Four-Dimensional B-Spline Algorithm for Mars Crater Reconstruction
Total Page:16
File Type:pdf, Size:1020Kb
Load more
Recommended publications
-
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). -
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 -
Moore Et Al., 1977
JOURNAL OF GEOPHYSICAL RESEARCH, VOL. 98, NO. E2, PAGES 3413-3429, FEBRUARY 25, 1993 SOIL TEXTURE AND GRANULOMETRY AT THE SURFACE OF MARS Audouin Dollfus and Marc Deschamps Observatoire de Paris, Meudon, France James R. Zimbelman Center for Earth and Planetary Sciences, National Air and Space Museum Smithsonian Institution, Washington, D. C. The physical behavior of the Martian surface soil has been characterized remotely by both photopolarimetry and radiometry. The degree of linear polarization defines a coefficient b which is related to the top surface soil texture and is calibrated in terms of grain size, or as a fraction of the area exhibiting uncovered clean rocks. This coefficient b was recorded with the instrument VPM (Visual Polarimeter Mars) on board Soviet orbiter MARS 5 in 1974. The radiometric thermal inertia coefficient I is essentially a measurement of the soil compaction, or an effective average particle size in the soil texture, through the few decimeters below the top surface sensed by polarimetry. The instrument IBTM (Infra Bed Thermal Mapper) was used on board the Viking spacecraft between 1976 and 1982. The polarimetric scans raked a strip covering two contrasting regions, the dark-hued Mare Erythraeum and the light-hued Thaumasia. Over these wide areas, several smaller typical terrains were characterized by the three parameters A (albedo), b (related to top surface grain size) and I (underlaying compaction or block size). The large dark region Erythraeum is characterized everywhere by a uniform polarization response, despite the large geomorphological diversity of the surface. The values of A and b indicate a ubiquitous coating or mantling with small dark grains of albedo 12.7%, with a radius of 10 to 20 urn. -
Annual Progress Report
? ASTRDGEOLOGIC ANNUAL PROGRESS REPORT July 1, 1964 to c July 1, 1965 xov&iiib&r1365 This preliminary report is distributed without editorial and technical review for conformity with official standards and nomenclature. It should not be quoted without permission. This report concerns work done on behalf of the National Aeronautics and Space Administration. DEPARTMENT OF THE INTERIOR UNITED STATES GEOIX)(;ICAL SURVEY 6 F DISTRIBUTION No. of Copies National Aeronautics and Space Administration Washington, D.C. ......................... -20 U.S. Geological Survey ...................... .10 A'~elsoii, Dr. P. E., Oirector Geophysical Laboratory Carnegie Institution Washington, D.C. .......................... 1 Allen, Mr. H. J. Ames Research Center Moffett Field, California. ..................... 1 Babcock, Dr. H. W., Director Mt. Wilson and Palomar Observatories Mount Wilson, California ...................... 1 Beattie, Mr. D. A. National Aeronautics and Space Administration Washington, D.C. ......................... .1 Brown, Professor Harrison Division of Geological Sciences California Institute of Technology Pasadena, California ........................ 1 Bryson, Mr. R. P. National Aeronautics and Space Administration Washington, D.C. .......................... 2 Cannell, Mr. W. D. Aeronautical Chart and Information Center Lowell Observatory Flagstaff, Arizona ......................... 1 Carder, Mr. R. W. Aeronautical Chart and Information Center Second and Arsenal Streets St. Louis, Missouri. ........................ 1 Chapman, 'Dr. D. -
MECA Workshop on Dust on Mars. Program, Abstracts
MECA WORKSHOP ON DUST ON MARS Sponsored by NASA and The Lunar and Planetary Institute Hosted by Arizona State University February 24-25, 1986 RECEIVED FEB 18 1986 PRGiECTS OFFICE CONTENTS PROGRAM . • • • • • • . • • • • • . • 1 ABSTRACTS On the rate of formation of sedimentary debris on Mars ••••••••••5 R.E. Arvidson Constraining Mars-dust mineralogy on the basis of Viking biology simulations and Mars spectral reflectance ••••••••••••••••6 ,. A. Banin Implications of a polar warming for dust transport into the North Polar region of Mars •••••••••••••••••••••••••••8 J.R. Barnes and J.L. Hollingsworth Dust deposition and erosion on Mars: Cyclic development of regional deposits • • • •••• •••••••••••, ••••••10 P.R. Christensen Surface albedo variations on Mars: Implications for yearly dust deposition and removal •••••••. • • • • 13 P.R. Christensen Influence of dust on water condensation at Mars •••••••••••••16 D.S. Colburn and J.B. Pollack Condensation of frosts on martian dust particles •••••••••••••19 J.L. Gooding Toward an understanding of the martian dust cycle •••••••••••••22 R. Greeley Martian dust: The case for "parna" • • • • • • • • • • • • • • • • • • • 25 R. Greeley The development of global dust storms on Mars: The role of the mean meridional circulation • • • • • • • • • , • . • . • 28 R.M. Haberle Dust scattering at the martian terminator during the Mariner 9 mission . • • . • • 30 K. Herkenhoff Are the Viking Lander sites representative of the surface of Mars? ••••33 B. Jakosky and P. Christensen Interannual variability in Mars' South Polar recessions and possible correlations with major duststorms . • • • • • • •••••• 35 P.B. James and L.J. Martin The vertical distribution of aerosols during the growth phase of a global dust storm ••••••••••••••••••••••••37 F. Jaquin The varying properties of martian aerosols ••••••••••••••••38 R. -
Glaciers of México
Glaciers of North America— GLACIERS OF MÉXICO By SIDNEY E. WHITE SATELLITE IMAGE ATLAS OF GLACIERS OF THE WORLD Edited by RICHARD S. WILLIAMS, Jr., and JANE G. FERRIGNO U.S. GEOLOGICAL SURVEY PROFESSIONAL PAPER 1386–J–3 Glaciers in México are restricted to its three highest mountains, all stratovolcanoes. Of the two that have been active in historic time, Volcán Pico de Orizaba (Volcán Citlaltépetl) has nine named glaciers, and Popocatépetl has three named glaciers. The one dormant stratovolcano, Iztaccíhuatl, has 12 named glaciers. The total area of the 24 glaciers is 11.44 square kilometers. The glaciers on all three volcanoes have been receding during the 20th century. Since 1993, intermittent explosive and effusive volcanic activity at the summit of Popocatépetl has covered its glaciers with tephra and caused some melting CONTENTS Page Abstract ---------------------------------------------------------------------------- J383 Introduction----------------------------------------------------------------------- 383 Volcán Pico de Orizaba (Volcán Citlaltépetl) ----------------------------- 384 FIGURE 1. Topographic map showing the glaciers on Citlaltépetl--------- 385 2. Sketch map showing the principal overland routes to Citlaltépetl, Iztaccíhuatl, and Popocatépetl ------------------ 386 3. Oblique aerial photograph of Citlaltépetl from the northwest in February 1942 --------------------------------------------- 387 4. Enlargement of part of a Landsat 1 MSS false-color composite image of Citlaltépetl and environs --------------------------- -
Los Andes Y El Reto Del Espacio Mundo : Homenaje a Olivier Dollfus
Sobre la obra Olivi.., Do II ILl~ [1~ 111, getlgrail l i,.mu'~~. 1md" ~lll l'mel ílll !Iv \,' Uníw'r"id.JeI c1 n r.ll i~ , h;\ I '(I'l lu;,c1o y dirigido i n"t',' li~¡¡rio m.:" sohn I.I ~ rn.'yolt!s ..'; Il I l' Il .l~ lit;' nl1lnt.lñ.l!> d... l muml» I /\ nc J¡~c; . l limalava , I\ II" .: !> I. ~lIhw , 1I~ 1 ·.1n1p t,' ~inllcl l) !> v ~ Il " '(' 1.1 insc r: jl'm dC' sus ('C 1)llorll i.l ~ V ele ~ 1I, "l c ¡eel.leI . ~ (' 11 1111 IlIlIIHln ¡.;lob.llil.Jl Jo, LI l.o:;r>.l('Í, I .,ndino trnpira l y en p. llti( 111.11 '-'1 p(4ní, Sil" ' ';l lllr ' l~ rlff'díl"d llS d.-· ','.;luell" d l~ ll' l'I ,1(ln IqSl . 11.111 d.ldll lug.1f .1 n UI1lCfI,"'-IS puhlicat'inn,·...,Su I'''''l'ñ.lnz., Un iVI'ISil<lriil . SlIS e" lu c! i"" y SlI l,tI,or i n~ l i lucíl l/ I .! I h..n m .III;'luO prlliuncl.lnlt':llll' (1 v.m.« )!,l :n e ' ,l d rll) ( ~" clt-. invc'';líg,ll!<lIl:<O. DI.' 1~ltí7 ,1 Itl7:! [ue ,lilel Io,r del lnsritu«1rr.lf W¡;" (le Esludi,.sArulinus yJ ltiriLe¡Jp 5111!' Pd IISicill durante '.',Isi meclj, I sigll'. E!- rc,' lihru. hllllll:n.ljl' el 1.1 ríqll\.'?J y el 1.. ieü !mliddd d,.' ~u t rayt'\ tnri a intdl'l lutll '! pr'J\L'sílln .ll , riene por IIhjl'livLJ d itu nrlir a rn plia mrnt« I'J ~ C() I \f(' rl o~ . -
Low-Albedo Surfaces and Eolian Sediment: Mars Orbiter Camera Views of Western Arabia Terra Craters and Wind Streaks
Low-albedo surfaces and eolian sediment: Mars Orbiter Camera views of western Arabia Terra craters and wind streaks Kenneth S. Edgett Malin Space Science Systems, Inc., San Diego, California, USA Abstract. High spatial resolution (1.5 to 6 m/pixel) Mars Global Surveyor Mars Orbiter Camera images obtained September 1997 to June 2001 show that each of the large, dark wind streaks of western Arabia Terra originate at a barchan dune field on a crater floor. The streaks consist of a relatively thin (< 1 m) coating of sediment deflated from the dune fields and their vicinity. In most cases, this sediment drapes over a previous mantle that more thickly covers nearly all of western Arabia Terra. No concurrent eolian bedforms are found within the dark streaks, nor do any dunes climb up crater walls to deliver sand via saltation to the streaks. The relations between dunes, wind streak, and subjacent terrain imply that dark-toned grains finer than those that comprise the dunes are lifted into suspension and carried out of the craters to be deposited on the adjacent terrain. Previous eolian physics and thermal inertia studies suggest that, under modern Martian conditions, such grains likely include silt (3.9–62.5 !m), very fine sand (62.5–125 !m), and possibly fine sand (to ~210 !m). The streaks change in terms of extent, relative albedo, and surface pattern over periods measured in years; however, through June 2001, very little evidence for recent eolian activity (dust plumes, storms, dune movement) was observed. received 18 July 2001, revised 21 December 2001, accepted 2 January 2002, published 13 June 2002 Citation: Edgett, K. -
PROJECT on MARS: EVQLUTION of ITS CLIMATE and Athaosphere
. SCIENTIFIC RESULTS OF THE NASA23PONSORED STUDY PROJECT ON MARS: EVQLUTION OF ITS CLIMATE AND AThaOSPHERE MECA (NASA-@$- K~/~&?SCIENTXPICEESULTS OF THE 18 9- 1 50 5 9 NBSA-SPCISORED SSEDY PBOJEC'L C6 EARS: EVCLUTICN OF IT2 CLIRAIE AHC A'ItCSPHERE (hASA) 36 F CSCL 03B Unclas G3/91 0170241 LPI Technical Report Number WHO9 LUNAR AND PLANETARY INSTITUTE 3303 NASA ROAD 1 HOUSTON, TEXAS 77058 I SCIENTIFIC RESULTS OF THE NASA-SPONSORED STUDY PROJECT ON MARS: EVOLUTION OF ITS CLIMATE AND ATMOSPHERE Stephen M. Clifford Lunar and Planetary Institute 3303 NASA Road 1 Houston, TX 77058 Ronald Greeley Department of Geology Arizona State University Tempe, AZ 85287 Robert M. Haberle Mail Code 245-3 NASA Ames Research Center Moffet Field, CA 94035 I Lunar and Planetary Inst it ut e 3303 NASA Road One Houston, Texas 77058-4399 I LPI Technical Report Number 88-09 Compiled in 1988 by the LUNAR AND PLANETARY INSTITUTE The Institute is operated by Universities Space Research Association under Contract NASW-4066 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: Clifford S. M., Greeley R., and Haberle R. M. (1988) Scientifi Results of the NASA-Sponsored Study Project on Mars: Evolution of its Climate and Atmosphere. LPI Tech. Rpt. 88-09. Lunar and Planetary Institute, Houston. 33 pp. Papers in this report may be cited as: Author A. -
Percival Lowell: the Sage As Astronomer David Sutton Dolan University of Wollongong
University of Wollongong Research Online University of Wollongong Thesis Collection University of Wollongong Thesis Collections 1992 Percival Lowell: the sage as astronomer David Sutton Dolan University of Wollongong Recommended Citation Dolan, David Sutton, Percival Lowell: the sage as astronomer, Doctor of Philosophy thesis, Department of Science and Technology Studies, University of Wollongong, 1992. http://ro.uow.edu.au/theses/1712 Research Online is the open access institutional repository for the University of Wollongong. For further information contact the UOW Library: [email protected] PERCIVAL LOWELL: THE SAGE AS ASTRONOMER by David Sutton Dolan, B.A. Hons. (Flinders), M. A. (Adelaide) Department of Science and Techology Studies University of Wollongong January 1992 PERCIVAL LOWELL: THE SAGE AS ASTRONOMER CONTENTS CHAPTER PAGE 1. PERCIVAL LOWELL (1855-1916) IN HIS TIMES 1 1.1 Lowell's life and work 1 1.2 An overview of Lowell's astronomical writings 17 1.3 A brief survey of the biographical literature on Lowell 31 2. LOWELL IN THE LITERATURE, BEFORE THE SPACE AGE 45 2.1 C1830-1924 50 2.2 1925-49 78 2.3 1949-57 101 3. LOWELL IN THE SPACE AGE 125 3.1 Sputnik to Mariner: 1958-1965 125 3.2 Mariner to Viking and after: 1965-1990 155 4. LOWELL AND THE LITERARY PERSONA OF THE SAGE 186 4.1 Lowell as an anomaly in the pluralist tradition 188 4.2 "The eye of the man of knowledge" 204 4.3 Thomas Carlyle: Victorian prose, the universe, science and history 228 4.4 John Ruskin: the morality of landscape and climate 240 5. -
Xve Assemblee Generale
XVth General Assembly Sydney, Australia 1973 XVe Assemblee Generale Sydney, Australie 1973 Resolution No. 1 The General Assembly of the International Astronomical Union resolves to adopt the following change of the Statutes: At the end of Articles 11 (a) et 11 (b), the following sentence is added: 'Exceptions from this rule cannot be considered unless decided by the Executive Committee.' L'Assemblee Generale de l'Union Astronomique Internationale decide d'adopter la modification suivante des Statuts: A la fin des articles 11 (a) et 11 (b), la phrase suivante est ajoutee: 'Des excep tions it cette regIe ne peuvent etre envisagees que sur decision du Comite Executif.' Resolution No. 2 The General Assembly of the International Astronomical Union requests th~ Executive Commit tee to examine the possibility of a change in the Statutes such as to allow the three years interval between two General Assemblies to be extended to a four-year interval, if such is, after study, the opinion of the Executive Committee. L'Assemblee Generale de l'Union Astronomique Internationale demande au Comite Executif d'examiner la possibilite de modifier les Statuts, de telle sorte que l'intervalle de trois ans entre deux Assemblees Generales puisse etre etendu it quatre ans, si telle est, apres examen, l'opinion du Comite Execufif. Resolution No. 3 The General Assembly of the International Astronomical Union recognizes the scientific interest of regional meetings and recommends to their organizers to take the appropriate steps so that the dates of these meetings and their programme be such as not to constitute for the member countries an excessive financial burden. -
Duststones on Mars: Source, Transport, Deposition, and Erosion
DUSTSTONES ON MARS: SOURCE, TRANSPORT, DEPOSITION, AND EROSION NATHAN T. BRIDGES Applied Physics Laboratory, MP3-E171, 11101 Johns Hopkins Road, Laurel, Maryland 20723 USA e-mail: [email protected] AND DANIEL R. MUHS US Geological Survey, MS 980, Box 25046, Federal Center, Denver, Colorado 80225 USA ABSTRACT: Dust is an abundant material on Mars, and there is strong evidence that it is a contributor to the rock record as ‘‘duststone,’’ analogous in many ways to loess on Earth. Although a common suite of dust formation mechanisms has operated on the two planets, fundamental differences in environments and geologic histories have resulted in vastly different weighting functions, causing distinct depositional styles and erosional mechanisms. On Earth, dust is derived predominantly from glacial grinding and, in nonglacial environments, by other processes, such as volcanism, eolian abrasion, and fluvial comminution. Hydrological and biological processes convert dust accumulations to loess deposits. Active hydrology also acts to clean dust from the atmosphere and convert loess into soil or erode it entirely. On Mars, glacial production of dust has been minor, with most fine particles probably produced from ancient volcanic, impact, and fluvial processes. Dust is deposited under arid conditions in which aggregate growth and cementation are the stabilizing agents. Thick accumulations result in duststone. KEY WORDS: dust, loess, Mars, eolian processes, analogs INTRODUCTION ripples, features formed by saltation and creep processes, contain particles less than 100 lm in diameter, which theory predicts should be The geologic record of a planetary body is reflective of its dominant suspended (Sullivan et al. 2008). This discrepancy between theory and rock-forming processes, preservation mechanisms, and degrees of observation may exist because of the lower atmospheric density on erosion and exposure.