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Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur
Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur To cite this version: Alex Soumbatov-Gur. Phobos, Deimos: Formation and Evolution. [Research Report] Karpov institute of physical chemistry. 2019. hal-02147461 HAL Id: hal-02147461 https://hal.archives-ouvertes.fr/hal-02147461 Submitted on 4 Jun 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Phobos, Deimos: Formation and Evolution Alex Soumbatov-Gur The moons are confirmed to be ejected parts of Mars’ crust. After explosive throwing out as cone-like rocks they plastically evolved with density decays and materials transformations. Their expansion evolutions were accompanied by global ruptures and small scale rock ejections with concurrent crater formations. The scenario reconciles orbital and physical parameters of the moons. It coherently explains dozens of their properties including spectra, appearances, size differences, crater locations, fracture symmetries, orbits, evolution trends, geologic activity, Phobos’ grooves, mechanism of their origin, etc. The ejective approach is also discussed in the context of observational data on near-Earth asteroids, main belt asteroids Steins, Vesta, and Mars. The approach incorporates known fission mechanism of formation of miniature asteroids, logically accounts for its outliers, and naturally explains formations of small celestial bodies of various sizes. -
A Possible Albian Impact Crater at Murshid, Southern Oman
GeoArabia, Vol. 7, No. 4, 2002 Gulf PetroLink, Bahrain A possible Albian impact crater at Murshid, southern Oman Bruce Levell1, Pascal Richard2 and Folco Hoogendijk2, Petroleum Development Oman ABSTRACT During interpretation of a 3-D seismic survey in southern Oman a solitary, 2.5-km-wide circular basin with a central peak and raised rim was identified in the subsurface 35 km west of the Marmul oil field. The feature is the only one of its kind in the area. The basinal structure is probably of Late Cretaceous (Albian) age and the regional geology strongly suggests that it is neither a volcanic crater nor related to salt-dome tectonics or salt dissolution. It possibly represents a crater formed by a terrestrial impact event and has been named the Murshid crater. This report does not constitute a detailed investigation of the possible impact crater but rather records the 3-D seismic observations and the drilling that has taken place near the structure so far. INTRODUCTION During interpretation of a newly acquired 3-D seismic survey for oil exploration in southern Oman, a solitary 2.5-km-diameter circular basinal feature was identified as a possible impact structure and was named the Murshid crater. It lies 35 km west of the Marmul oil field in the South Oman Salt Basin (Figure 1). The center of the structure is at latitude 18º10’59"N, longitude 54º55’08”E, and it is buried at a depth of approximately 380 m below mean sea level (680 m below the ground surface). The authors are petroleum geologists who felt that the Murshid basinal structure needed reporting to the wider scientific community. -
TRANSIENT LUNAR PHENOMENA: REGULARITY and REALITY Arlin P
The Astrophysical Journal, 697:1–15, 2009 May 20 doi:10.1088/0004-637X/697/1/1 C 2009. The American Astronomical Society. All rights reserved. Printed in the U.S.A. TRANSIENT LUNAR PHENOMENA: REGULARITY AND REALITY Arlin P. S. Crotts Department of Astronomy, Columbia University, Columbia Astrophysics Laboratory, 550 West 120th Street, New York, NY 10027, USA Received 2007 June 27; accepted 2009 February 20; published 2009 April 30 ABSTRACT Transient lunar phenomena (TLPs) have been reported for centuries, but their nature is largely unsettled, and even their existence as a coherent phenomenon is controversial. Nonetheless, TLP data show regularities in the observations; a key question is whether this structure is imposed by processes tied to the lunar surface, or by terrestrial atmospheric or human observer effects. I interrogate an extensive catalog of TLPs to gauge how human factors determine the distribution of TLP reports. The sample is grouped according to variables which should produce differing results if determining factors involve humans, and not reflecting phenomena tied to the lunar surface. Features dependent on human factors can then be excluded. Regardless of how the sample is split, the results are similar: ∼50% of reports originate from near Aristarchus, ∼16% from Plato, ∼6% from recent, major impacts (Copernicus, Kepler, Tycho, and Aristarchus), plus several at Grimaldi. Mare Crisium produces a robust signal in some cases (however, Crisium is too large for a “feature” as defined). TLP count consistency for these features indicates that ∼80% of these may be real. Some commonly reported sites disappear from the robust averages, including Alphonsus, Ross D, and Gassendi. -
Scientific Rationale and Requirements for a Global Seismic Network on Mars
SCIENTIFIC RATIONALE AND REQUIREMENTS FOR A GLOBAL SEISMIC NETWORK ON MARS MARS Model AR 90 EARTH 180 (NASA-CR-188806) SCIENTIFIC RATIONALE AND N92-14949 REQUIREMENTS FOR A GLOBAL SEISMIC NETWORK ON MARS (Lunar and Planetary Inst.) 48 p CSCL 03B Unclas G3/91 0040098 LPI Technical Report Number 91-02 LUNAR AND PLANETARY INSTITUTE 3303 NASA ROAD 1 HOUSTON TX 77058-4399 LPI/TR-91-02 SCIENTIFIC RATIONALE AND REQUIREMENTS FOR A GLOBAL SEISMIC NETWORK ON MARS Sean C. Solomon, Don L. Anderson, W. Bruce Banerdt, Rhett G. Butler, Paul M. Davis, Frederick K. Duennebier, Yosio Nakamura, Emile A. Okal, and Roger J. Phillips Report of a Workshop Held at Morro Bay, California May 7-9, 1990 Lunar and Planetary Institute 3303 NASA Road 1 Houston TX 77058 LPI Technical Report Number 91-02 LPI/TR-91-02 Compiled in 1991 by the LUNAR AND PLANETARY INSTITUTE The Institute is operated by Universities Space Research Association under Contract NASW-4574 with the National Aeronautics and Space Administration. Material in this document may be copied without restraint for library, abstract service, educational, or personal research purposes; however, republication of any portion requires the written permission of the authors as well as appropriate acknowledgment of this publication. This report may be cited as: Solomon S. C. et al. (1991) Scientific Rationale and Requirements far a Global Seismic Network on Mars. LPI Tech. Rpt. 91-02, Lunar and Planetary Institute, Houston. 51 pp. This report is distributed by: ORDER DEPARTMENT Lunar and Planetary Institute 3303 NASA Road 1 Houston TX 77058-4399 Mail order requestors will be invoiced for the cost of shipping and handling. -
March 21–25, 2016
FORTY-SEVENTH LUNAR AND PLANETARY SCIENCE CONFERENCE PROGRAM OF TECHNICAL SESSIONS MARCH 21–25, 2016 The Woodlands Waterway Marriott Hotel and Convention Center The Woodlands, Texas INSTITUTIONAL SUPPORT Universities Space Research Association Lunar and Planetary Institute National Aeronautics and Space Administration CONFERENCE CO-CHAIRS Stephen Mackwell, Lunar and Planetary Institute Eileen Stansbery, NASA Johnson Space Center PROGRAM COMMITTEE CHAIRS David Draper, NASA Johnson Space Center Walter Kiefer, Lunar and Planetary Institute PROGRAM COMMITTEE P. Doug Archer, NASA Johnson Space Center Nicolas LeCorvec, Lunar and Planetary Institute Katherine Bermingham, University of Maryland Yo Matsubara, Smithsonian Institute Janice Bishop, SETI and NASA Ames Research Center Francis McCubbin, NASA Johnson Space Center Jeremy Boyce, University of California, Los Angeles Andrew Needham, Carnegie Institution of Washington Lisa Danielson, NASA Johnson Space Center Lan-Anh Nguyen, NASA Johnson Space Center Deepak Dhingra, University of Idaho Paul Niles, NASA Johnson Space Center Stephen Elardo, Carnegie Institution of Washington Dorothy Oehler, NASA Johnson Space Center Marc Fries, NASA Johnson Space Center D. Alex Patthoff, Jet Propulsion Laboratory Cyrena Goodrich, Lunar and Planetary Institute Elizabeth Rampe, Aerodyne Industries, Jacobs JETS at John Gruener, NASA Johnson Space Center NASA Johnson Space Center Justin Hagerty, U.S. Geological Survey Carol Raymond, Jet Propulsion Laboratory Lindsay Hays, Jet Propulsion Laboratory Paul Schenk, -
A Study About the Temporal Constraints on the Martian Yardangs’ Development in Medusae Fossae Formation
remote sensing Article A Study about the Temporal Constraints on the Martian Yardangs’ Development in Medusae Fossae Formation Jia Liu 1,2 , Zongyu Yue 1,3,*, Kaichang Di 1,3 , Sheng Gou 1,4 and Shengli Niu 4 1 State Key Laboratory of Remote Sensing Science, Aerospace Information Research Institute, Chinese Academy of Sciences, Beijing 100101, China; [email protected] (J.L.); [email protected] (K.D.); [email protected] (S.G.) 2 University of Chinese Academy of Sciences, Beijing 100049, China 3 CAS Center for Excellence in Comparative Planetology, Hefei 230026, China 4 State Key Laboratory of Lunar and Planetary Sciences, Macau University of Science and Technology, Macau 999078, China; [email protected] * Correspondence: [email protected]; Tel.: +86-10-64889553 Abstract: The age of Mars yardangs is significant in studying their development and the evolution of paleoclimate conditions. For planetary surface or landforms, a common method for dating is based on the frequency and size distribution of all the superposed craters after they are formed. However, there is usually a long duration for the yardangs’ formation, and they will alter the superposed craters, making it impossible to give a reliable dating result with the method. An indirect method by analyzing the ages of the superposed layered ejecta was devised in the research. First, the layered ejecta that are superposed on and not altered by the yardangs are identified and mapped. Then, the ages of the layered ejecta are derived according to the crater frequency and size distribution on them. These ages indicate that the yardangs ceased development by these times, and the ages are valuable for studying the evolution of the yardangs. -
Bibliographyof Space Books Andarticlesfrom Non
https://ntrs.nasa.gov/search.jsp?R=19800016707N 2020-03-11T18:02:45+00:00Zi_sB--rM-._lO&-{/£ 3 1176 00167 6031 HHR-51 NASA-TM-81068 ]9800016707 BibliographyOf Space Books And ArticlesFrom Non-AerospaceJournals 1957-1977 _'C>_.Ft_iEFERENC_ I0_,'-i p,,.,,gvi ,:,.2, , t ,£}J L,_:,._._ •..... , , .2 ,IFER History Office ...;_.o.v,. ._,.,- NASA Headquarters Washington, DC 20546 1979 i HHR-51 BIBLIOGRAPHYOF SPACEBOOKS AND ARTICLES FROM NON-AEROSPACE JOURNALS 1957-1977 John J. Looney History Office NASA Headquarters Washlngton 9 DC 20546 . 1979 For sale by the Superintendent of Documents, U.S. Government Printing Office Washington, D.C. 20402 Stock Number 033-000-0078t-1 Kc6o<2_o00 CONTENTS Introduction.................................................... v I. Space Activity A. General ..................................................... i B. Peaceful Uses ............................................... 9 C. Military Uses ............................................... Ii 2. Spaceflight: Earliest Times to Creation of NASA ................ 19 3. Organlzation_ Admlnlstration 9 and Management of NASA ............ 30 4. Aeronautics..................................................... 36 5. BoostersandRockets............................................ 38 6. Technology of Spaceflight....................................... 45 7. Manned Spaceflight.............................................. 77 8. Space Science A. Disciplines Other than Space Medicine ....................... 96 B. Space Medicine ..............................................119 C. -
Pre-Mission Insights on the Interior of Mars Suzanne E
Pre-mission InSights on the Interior of Mars Suzanne E. Smrekar, Philippe Lognonné, Tilman Spohn, W. Bruce Banerdt, Doris Breuer, Ulrich Christensen, Véronique Dehant, Mélanie Drilleau, William Folkner, Nobuaki Fuji, et al. To cite this version: Suzanne E. Smrekar, Philippe Lognonné, Tilman Spohn, W. Bruce Banerdt, Doris Breuer, et al.. Pre-mission InSights on the Interior of Mars. Space Science Reviews, Springer Verlag, 2019, 215 (1), pp.1-72. 10.1007/s11214-018-0563-9. hal-01990798 HAL Id: hal-01990798 https://hal.archives-ouvertes.fr/hal-01990798 Submitted on 23 Jan 2019 HAL is a multi-disciplinary open access L’archive ouverte pluridisciplinaire HAL, est archive for the deposit and dissemination of sci- destinée au dépôt et à la diffusion de documents entific research documents, whether they are pub- scientifiques de niveau recherche, publiés ou non, lished or not. The documents may come from émanant des établissements d’enseignement et de teaching and research institutions in France or recherche français ou étrangers, des laboratoires abroad, or from public or private research centers. publics ou privés. Open Archive Toulouse Archive Ouverte (OATAO ) OATAO is an open access repository that collects the wor of some Toulouse researchers and ma es it freely available over the web where possible. This is an author's version published in: https://oatao.univ-toulouse.fr/21690 Official URL : https://doi.org/10.1007/s11214-018-0563-9 To cite this version : Smrekar, Suzanne E. and Lognonné, Philippe and Spohn, Tilman ,... [et al.]. Pre-mission InSights on the Interior of Mars. (2019) Space Science Reviews, 215 (1). -
Globular Clusters and Galactic Nuclei
Scuola di Dottorato “Vito Volterra” Dottorato di Ricerca in Astronomia– XXIV ciclo Globular Clusters and Galactic Nuclei Thesis submitted to obtain the degree of Doctor of Philosophy (“Dottore di Ricerca”) in Astronomy by Alessandra Mastrobuono Battisti Program Coordinator Thesis Advisor Prof. Roberto Capuzzo Dolcetta Prof. Roberto Capuzzo Dolcetta Anno Accademico 2010-2011 ii Abstract Dynamical evolution plays a key role in shaping the current properties of star clus- ters and star cluster systems. We present the study of stellar dynamics both from a theoretical and numerical point of view. In particular we investigate this topic on different astrophysical scales, from the study of the orbital evolution and the mutual interaction of GCs in the Galactic central region to the evolution of GCs in the larger scale galactic potential. Globular Clusters (GCs), very old and massive star clusters, are ideal objects to explore many aspects of stellar dynamics and to investigate the dynamical and evolutionary mechanisms of their host galaxy. Almost every surveyed galaxy of sufficiently large mass has an associated group of GCs, i.e. a Globular Cluster System (GCS). The first part of this Thesis is devoted to the study of the evolution of GCSs in elliptical galaxies. Basing on the hypothesis that the GCS and stellar halo in a galaxy were born at the same time and, so, with the same density distribution, a logical consequence is that the presently observed difference may be due to evolution of the GCS. Actually, in this scenario, GCSs evolve due to various mechanisms, among which dynamical friction and tidal interaction with the galactic field are the most important. -
Water on the Moon, III. Volatiles & Activity
Water on The Moon, III. Volatiles & Activity Arlin Crotts (Columbia University) For centuries some scientists have argued that there is activity on the Moon (or water, as recounted in Parts I & II), while others have thought the Moon is simply a dead, inactive world. [1] The question comes in several forms: is there a detectable atmosphere? Does the surface of the Moon change? What causes interior seismic activity? From a more modern viewpoint, we now know that as much carbon monoxide as water was excavated during the LCROSS impact, as detailed in Part I, and a comparable amount of other volatiles were found. At one time the Moon outgassed prodigious amounts of water and hydrogen in volcanic fire fountains, but released similar amounts of volatile sulfur (or SO2), and presumably large amounts of carbon dioxide or monoxide, if theory is to be believed. So water on the Moon is associated with other gases. Astronomers have agreed for centuries that there is no firm evidence for “weather” on the Moon visible from Earth, and little evidence of thick atmosphere. [2] How would one detect the Moon’s atmosphere from Earth? An obvious means is atmospheric refraction. As you watch the Sun set, its image is displaced by Earth’s atmospheric refraction at the horizon from the position it would have if there were no atmosphere, by roughly 0.6 degree (a bit more than the Sun’s angular diameter). On the Moon, any atmosphere would cause an analogous effect for a star passing behind the Moon during an occultation (multiplied by two since the light travels both into and out of the lunar atmosphere). -
Massachusetts Inst. of Thch.) 666 P HC A9NATIF A0L AEOA, CSCD 03F Unclas
lo2 to the " NATIONAL AERONAUTICS AND SPACE ADMINISTRATION Contract NAS9-12334 -APOLLOPASSIVE SEISMICEXPERIMENT PARTICIPATION 'I NASA-CR-151882) LUNAR SEISMOLOGY: THE 1479-17782 INTERNAL STRUCTURE ORHE LOt Ph. Thesis (Massachusetts Inst. of Thch.) 666 p HC A9NATIF A0L AEOA, CSCD 03f Unclas 1 Januarya-19-12 -o 3.0 September .1978 G3/91' 1351 0 M. Nafi Toksbz- Principal Investigator Department of Earth and Planetar SciencesO Massachusetts Institute of Technology Cambridge, Massachusetts 02139 LUNAR SEISMOLOGY: THE INTERNAL STRUCTURE OF THE MOON by -Neal Rodney Goins Submitted to the Department of-Earth -and Planetary Sciences on May 24,.1978, in parti&l .flfillment of the requirements for the degree of Doctor of Philosophy.. ABSTRACT, A primary goal of-the Apollo missions was the exploration and scientific study of the moon. The nature of the lunar interior is of particular interest for comparison with the earth and in studying comparative planetology. The principal experiment designed to study the lunar interior was the passive seismic experiment (PSE) included as part of the science package on missions 12, 14, 15, and 16. Thus seis mologists were provided with a uniqueopportunity ta study the seismicity and seismic characteristics of a second planetary 'bdy and ascertain if analysis methods developed on earth could illuminate the structure of the lunar interior. The lunar seismic data differ from terrestrial data in three major respects. First, the seismic sources are much smaller than on earth, so that no significant information has -been yet obtained for the 4v/ry deep lunar interior. Second, a strong, high Q scattering layer exists on the surface of the moon, resulting in very emergent seismic arrivals, long ringing-codas that obscure secondary (later arriving)-phases., and 'the-destruction of coherent dispersed surface wave trains. -
NASA Advisory Council Planetary Protection Subcommittee, May 20‐21, 2014
NASA Advisory Council Planetary Protection Subcommittee, May 20‐21, 2014 NASA ADVISORY COUNCIL Planetary Protection Subcommittee May 20-21, 2014 NASA Headquarters Washington, D.C. MEETING MINUTES _____________________________________________________________ Eugene Levy, Chair ____________________________________________________________ Gale Allen, Executive Secretary Report prepared by Joan M. Zimmermann Zantech IT, Inc. 1 NASA Advisory Council Planetary Protection Subcommittee, May 20-2t 2014 Table of Contents Introduction 3 PPO Update and Review 3 MSL Lessons Learned 5 InSight Status 8 Planetary Science and Mars Program Update 10 Contamination Limits for Planetary Life Detection 12 Mars Landing Site Selection Process 14 ESA 2018 Landing Site Selection 15 Mars 2020 Project Status 15 Public Comment 16 Discussion 16 Ethics Briefing 17 Discussion 17 Science Mission Directorate and Planetary Protection 17 Update on Special Regions Parameters 19 Status of Phobos /Demos Materials 21 Outer Solar System Special Regions: Enceladus and Beyond 22 JAXA Sample Return Working Group 23 Public Comment 24 Discussion 25 Appendix A- Attendees Appendix 8- Membership roster Appendix C- Presentations Appendix D- Agenda 2 NASA Advisory Council Planetary Protection Subcommittee, May 20-2t 2014 May 20.2014 Introduction The Executive Secretary of the Planetary Protection Subcommittee (PPS), Dr. Gale Allen, made preparatory announcements. Dr. Eugene Levy, PPS Chair, opened the meeting and noted there would be a heavy focus on Mars exploration, as it has become a timely and important issue. Introductions were made around the meeting room. Planetary Protection Office Update and Review Dr. Catharine Conley, Planetary Protection Officer (PPO) for NASA, briefly described the broad base of experience in the PPS, and reviewed the purpose of Planetary Protection (PP) and the policy, as it applies to all missions.