DOCSLIB.ORG

Selenology Today D E V R E S E R

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text

Load more

GLR GROUP 2007 ALL RIGTHS RESERVED SELENOLOGY TODAY #11 October 2008 SELENOLOGY SELENOLOGY TODAY TODAY Selenology Today is devoted to the publi- cation of contributions in the field of lunar studies. Manuscripts reporting the results of new re- search concerning the astronomy, geology, physics, chemistry and other scientific as- pects of Earth’s Moon are welcome. Editor-in-Chief: Selenology Today publishes papers de- voted exclusively to the Moon. R. Lena Reviews, historical papers and manu- scripts describing observing or spacecraft Editors: instrumentation are considered. M.T. Bregante J. Phillips The Selenology Today C. Wöhler Editorial Office C. Wood [email protected] Cover Raffaele Barzacchi May 14 2008 21:21 UT Selenology Today # 11 October 2008 SELENOLOGY TODAY #11 October 2008 Selenology Today website http://digilander.libero.it/glrgroup/ A study about two domes near craters C. Herschel and Archytas, and an effusive dome in Mare Frigoris By R. Lena, J. Phillips, M. T. Bregante, S. Lammel and G. Tarsoudis ………………..………........................................ 1 Spectral studies of banded craters using Clementine 5 band UVVIS data By R. Evans ………......................................................................................26 Detection of satellites and space debris in transit across the moon By R. Lena ..……….......................................................................................78 Partial lunar eclipse August 16-17 2008 by P. Dominguez, G. Tarsoudis, R. Lena and C. Cellini -F. Mazzotti ……………..................................................83 Upcoming LCROSS impact at lunar south pole by R. Evans ..............89..............89 Selenology Today # 11 October 2008 LUNAR DOMES SELENOLOGY TODAY # 11 A Study about two domes near craters C. Herschel and Archytas, and an effusive dome in Mare and duration of the effusion process of 3.4 years. Furthermore, we have Frigoris derived a magma rise speed of 4.4 x 10-6 m s-1 through a dike 170 km long and 114 m wide. In this study we have By Raffaello Lena, Jim Phillips, Maria examined another dome located near Teresa Bregante, Stefan Lammel and the crater C. Herschel (CH1), which George Tarsoudis has a diameter of 16.8 ± 0.4 km, height of 64 ± 10 m , resulting in Geologic Lunar Research (GLR) group flank slope of 0.44°. The dome CH1 has a rille which cannot be unambi- guously attributed to formation by Abstract tensional stress or flowing of lava. If In this study we examine three lunar it was assumed to be of intrusive ori- gin, the dome C. Herschel 1 could be domes located near the crater C. Herschel and Archytas, in Mare assigned to class In2. Regarding it as Frigoris. The diameters of the domes an effusive dome would imply to as- Archytas 1 and 2 are determined to 33.0 sign it to the effusive class C1. ± 1 km and 11.0 ± 0.4 km. Their heights amount to 70 ±120 m and 265 ± 30 m, resulting in flank slopes of 0.25° and 2.7°. The edifice volumes correspond to 22.4 and 12.6 km³. The dome Archytas 1 1.Introduction belongs to class In3 in the GLR classifi- The Mare Basins were formed by large cation scheme of intrusive domes while impacts. These impacts formed large Archytas 2 belongs to class B1 of the cavities which collapsed. These GLR classification scheme of effusive collapses led to large-scale fracturing in domes. Archytas 1 is a large dome inter- the crust. The fractures are thought to be preted to be an intrusive structure due the conduits along which the basaltic to the presence of a short straight rille magmas ascended to the surface. Lunar and a fault traversing the surface, sug- domes have formed as effusive shield- gesting that its uplift resulted from the like volcanoes or as laccoliths, if the rise of magma that did not erupt onto the magma remained subsurface (Head and surface, producing a vertical rupture of Gifford, 1980). The summit pit is an the surface. It is the first lunar dome indication of the volcanic origin of these having a concentric crater on the sum- structures but it is not always present. mit. Domes without a summit pit could still Based on rheologic modelling we obtai- be volcanic in origin, but appear to have ned for Archytas 2 dome effusion rate of covered their central vent with lava 3 -1 6 (plug domes). Another possibility is that 119 m s , magma viscosity of 4.4 x 10 page 1 LUNAR DOMES SELENOLOGY TODAY # 11 Fig. 1 page 2 LUNAR DOMES SELENOLOGY TODAY # 11 Fig. 2a page 3 LUNAR DOMES SELENOLOGY TODAY # 11 Fig. 2b page 4 LUNAR DOMES SELENOLOGY TODAY # 11 these domes represent intrusion of the UCLN 1994 list of control points. lava: the magma accumulated within All images are oriented with north up the lunar crust, slowly increasing in and west (IAU) to the left. pressure and causing the crustal rock above it to bow up-ward. The profile Further morphometric data were of domes that are flat suggests that obtained by a photoclinometric there was no gradual inclination at analysis (Horn, 1989; Carlotto, 1996; the vent (the rising lava did not build cf. also Wöhler et al., 2006; Lena et al., up the dome in a series of flows) but 2006 and references therein). We a subsurface intrusion of magma furthermore determined a UVVIS five- (intrusive origin). Due to their low band spectrum of the dome based on profile, Lunar Orbiter and Clementine Clementine imagery at the wavelengths of 415, 750, 900, 950, and 1000 nm. images do not tend to show them very 2 well, due to the typically high solar The sample area was 2x2 km . The angle on such images. Hence, as part reflectance values were derived relying of our program of observations and on the calibrated and normalised cataloguing of lunar domes, we have Clementine UVVIS reflectance data as used high resolution telescopic CCD provided by Eliason et al. (1999). The images carried out under oblique extracted Clementine UVVIS data illumination conditions. In this article were examined in terms of 750 nm we report measurement and include reflectance (albedo) and the R415/R750 CCD images of two previously and R950/R750 colour ratios. Albedo at unlisted lunar domes, located at 750 nm is an indicator of variations in latitude 34.76°N and longitude soil composition, maturity, particle 32.57°W (near crater C. Herschel) size, and viewing geometry. and latitude 56.52° N and 2.71° W The R /R colour ratio essentially is (in Mare Frigoris). Moreover we 415 750 a measure for the TiO2 content of examine another lunar dome in Mare mature basaltic soils, where high R / Frigoris, possibly of intrusive origin, 415 R ratios correspond to high TiO situated at 55.71°N and longitude 750 2 content and vice versa (Charette et al., 0.71°E. 1974). However, for many lunar 2. Method and measurement regions the relation between R415/R750 ratio and TiO2 content displays a For each of the observations, the local significant scatter (Gillis and Lucey, solar altitude and the Sun's 2005). The R950/R750 colour ratio is selenographic colongitude were related to the strength of the mafic calculated using the LTVT software absorption band, representing a package by Mosher and Bondo measure for the FeO content of the (2006) which requires a calibration of soil, and is also sensitive to the optical the images by identifying the precise maturity of mare and highland selenographic coordinates of some materials (Lucey et al. 1998). landmarks on the image. This calibration was performed based on page 5 LUNAR DOMES SELENOLOGY TODAY # 11 3. Region around C. Herschel. basin suggesting that KREEP is General description abundant in the region, although its specific distribution appears to be not Mare Imbrium sits in the Imbrium basin. directly related to the distribution of The basin material is of the Lower Imbrium basin deposits. Moreover the Imbrian epoch, with the mare material distribution of KREEP, tracked by Th being of the Upper Imbrian and content, is not directly correlated with Eratosthenian epochs (Wilhelms,1987). Imbrium basin ejecta, but has had a The mare is lined with mountain ranges complex, multiphase history involving to the south. The Alpes are part of the both impact and volcanic process 1200 km diameter basin defining ring of (Spudis, 1993). Different lithological Imbrium as also the Montes Carpatus in units, included in USGS lunar geologic the south, the Apennines in the map I-602, are apparent in the western southeast, and the Montes Caucasus to part of Mare Imbrium, characterized by the east. The Montes Caucasus and long wrinkle ridges and basalts of Alpes consist of rugged massifs that Imbrian age, mapped as 3 distinct units, make up the rim crest of the Imbrium Im1 through Im3, and described as flat, basin. The knobby Alpes formation, a smooth material of mare areas (Schaber, unit with wide distribution around the 1969). We have studied a dome, located Imbrium basin (Spudis, 1988; Spudis, in the western part of Mare Imbrium, 1993; Wilhelms,1987; Whitford-Stark, near a small lunar crater named 1990) is found along the backslope of C.Herschel, a circular bowl shaped the basin rim crest in the north and east formation. The crater lies on a wrinkle- of the basin. ridge of the lunar mare named Dorsum In the western segment of the basin Heim. No lunar domes located near exterior, hummocky to radially lineated Dorsum Heim and crater C. Herschel Fra Mauro material makes up the are reported in the USGS I-602, in backslope deposits (Spudis, 1988). ALPO catalogue and in the revised list of lunar domes (Kapral and Garfinkle, Basalts of Mare Frigoris cover Imbrium 2005). In the revised list is reported a basin deposits north of the basin rim at radial distances of 300-700 km from the dome of 3 km in diameter located at rim crest.
Recommended publications
  • Report Resumes

    Report Resumes

    REPORT RESUMES ED 019 218 88 SE 004 494 A RESOURCE BOOK OF AEROSPACE ACTIVITIES, K-6. LINCOLN PUBLIC SCHOOLS, NEBR. PUB DATE 67 EDRS PRICEMF.41.00 HC-S10.48 260P. DESCRIPTORS- *ELEMENTARY SCHOOL SCIENCE, *PHYSICAL SCIENCES, *TEACHING GUIDES, *SECONDARY SCHOOL SCIENCE, *SCIENCE ACTIVITIES, ASTRONOMY, BIOGRAPHIES, BIBLIOGRAPHIES, FILMS, FILMSTRIPS, FIELD TRIPS, SCIENCE HISTORY, VOCABULARY, THIS RESOURCE BOOK OF ACTIVITIES WAS WRITTEN FOR TEACHERS OF GRADES K-6, TO HELP THEM INTEGRATE AEROSPACE SCIENCE WITH THE REGULAR LEARNING EXPERIENCES OF THE CLASSROOM. SUGGESTIONS ARE MADE FOR INTRODUCING AEROSPACE CONCEPTS INTO THE VARIOUS SUBJECT FIELDS SUCH AS LANGUAGE ARTS, MATHEMATICS, PHYSICAL EDUCATION, SOCIAL STUDIES, AND OTHERS. SUBJECT CATEGORIES ARE (1) DEVELOPMENT OF FLIGHT, (2) PIONEERS OF THE AIR (BIOGRAPHY),(3) ARTIFICIAL SATELLITES AND SPACE PROBES,(4) MANNED SPACE FLIGHT,(5) THE VASTNESS OF SPACE, AND (6) FUTURE SPACE VENTURES. SUGGESTIONS ARE MADE THROUGHOUT FOR USING THE MATERIAL AND THEMES FOR DEVELOPING INTEREST IN THE REGULAR LEARNING EXPERIENCES BY INVOLVING STUDENTS IN AEROSPACE ACTIVITIES. INCLUDED ARE LISTS OF SOURCES OF INFORMATION SUCH AS (1) BOOKS,(2) PAMPHLETS, (3) FILMS,(4) FILMSTRIPS,(5) MAGAZINE ARTICLES,(6) CHARTS, AND (7) MODELS. GRADE LEVEL APPROPRIATENESS OF THESE MATERIALSIS INDICATED. (DH) 4:14.1,-) 1783 1490 ,r- 6e tt*.___.Vhf 1842 1869 LINCOLN PUBLICSCHOOLS A RESOURCEBOOK OF AEROSPACEACTIVITIES U.S. DEPARTMENT OF HEALTH, EDUCATION & WELFARE OFFICE OF EDUCATION K-6) THIS DOCUMENT HAS BEEN REPRODUCED EXACTLY AS RECEIVED FROM THE PERSON OR ORGANIZATION ORIGINATING IT.POINTS OF VIEW OR OPINIONS STATED DO NOT NECESSARILY REPRESENT OFFICIAL OFFICE OF EDUCATION POSITION OR POLICY. 1919 O O Vj A PROJECT FUNDED UNDER TITLE HIELEMENTARY AND SECONDARY EDUCATION ACT A RESOURCE BOOK OF AEROSPACE ACTIVITIES (K-6) The work presentedor reported herein was performed pursuant to a Grant from the U.
  • Geologic Structure of Shallow Maria

    Geologic Structure of Shallow Maria

    NASA CR. Photo Data Analysis S-221 NASA Contract NAS 9-13196 GEOLOGIC STRUCTURE OF SHALLOW MARIA Rene' A. De Hon, Principal Investigator John A. Waskom, Co-Investigator (NASA-CR-lq7qoo GEOLOGIC STahJCTUnF OF N76-17001 ISBALOW M1BIA-'(Arkansas Uni.v., mHiticelio.) ­ 96 p BC $5.00' CSCL O3B Unclas G3/91, 09970- University of Arkansas at Monticello Monticello, Arkansas December 1975 Photo Data Analysis S-221 NASA Contract NAS 9-13196 GEOLOGIC STRUCTURE OF SHALLOW MARIA Rene' A. De Hon, Principal Investigator I John A. Waskom, Co-Investigator Un-iversity-of Arkansas-:at-.Monticl o Monticello, Arkansas December 1975 ABSTRACT Isopach maps and structural contour maps of the 0 0 eastern mare basins (30 N to 30 OS; 00 to 100 E) are constructed from measurements of partially buried craters. The data, which are sufficiently scattered to yield gross thickness variations, are restricted to shallow maria with less than 1500-2000 m of mare basalts. The average thickness of b-asalt in the irregular maria is between 200 and 400 m. Multiringed mascon basins are filled to various levels. The Serenitatis and Crisium basins have deeply flooded interiors and extensively flooded shelves. Mare basalts in the Nectaris basin fill only the innermost basin, and mare basalts in the Smythii basin occupy a small portion of the basin floor. Sinus Amoris, Mare Spumans, and Mare Undarum are partially filled troughs concentric to large circular basins. The Tranquillitatis and Fecunditatis are composite depressions containing basalts which flood degraded circular basins and adjacent terrain modified by the formation of nearby cir­ cular basins.
  • EPSC-DPS2011-1845, 2011 EPSC-DPS Joint Meeting 2011 C Author(S) 2011

    EPSC-DPS2011-1845, 2011 EPSC-DPS Joint Meeting 2011 C Author(S) 2011

    EPSC Abstracts Vol. 6, EPSC-DPS2011-1845, 2011 EPSC-DPS Joint Meeting 2011 c Author(s) 2011 Analysis of mineralogy of an effusive volcanic lunar dome in Marius Hills, Oceanus Procellarum. A.S. Arya, Guneshwar Thangjam, R.P. Rajasekhar, Ajai Space Applications Centre, Indian Space Research Organization, Ahmedabad-380 015 (India). Email:[email protected] Abstract found on the lunar surface. As a part of initiation of the study of mineralogy of MHC, an effusive dome Domes are analogous to the terrestrial shield located in the south of Rima Galilaei, near the volcanoes and are among the important volcanic contact of Imbrian and Eratosthenian geological units features found on the lunar surface indicative of is taken up for the present study. The morphology, effusive vents of primary volcanism within Mare rheology and the possible dike parameters have regions. Marius Hills Complex (MHC) is one of the already been studied and reported [5]. most important regions on the entire lunar surface, having a complex geological setting and largest distribution of volcanic constructs with an abundant number of volcanic features like domes, cones and rilles. The mineralogical study of an effusive dome located in the south of Rima Galilaei, near the contact of Imbrian and Eratosthenian geological units is done using hyperspectral band parameters and spectral plots so as to understand the compositional variation, the nature of the volcanism and relate it to the rheology of the dome. Fig. 1: Distribution of dome in MHC (Red-the dome under study, Green- from Virtual Moon Atlas, Magenta [6]) and the Study area showing the dome under study on M3 1.
  • OMNI Magazine Interview, July 1992)

    OMNI Magazine Interview, July 1992)

    ALIEN CITY ON MARS? TiTil W i^ -A Im; SCENES Lji U *' Ul EDITOR IN CHIEF & DESIGN DIRECTOR: BOB GUCCIONE PRESIDENT a C.O.O.: KATHY KEETON VP/EDITOR' KEITH FERRELL EXECUTIVE VP/GBAPHICS DIRECTOR- FRANK DEVINO MANAGING EDITOR: CAROLINE DARK ART DIRECTOR: CATHRYN MEZZO First Word Continuum By Dana Rohrabacher 42 Fighting for Opening the X-Files U.S. patent rights By David Bischoff S Mulder and Scully know Communications something is m out there—and so do their Funds many fans. A behind- By Linda Marsa the-scenes lool< at this fas- Cashing in on collectibles cinating and m increasingly popular Electronic Universe new show. By Grsgg Keizer ArchiTreIc Medicine Designing Generations By Anita Bartholomew By Herman Zimmerman m and Philip Thomas Edgerly .Sounds Boldly going where By Steve Nadis few. production designers Sounds of the silent have gone before: 22 designing the Star Trek Eanii By Melanie Menagh Choices Fiction: S.4 Dying Virtual Realities [Vlichael IVlarshall Smith By Tom Dworetzl<y 7^ 23 Cartoon Feature Artificial Intelligence . By Steve Nadis Interview: 32 Richard hioa gland Mind By Steve Nadis By Steve Nadis A close-up lool< at the Hallucinations, man behind delusions, the face on Mars and schizophrenia SS 33 Tsuneo Sanda's cover painting, On Patrol, made possible by Antimatter the PI" I p Edge ly Age cy n a'^sar qt on witi ZD^sgn Copyrght Pa amount PcturesCorporaticn Games (Additional art rred t"^ page 110) By bi, iff Morris SR1''6ril7'iBn FIRST UUORD INVENTING AMERICA: Patent laws and the protection of individual rights By Dana Rohrabacher merica's greatest asset side.
  • Glossary Glossary

    Glossary Glossary

    Glossary Glossary Albedo A measure of an object’s reflectivity. A pure white reflecting surface has an albedo of 1.0 (100%). A pitch-black, nonreflecting surface has an albedo of 0.0. The Moon is a fairly dark object with a combined albedo of 0.07 (reflecting 7% of the sunlight that falls upon it). The albedo range of the lunar maria is between 0.05 and 0.08. The brighter highlands have an albedo range from 0.09 to 0.15. Anorthosite Rocks rich in the mineral feldspar, making up much of the Moon’s bright highland regions. Aperture The diameter of a telescope’s objective lens or primary mirror. Apogee The point in the Moon’s orbit where it is furthest from the Earth. At apogee, the Moon can reach a maximum distance of 406,700 km from the Earth. Apollo The manned lunar program of the United States. Between July 1969 and December 1972, six Apollo missions landed on the Moon, allowing a total of 12 astronauts to explore its surface. Asteroid A minor planet. A large solid body of rock in orbit around the Sun. Banded crater A crater that displays dusky linear tracts on its inner walls and/or floor. 250 Basalt A dark, fine-grained volcanic rock, low in silicon, with a low viscosity. Basaltic material fills many of the Moon’s major basins, especially on the near side. Glossary Basin A very large circular impact structure (usually comprising multiple concentric rings) that usually displays some degree of flooding with lava. The largest and most conspicuous lava- flooded basins on the Moon are found on the near side, and most are filled to their outer edges with mare basalts.
  • Planetary Surfaces

    Planetary Surfaces

    Chapter 4 PLANETARY SURFACES 4.1 The Absence of Bedrock A striking and obvious observation is that at full Moon, the lunar surface is bright from limb to limb, with only limited darkening toward the edges. Since this effect is not consistent with the intensity of light reflected from a smooth sphere, pre-Apollo observers concluded that the upper surface was porous on a centimeter scale and had the properties of dust. The thickness of the dust layer was a critical question for landing on the surface. The general view was that a layer a few meters thick of rubble and dust from the meteorite bombardment covered the surface. Alternative views called for kilometer thicknesses of fine dust, filling the maria. The unmanned missions, notably Surveyor, resolved questions about the nature and bearing strength of the surface. However, a somewhat surprising feature of the lunar surface was the completeness of the mantle or blanket of debris. Bedrock exposures are extremely rare, the occurrence in the wall of Hadley Rille (Fig. 6.6) being the only one which was observed closely during the Apollo missions. Fragments of rock excavated during meteorite impact are, of course, common, and provided both samples and evidence of co,mpetent rock layers at shallow levels in the mare basins. Freshly exposed surface material (e.g., bright rays from craters such as Tycho) darken with time due mainly to the production of glass during micro- meteorite impacts. Since some magnetic anomalies correlate with unusually bright regions, the solar wind bombardment (which is strongly deflected by the magnetic anomalies) may also be responsible for darkening the surface [I].
  • By DWG Arthur, Alice P. Agnieray, Ruth H. Pellicori, CA Wood, and T

    By DWG Arthur, Alice P. Agnieray, Ruth H. Pellicori, CA Wood, and T

    No. 50 THE SYSTEM OF LUNAR CRATERS, QUADRANT III by D. W. G. Arthur, Alice P. Agnieray, Ruth H. Pellicori, C. A. Wood, and T. Weller February 25, 1965 ABSTRACT The designation, diameter, position, central peak information, and state of completeness are listed for each discernible crater with a diameter exceeding 3.5 km in the third lunar quadrant. The catalog contains about 5200 items and is illustrated by a map in 11 sections. on the averted lunar hemisphere, and therefore, these Thistem Communication of Lunar Craters, is the which third is part a catalog of The in Sys four are not listed in the catalog. parts of all craters recognizable with reasonable The approximate positions and diameters for certainty on photographs and having a diameter these craters are: greater than 3.5 km. It is thus a continuation of the work in Comm. LPL Nos. 30 and 40, and the same Long. Lat. Diam, (.00Ir) Hausen -91?5 - 6 5 ? 6 9 9 . 5 conventions and format are used. Boltzmann -96?0 - 7 5 ? 5 3 9 . 1 As in the earlier parts, it was found necessary S t e f a n - 9 4 ? 0 - 7 2 ? 0 7 8 . 0 to add names for large craters in the extreme limb regions. The new crater names for Quadrant III are: The above are mere additions to the Blagg and Miiller scheme. A more notable innovation, which Baade German-American astronomer has already been authorized by the International Boltzmann Austrian physicist Astronomical Union at its 1964 general meeting at Drygalski German geographer Hamburg, is the addition of the name Mare Cogni- Hartwig German selenodetist tum (the known sea) for the dark area between Krasnov Russian selenodetic observer Riphaeus and the crater Guerike.
  • DMAAC – February 1973

    DMAAC – February 1973

    LUNAR TOPOGRAPHIC ORTHOPHOTOMAP (LTO) AND LUNAR ORTHOPHOTMAP (LO) SERIES (Published by DMATC) Lunar Topographic Orthophotmaps and Lunar Orthophotomaps Scale: 1:250,000 Projection: Transverse Mercator Sheet Size: 25.5”x 26.5” The Lunar Topographic Orthophotmaps and Lunar Orthophotomaps Series are the first comprehensive and continuous mapping to be accomplished from Apollo Mission 15-17 mapping photographs. This series is also the first major effort to apply recent advances in orthophotography to lunar mapping. Presently developed maps of this series were designed to support initial lunar scientific investigations primarily employing results of Apollo Mission 15-17 data. Individual maps of this series cover 4 degrees of lunar latitude and 5 degrees of lunar longitude consisting of 1/16 of the area of a 1:1,000,000 scale Lunar Astronautical Chart (LAC) (Section 4.2.1). Their apha-numeric identification (example – LTO38B1) consists of the designator LTO for topographic orthophoto editions or LO for orthophoto editions followed by the LAC number in which they fall, followed by an A, B, C or D designator defining the pertinent LAC quadrant and a 1, 2, 3, or 4 designator defining the specific sub-quadrant actually covered. The following designation (250) identifies the sheets as being at 1:250,000 scale. The LTO editions display 100-meter contours, 50-meter supplemental contours and spot elevations in a red overprint to the base, which is lithographed in black and white. LO editions are identical except that all relief information is omitted and selenographic graticule is restricted to border ticks, presenting an umencumbered view of lunar features imaged by the photographic base.
  • October 2006

    October 2006

    OCTOBER 2 0 0 6 �������������� http://www.universetoday.com �������������� TAMMY PLOTNER WITH JEFF BARBOUR 283 SUNDAY, OCTOBER 1 In 1897, the world’s largest refractor (40”) debuted at the University of Chica- go’s Yerkes Observatory. Also today in 1958, NASA was established by an act of Congress. More? In 1962, the 300-foot radio telescope of the National Ra- dio Astronomy Observatory (NRAO) went live at Green Bank, West Virginia. It held place as the world’s second largest radio scope until it collapsed in 1988. Tonight let’s visit with an old lunar favorite. Easily seen in binoculars, the hexagonal walled plain of Albategnius ap- pears near the terminator about one-third the way north of the south limb. Look north of Albategnius for even larger and more ancient Hipparchus giving an almost “figure 8” view in binoculars. Between Hipparchus and Albategnius to the east are mid-sized craters Halley and Hind. Note the curious ALBATEGNIUS AND HIPPARCHUS ON THE relationship between impact crater Klein on Albategnius’ southwestern wall and TERMINATOR CREDIT: ROGER WARNER that of crater Horrocks on the northeastern wall of Hipparchus. Now let’s power up and “crater hop”... Just northwest of Hipparchus’ wall are the beginnings of the Sinus Medii area. Look for the deep imprint of Seeliger - named for a Dutch astronomer. Due north of Hipparchus is Rhaeticus, and here’s where things really get interesting. If the terminator has progressed far enough, you might spot tiny Blagg and Bruce to its west, the rough location of the Surveyor 4 and Surveyor 6 landing area.
  • August 2017 Posidonius P & Luther

    August 2017 Posidonius P & Luther

    A PUBLICATION OF THE LUNAR SECTION OF THE A.L.P.O. EDITED BY: Wayne Bailey [email protected] 17 Autumn Lane, Sewell, NJ 08080 RECENT BACK ISSUES: http://moon.scopesandscapes.com/tlo_back.html FEATURE OF THE MONTH – AUGUST 2017 POSIDONIUS P & LUTHER Sketch and text by Robert H. Hays, Jr. - Worth, Illinois, USA March 5, 2017 01:28-01:48; UT, 15 cm refl, 170x, seeing 7-8/10. I drew these craters on the evening of March 4/5, 2017 while the moon was hiding some Hyades stars. This area is in northeast Mare Serenitatis west of Posidonius itself. Posidonius P is the largest crater on this sketch. The smaller crater south of P is Posidonius F and Posidonius G is the tiny pit to the north. There is a halo around Posidonius G, but this crater is noticeably north of the halo's center. A very low round swelling is northeast of Posidonius G. Luther is the crater well to the west of Posidonius P. All four of these craters are crisp, symmetric features, differing only in size. There are an assortment of elevations near Luther. The peak Luther alpha is well to the west of Luther, and showed dark shadowing at this time. All of the other features near Luther are more subtle than Luther alpha. One mound is between Luther and Luther alpha. Two more mounds are north of Luther, and a low ridge is just east of this crater. A pair of very low mounds are south of Luther. These are the vaguest features depicted here, and may be too conspicuous on the sketch.
  • List of Targets for the Lunar II Observing Program (PDF File)

    List of Targets for the Lunar II Observing Program (PDF File)

    Task or Task Description or Target Name Wood's Rükl Target LUNAR # 100 Atlas Catalog (chart) Create a sketch/map of the visible lunar surface: 1 Observe a Full Moon and sketch a large-scale (prominent features) L-1 map depicting the nearside; disk of visible surface should be drawn 2 at L-1 3 least 5-inches in diameter. Sketch itself should be created only by L-1 observing the Moon, but maps or guidebooks may be used when labeling sketched features. Label all maria, prominent craters, and major rays by the crater name they originated from. (Counts as 3 observations (OBSV): #1, #2 & #3) Observe these targets; provide brief descriptions: 4 Alpetragius 55 5 Arago 35 6 Arago Alpha & Arago Beta L-32 35 7 Aristarchus Plateau L-18 18 8 Baco L-55 74 9 Bailly L-37 71 10 Beer, Beer Catena & Feuillée 21 11 Bullialdus, Bullialdus A & Bullialdus B 53 12 Cassini, Cassini A & Cassini B 12 13 Cauchy, Cauchy Omega & Cauchy Tau L-48 36 14 Censorinus 47 15 Crüger 50 16 Dorsae Lister & Smirnov (A.K.A. Serpentine Ridge) L-33 24 17 Grimaldi Basin outer and inner rings L-36 39, etc. 18 Hainzel, Hainzel A & Hainzel C 63 19 Hercules, Hercules G, Hercules E 14 20 Hesiodus A L-81 54, 64 21 Hortensius dome field L-65 30 22 Julius Caesar 34 23 Kies 53 24 Kies Pi L-60 53 25 Lacus Mortis 14 26 Linne 23 27 Lamont L-53 35 28 Mairan 9 29 Mare Australe L-56 76 30 Mare Cognitum 42, etc.
  • The Agatharchides Plateau (60 X 45Km) Is Classified As an Intrusive Lunar Mega Plateau, Similar to the Gardner Mega Plateau

    The Agatharchides Plateau (60 X 45Km) Is Classified As an Intrusive Lunar Mega Plateau, Similar to the Gardner Mega Plateau

    The Agatharchides Plateau (60 x 45km) is classified as an intrusive lunar Mega Plateau, similar to the Gardner Mega Plateau. The composition of the rocks is similar to the Gruithuisen domes and the mountain Mons Hansteen. On the eastern edge of the plateau is an extremely narrow - unnamed - rille. Unofficially this structure is named "The Helmet" because its shape is reminiscent of the helmets of the famous Star Wars movies. The Hortensius Domes are a classic small-scale lunar field of 7 lunar effusive shield volcanoes with diameters of 10 to 15 kilometers and small summit calderas. In this region between Kepler in the west and Copernicus in the east are around 2 dozen other domes, e.g. west of Milichius the great Dome Milichius Phi. Heinzel (68 x 19km) has, due to its shape, the nickname "Peanut crater". It is the result of a superposition of 3 impacts over a total length of nearly 70 km. Hesiodus A (14 km) is the largest and most easily observable double concentric crater on the front of the moon. Copernicus measures roughly 100 kilometers in diameter and is the prototype of a very young, complex crater. He has clearly terraced crater walls and the central mountains are divided into two parts. The crater floor is partially smooth and flat (covered with molten ejecta), on the opposite side there is a hilly region. The crater floor is 3.8 kilometers beneath the crater walls which rises less than 1 km above the surrounding landscape. The longest rays of the young ray system can be tracked up to a distance of 800 km.