWAIN 1/2 Mercury Craters: Famous Writers, Artists, and Composers: Location and Sizes Beethoven: Ludwig van Beethoven (1770−1827). German composer and pianist. 20.9°S, 124.2°W; Diameter = 630 km. Byron: Lord Byron (George Byron) (1788−1824). British poet and politician. 8.4°S, 33°W; Diameter = 106.6 km. Cunningham: Imogen Cunningham (1883−1976). American photographer. 30.4°N, 157.1°E; Diameter = 37 km. Damer: Anne Seymour Damer (1748−1828). English sculptor. 36.4°N, 115.8°W; Diameter = 60 km. Dominici: Maria de Dominici (1645−1703). Maltese painter, sculptor, and Carmelite nun. 1.3°N, 36.5°W; Diameter = 20 km. Driscoll: Clara Driscoll (1861−1944). American glass designer. 30.6°N, 33.6°W; Diameter = 30 km. Ellington: Edward Kennedy “Duke” Ellington (1899−1974). American composer, pianist, and jazz orchestra leader. 12.9°S, 26.1°E; Diameter = 216 km. Faulkner: William Faulkner (1897−1962). American writer and Nobel Prize laureate. 8.1°N, 77.0°E; Diameter = 168 km. Hemingway: Ernest Hemingway (1899−1961). American journalist, novelist, and short-story writer. 17.4°N, 3.1°W; Diameter = 126 km.
    [Show full text]
  • Modeling and Mapping of the Structural Deformation of Large Impact Craters on the Moon and Mercury
    MODELING AND MAPPING OF THE STRUCTURAL DEFORMATION OF LARGE IMPACT CRATERS ON THE MOON AND MERCURY by JEFFREY A. BALCERSKI Submitted in partial fulfillment of the requirements for the degree of Doctor of Philosophy Department of Earth, Environmental, and Planetary Sciences CASE WESTERN RESERVE UNIVERSITY August, 2015 CASE WESTERN RESERVE UNIVERSITY SCHOOL OF GRADUATE STUDIES We hereby approve the thesis/dissertation of Jeffrey A. Balcerski candidate for the degree of Doctor of Philosophy Committee Chair Steven A. Hauck, II James A. Van Orman Ralph P. Harvey Xiong Yu June 1, 2015 *we also certify that written approval has been obtained for any proprietary material contained therein ~ i ~ Dedicated to Marie, for her love, strength, and faith ~ ii ~ Table of Contents 1. Introduction ............................................................................................................1 2. Tilted Crater Floors as Records of Mercury’s Surface Deformation .....................4 2.1 Introduction ..............................................................................................5 2.2 Craters and Global Tilt Meters ................................................................8 2.3 Measurement Process...............................................................................12 2.3.1 Visual Pre-selection of Candidate Craters ................................13 2.3.2 Inspection and Inclusion/Exclusion of Altimetric Profiles .......14 2.3.3 Trend Fitting of Crater Floor Topography ................................16 2.4 Northern
    [Show full text]
  • Planetológiai Helyesírási Tanácsadó
    Planetológiai helyesírási tanácsadó GEOLÓGIA Kőzetrétegtani egységek ridged member = gerinces tagozat Heveliusi Formáció, Hold Geokronológia (idő) imbriumi időszak kora-imbriumi kor noachi időszak Kronosztratigráfia (időrétegtani)(kőzettestek) imbriumi rendszer alsó-imbriumi sorozat noachi rendszer Az egyes egységek magyar elnevezései MERKÚR kuiperi mansuri calorisi tolsztoji pretolsztoji VÉNUSZ aureliai atlai guinevrai ruszalkai laviniai sigrúni fortunai prefortunai HOLD kopernikuszi eratoszthenészi imbriumi nektári prenektári (procellárumi: elavult) MARS amazoni heszperiai noachi prenoachi MARS - geokémiai sideriki theiiki phylloci (ejtsd: filloszi) GEOGRÁFIA Bolygófelszíni alakzatok elnevezései Köznévi taggal (az alábbiakat mindig kötőjellel kapcsoljuk, kivéve birtokos esetben: Cassini-régió, de: Válságok tengere) Megjegyzések: • Az itt felsorolt alakok: latin alak egyes szám, többes szám [latin alak latinos kiejtése], magyar megfelelő • A ¯ jel az előtte álló u-n vagy e-n lévő vonalékezet • A toldalékok a (magyar vagy latin) nevekhez általában közvetlenül kapcsolódnak, a szükséges hasonulások vagy a szóvégi magánhangzó nyúlásának a jelölésével: Caloris Montesszal, Lavinia Planitián, Ión. • A két különírt tagból álló latin elnevezésekhez az -i/-beli képzô kötôjellel kapcsolódik; az eredeti kis- és nagybetûket megtartjuk: Caloris Planitia-i, Sinus Meridiani-beli stb. (vö. AkH. 1984: 217. b) pont). A két különírt tagból álló magyar elnevezéseknél az -i képzôs forma: Halál tavabeli, Méz tengerebeli, Rothadás mocsarabeli, Szivárvány öblebeli
    [Show full text]
  • SELENOLOGY the Journal of the American Lunar Society
    DEVOTED TO THE STUDY OF EARTH’S MOON VOL. 26 NO. 2 SUMMER 2007 SELENOLOGY The Journal of The American Lunar Society Selenology Vol. 26 No. 2 - Summer 2007 The official journal of the American Lunar Society, an organization devoted to the observation and discovery of the earth’s moon TABLE OF CONTENTS: Cassini A and the Washbowl: As Described by Wilkins and Moore ......... 2 On Closer Examination .......................................................................... 6 Vertical Displacement of Features in the Montes Spitzbergensis Area ....... 15 COVER: Cassini Crater imaged by Wes Higgins on August, 25 2005 at 10:45 UT with a 45 cm Newtonian telescope. Selenology, Vol. 26 No. 2, Summer 2007. A publication of the American Lunar Society. President: Eric Douglass; Vice President: Steve Boint; Editor: Francis G. Graham. Web site: http://amlunsoc.org/ Layout/design by A Distant Wind (www.distantwind.com) This issue edited by Steve Boint. Copyright © 2007 by the American Lunar Society and individual authors; all rights reserved. Send manuscripts, general observations, photographs, drawings and other correspondence to: Steve Boint, VP ALS, 1807 S. Spring Ave., Sioux Falls, SD 57105 E-mail: [email protected] Send changes of address to Eric Douglass at [email protected] If you don’t have e-mail, send them to Steve Boint Page 2 SELENOLOGY Vol. 26 No. 2 Cassini A and the Washbowl: As Described by Wilkins and Moore By Raffaello Lena, Maria Teresa Bregante, Eric Douglass and Giorgio Mengoli GLR group 1. INTRODUCTION degrees. When the colongitude In this article, we report on is the same, on different several observations made by cycles, the lighting conditions the Geologic Lunar Research are similar.
    [Show full text]
  • Distribution and Volumes of Lava Ponds in the Orientale Region of the Moon
    DISTRIBUTION AND VOLUMES OF LAVA PONDS IN THE ORIENTALE REGION OF THE MOON. Lisa R. Gaddis and James W. Head, Dept, of Geological Sciences, Brown University, Providence, R. I, 02912 Stratigraphic and volumetric studies of mare deposits on the Moon have generally been restricted to areas which display several stages of mare fil- ling (1-3). With the notable exception of the Imbrium flows (4), little work has been done on the volumes and extent of individual flows and small volcanic deposits isolated by nap-mare units. Informati on cn these small mare deposits or lava ponds could lead to a better understanding of minimum eruption volumes, the relati onship between these volumes and associated vent characteristics , and their eruption conditions. In addition, the distribution and mode of occurrence of small lava ponds may be useful in determining the nature of the early stages of volcanism in the highland crust. One approach to this problem is LO examine individual lava ponds in high- land areas adjacent to the major lunar maria. The purpose of this study is to present an analysis of such an area, between Mare Orientale and southwestern Oceanus Procell arum, in order to further characterize erupti on vol umes and the relation of volcanism to the lunar crustal environment. Distribution of Lava Ponds - Lava ponds chosen for this study are con- centrated in an arc between Mare Orientale and southwestern Oceanus Procellarum (Figure 1). Of the thirty-three ponds analyzed, eleven are located within the mu1 ti-ringed basin of Orientale (nos. 1 - ll), ten occur predominantly in crater floors (nos.
    [Show full text]
  • From Here to There: the Odyssey of the Liberal Arts
    FROM HERE TO THERE: THE ODYSSEY OF THE LIBERAL ARTS Selected Proceedings from the Thirteenth Annual Conference of the Association for Core Texts and Courses Williamsburg, VA, March 29–April 1, 2007 Edited by Roger Barrus John Eastby J. Scott Lee Contents Acknowledgments Introduction Roger Barrus and John Eastby ix Odysseys in Poetry and Epic Petrarch’s Triumphs: An Introduction to Humanism and the Renaissance Ann Dunn 3 Shakespeare’s Sonnet 73: Drama in Lyric Poetry Stephen Zelnick 11 The Mahabharata Patricia M. Greer 17 Hospitality Re-visioned: Odysseus’s Recognitions in Book 14 Kathleen Marks 23 The Homeric Question: Is the Odyssey a Great Book? Paul A. Cantor 27 iv Contents Odysseys in Modern Creative Prose “Good Surviving”: Heroes, Heroines, and Realism in Dickens’s Early Novels Sandra A. Grayson 41 Mentorship in Soseki’s Kokoro Richard Myers 45 Odyssey of Despair: Using Chiasmus to Examine the Domestic Sphere in Leo Tolstoy’s Anna Karenina Arthur Rankin 49 The Odyssey of Reading Proust Erik Liddell 53 My Journey with James Joyce Nicholas Margaritis 61 Creative Writing and the Classics: Contrapuntal Music Steven Faulkner 67 Bronzeville Odyssey: The Literary Legacy of Gwendolyn Brooks Joanne V. Gabbin 71 Odysseys in the Political World “Family Values” in Livy’s Rome Joseph Knippenberg 81 One Story: An Approach to Teaching the History of Political Philosophy in One Semester Joseph Lane 87 Ethics, Espionage, and War Daniel G. Lang 97 Using The Good Woman of Setzuan to Illuminate The Communist Manifesto Kathleen A. Kelly 103 Contents v Actualizing Memory Nafisi’s Way: Reading Homer in El Paso Ronald J.
    [Show full text]
  • Rimae Sirsalis
    RIMAE SIRSALIS Nieves del Río, José Castillo, Eduardo Adarve, Jorge Arranz y Alberto Martos del Grupo de Estudios Lunares “Enrique Silva”. [Página dejada intencionadamente en blanco] - 2 - INTRODUCCIÓN Rimae Sirsalis es un sistema de grietas que comprende dos estructuras de esta clase, Rima Sirsalis y Rima Sirsalis I, siendo la primera mucho más larga y mucho más perceptible que la segunda. Pertenecen a la clase de grietas rectas, cuyo aspecto es diferente del aspecto de las grietas circulares que bordean las cuencas de las grandes estructuras de impacto. Lo que tiene de particular este sistema, para que haya merecido figurar como objetivo 1 en el apartado “Call for Observations 2”, del boletín TLO 3 de ALPO 4, son sus dos características principales: siendo Rima Sirsalis la grieta más larga existente en la cara cislunar (la visible), está situada en una región cuyo suelo es geológicamente distinto de la naturaleza de suelos por los que discurren en general las grietas lunares. En efecto, las grietas lunares (llamadas en latín rimae ) son siempre estructuras volcánicas, generalmente túneles de lava cuyo techo se ha desplomado, o surcos por los cuales fluyó la lava en su día, en favor de la pendiente del suelo. Por esta razón, se las encuentra siempre sobre terrenos magmáticos, como los maria (plural de mare ), los sini (plural de sinus ), los laci (plural de lacus ), o los paludes (plural de palus ), o sea sobre los “mares”, las “bahías”, los “lagos” o las “marismas” lunares. Como ejemplos de esta condición se puede citar a Rimae Hypatia, situada en el Mare Tranquillitatis, a Rima Oppolzer, en Sinus Medii, a Rimae Bürg y Rimae Daniell, en Lacus Mortis y Lacus Somniorum, respectivamente y Rima Hesiodus en Palus Epidemiarum.
    [Show full text]
  • IAU Mercurian Nomenclature
    Appendix 1 IAU Mercurian Nomenclature 1. IAU Nomenclature Rules Since its inception in Brussels in 1919 [1], the International Astronomical Union (IAU) has gradually developed a planetary nomenclature system that has evolved from a purely classically based system into a quite so- phisticated attempt to broaden the cultural base of the names approved for planetary bodies and surface features. At present, name selection is guided by 11 rules (quoted verbatim below) in addition to conventions decided upon by nomenclature task groups for individual Solar System bodies. The general rules are as follows1: 1. Nomenclature is a tool and the first consideration should be to make it simple, clear, and unambiguous. 2. In general, official names will not be given to features whose longest di- mensions are less than 100 metres, although exceptions may be made for smaller features having exceptional scientific interest. 3. The number of names chosen for each body should be kept to a minimum. Features should be named only when they have special scientific inter- est, and when the naming of such features is useful to the scientific and cartographic communities at large. 4. Duplication of the same surface feature name on two or more bodies, and of the same name for satellites and minor planets, is discouraged. Duplications may be allowed when names are especially appropriate and the chances for confusion are very small. 5. Individual names chosen for each body should be expressed in the language of origin. Transliteration for various alphabets should be given, but there will be no translation from one language to another.
    [Show full text]
  • Factoring Origin of Life Hypotheses Into the Search for Life in the Solar System and Beyond
    life Review Factoring Origin of Life Hypotheses into the Search for Life in the Solar System and Beyond Alex Longo 1,2,* and Bruce Damer 3,4 1 National Aeronautics and Space Administration Headquarters, Washington, DC 20546, USA 2 Department of Geology, The University of North Carolina, Chapel Hill, NC 27599, USA 3 Department of Biomolecular Engineering, University of California, Santa Cruz, CA 95064, USA; [email protected] or [email protected] 4 Digital Space Research, Boulder Creek, CA 95006, USA * Correspondence: [email protected] or [email protected] Received: 17 February 2020; Accepted: 22 April 2020; Published: 27 April 2020 Abstract: Two widely-cited alternative hypotheses propose geological localities and biochemical mechanisms for life’s origins. The first states that chemical energy available in submarine hydrothermal vents supported the formation of organic compounds and initiated primitive metabolic pathways which became incorporated in the earliest cells; the second proposes that protocells self-assembled from exogenous and geothermally-delivered monomers in freshwater hot springs. These alternative hypotheses are relevant to the fossil record of early life on Earth, and can be factored into the search for life elsewhere in the Solar System. This review summarizes the evidence supporting and challenging these hypotheses, and considers their implications for the search for life on various habitable worlds. It will discuss the relative probability that life could have emerged in environments on early Mars, on the icy moons of Jupiter and Saturn, and also the degree to which prebiotic chemistry could have advanced on Titan. These environments will be compared to ancient and modern terrestrial analogs to assess their habitability and biopreservation potential.
    [Show full text]
  • Feature of the Month—September 2019 Gemma Frisius
    A publication of the Lunar Section of ALPO Edited by David Teske: [email protected] 2162 Enon Road, Louisville, Mississippi, USA Recent back issues: http://moon.scopesandscapes.com/tlo_back.html Feature of the Month—September 2019 Gemma Frisius Sketch by Robert H. Hayes, Jr—Worth, Illinois, USA June 11, 2019 0226-0306; 0328-0340 UT, 15 cm reflector, 170 x Seeing 8-9/10, transparency 6/6 I observed this crater and vicinity on the evening of June 10/11, 2019. This area is located north of Maurolycus and just west of Gemma Frisius itself. Gemma Frisius D (Gem Fri D) is another example of a non-circular crater. Its eastern side is quite round, but its western side has sharp angles. There are straight edges coming to a point on the west end. Its interior shadow also looked odd. The shape may have resulted from slumped walls. Gem Fri D has obliterated the north end of a larger but vague old ring. There is a great variety of craters nearby. Gemma Frisius F is the middling crater just southwest of the old ring. A clump of four smaller craters straddles this old rim. Three more small pits and a fuzzy squarish crater are east of this group. Gemma Frisius Z is the largest crisp feature southwest of D. The Lunar Quad- rant map shows it as single, but I saw it as a double crater. A vague saucer is just east of Z, and a larger, similar saucer is to its north. There is a generous sprinkling of tiny pits in this area.
    [Show full text]
  • Hungarian Localization of the International Planetary Nomenclature System
    3rd INTERNATIONAL CONFERENCE ON CARTOGRAPHY AND GIS 15-20 June, 2010, Nessebar, Bulgaria HUNGARIAN LOCALIZATION OF THE INTERNATIONAL PLANETARY NOMENCLATURE SYSTEM Henrik Hargitai Author: Henrik Hargitai Eötvös Loránd University, Institute of Geography and Earth Sciences, Planetary Science Research Group 1117 Budapest, Pázmány P st 1/1 hhargitai[at]gmail.com Abstract: The paper describes the Hungarian localization of the official IAU nomenclature system of planetary body surface features and planetary body names. The localized forms are recommended for use in texts published in popular science journals and newspapers and books for the general public. Keywords: planetary cartography, Mars, Moon, planetary nomenclature, placenames, toponymy INTRODUCTION The Planetary Nomenclature System is maintained by the Working Group for Planetary System Nomenclature (WGPSN) of the International Astronomical Union, and is published as the Gazetteer of Planetary Nomenclature which is distributed by the U.S. Geological Survey (USGS). Planetary surface feature Place Names consist of two elements: a specific term and a descriptor term. Crater, bright albedo and some other names have no descriptor term. Descriptor terms are in Latin language; for specifics, the original form is retained if the original is using Latin alphabet; if not, a transformation to Latin alphabet is applied. The origin of this system goes back to the 17th century, when the first Lunar maps, especially the Grimaldi-Riccioli map used Latin terms which was a conventional custom of cartographers
    [Show full text]