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The History Group's Silver Jubilee
History of Meteorology and Physical Oceanography Special Interest Group Newsletter 1, 2010 ANNUAL REPORT CONTENTS We asked in the last two newsletters if you Annual Report ........................................... 1 thought the History Group should hold an Committee members ................................ 2 Annual General Meeting. There is nothing in Mrs Jean Ludlam ...................................... 2 the By-Law s or Standing Orders of the Royal Meteorological Society that requires the The 2010 Summer Meeting ..................... 3 Group to hold one, nor does Charity Law Report of meeting on 18 November .......... 4 require one. Which papers have been cited? .............. 10 Don’t try this at home! ............................. 10 Only one person responded, and that was in More Richard Gregory reminiscences ..... 11 passing during a telephone conversation about something else. He was in favour of Storm warnings for seafarers: Part 2 ....... 13 holding an AGM but only slightly so. He Swedish storm warnings ......................... 17 expressed the view that an AGM provides an Rikitea meteorological station ................. 19 opportunity to put forward ideas for the More on the D-Day forecast .................... 20 Group’s committee to consider. Recent publications ................................ 21 As there has been so little response, the Did you know? ........................................ 22 Group’s committee has decided that there will Date for your diary .................................. 23 not be an AGM this year. Historic picture ........................................ 23 2009 members of the Group ................... 24 CHAIRMAN’S REVIEW OF 2009 by Malcolm Walker year. Sadly, however, two people who have supported the Group for many years died during I begin as I did last year. Without an enthusiastic 2009. David Limbert passed away on 3 M a y, and conscientious committee, there would be no and Jean Ludlam died in October (see page 2). -
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]. -
Testing Hypotheses for the Origin of Steep Slope of Lunar Size-Frequency Distribution for Small Craters
CORE Metadata, citation and similar papers at core.ac.uk Provided by Springer - Publisher Connector Earth Planets Space, 55, 39–51, 2003 Testing hypotheses for the origin of steep slope of lunar size-frequency distribution for small craters Noriyuki Namiki1 and Chikatoshi Honda2 1Department of Earth and Planetary Sciences, Kyushu University, Hakozaki 6-10-1, Higashi-ku, Fukuoka 812-8581, Japan 2The Institute of Space and Astronautical Science, Yoshinodai 3-1-1, Sagamihara 229-8510, Japan (Received June 13, 2001; Revised June 24, 2002; Accepted January 6, 2003) The crater size-frequency distribution of lunar maria is characterized by the change in slope of the population between 0.3 and 4 km in crater diameter. The origin of the steep segment in the distribution is not well understood. Nonetheless, craters smaller than a few km in diameter are widely used to estimate the crater retention age for areas so small that the number of larger craters is statistically insufficient. Future missions to the moon, which will obtain high resolution images, will provide a new, large data set of small craters. Thus it is important to review current hypotheses for their distributions before future missions are launched. We examine previous and new arguments and data bearing on the admixture of endogenic and secondary craters, horizontal heterogeneity of the substratum, and the size-frequency distribution of the primary production function. The endogenic crater and heterogeneous substratum hypotheses are seen to have little evidence in their favor, and can be eliminated. The primary production hypothesis fails to explain a wide variation of the size-frequency distribution of Apollo panoramic photographs. -
Compositional and Mineralogical Characteristics of Archimedes Crater Region Using Chandrayaan – 1 M3 Data
50th Lunar and Planetary Science Conference 2019 (LPI Contrib. No. 2132) 1040.pdf COMPOSITIONAL AND MINERALOGICAL CHARACTERISTICS OF ARCHIMEDES CRATER REGION USING CHANDRAYAAN – 1 M3 DATA. P. R. Kumaresan1 and J. Saravanavel2, 1Research Scholar, 2Assistant Professor, Department of Remote Sensing, Bharathidasan University, Tiruchirappalli-23, Tamil Nadu, India, email: [email protected], [email protected] Introduction: The Earth’s natural satellite the tometry corrected reflectance data captured during the moon is nearest celestial body appears brightest object OP1B optical period. in our night sky. Moon surfaces are composed of dark and light areas. The dark areas are called Maria which is made up of basaltic terrain and light areas are high- lands mostly made up of Anorthositic rocks. The moon surface is littered with craters, which are formed when meteors hit its surface. To understand the evolution, geological process of the moon it is important to study the surface composition and minerals present in crustal surface. In this regard, in our study, we have attempted to map the minerals and surface composition of Archi- medes crater region. Study area: Archimedes crater is a large impact crater located on the eastern edges of the Mare Imbri- um of near side moon (29.7° N, 4.0° W). The diameter of the crater is 83 km with smooth floor flooded (1) with mare basalt and lack of a central peak. The rim (2) has a significant outer rampart brightened with ejecta (3) and the some portion of a terraced inner wall. Ar- chimedes Crater is named for the Greek mathematician Archimedes, who made many mathematical discoveries in the 200 B.C [1, 2]. -
The Moon After Apollo
ICARUS 25, 495-537 (1975) The Moon after Apollo PAROUK EL-BAZ National Air and Space Museum, Smithsonian Institution, Washington, D.G- 20560 Received September 17, 1974 The Apollo missions have gradually increased our knowledge of the Moon's chemistry, age, and mode of formation of its surface features and materials. Apollo 11 and 12 landings proved that mare materials are volcanic rocks that were derived from deep-seated basaltic melts about 3.7 and 3.2 billion years ago, respec- tively. Later missions provided additional information on lunar mare basalts as well as the older, anorthositic, highland rocks. Data on the chemical make-up of returned samples were extended to larger areas of the Moon by orbiting geo- chemical experiments. These have also mapped inhomogeneities in lunar surface chemistry, including radioactive anomalies on both the near and far sides. Lunar samples and photographs indicate that the moon is a well-preserved museum of ancient impact scars. The crust of the Moon, which was formed about 4.6 billion years ago, was subjected to intensive metamorphism by large impacts. Although bombardment continues to the present day, the rate and size of impact- ing bodies were much greater in the first 0.7 billion years of the Moon's history. The last of the large, circular, multiringed basins occurred about 3.9 billion years ago. These basins, many of which show positive gravity anomalies (mascons), were flooded by volcanic basalts during a period of at least 600 million years. In addition to filling the circular basins, more so on the near side than on the far side, the basalts also covered lowlands and circum-basin troughs. -
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 -
The Composition of the Lunar Crust: Radiative Transfer Modeling and Analysis of Lunar Visible and Near-Infrared Spectra
THE COMPOSITION OF THE LUNAR CRUST: RADIATIVE TRANSFER MODELING AND ANALYSIS OF LUNAR VISIBLE AND NEAR-INFRARED SPECTRA A DISSERTATION SUBMITTED TO THE GRADUATE DIVISION OF THE UNIVERSITY OF HAWAI‘I IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY IN GEOLOGY AND GEOPHYSICS DECEMBER 2009 By Joshua T.S. Cahill Dissertation Committee: Paul G. Lucey, Chairperson G. Jeffrey Taylor Patricia Fryer Jeffrey J. Gillis-Davis Trevor Sorensen Student: Joshua T.S. Cahill Student ID#: 1565-1460 Field: Geology and Geophysics Graduation date: December 2009 Title: The Composition of the Lunar Crust: Radiative Transfer Modeling and Analysis of Lunar Visible and Near-Infrared Spectra We certify that we have read this dissertation and that, in our opinion, it is satisfactory in scope and quality as a dissertation for the degree of Doctor of Philosophy in Geology and Geophysics. Dissertation Committee: Names Signatures Paul G. Lucey, Chairperson ____________________________ G. Jeffrey Taylor ____________________________ Jeffrey J. Gillis-Davis ____________________________ Patricia Fryer ____________________________ Trevor Sorensen ____________________________ ACKNOWLEDGEMENTS I must first express my love and appreciation to my family. Thank you to my wife Karen for providing love, support, and perspective. And to our little girl Maggie who only recently became part of our family and has already provided priceless memories in the form of beautiful smiles, belly laughs, and little bear hugs. The two of you provided me with the most meaningful reasons to push towards the "finish line". I would also like to thank my immediate and extended family. Many of them do not fully understand much about what I do, but support the endeavor acknowledging that if it is something I’m willing to put this much effort into, it must be worthwhile. -
OSAA Boys Track & Field Championships
OSAA Boys Track & Field Championships 4A Individual State Champions Through 2006 100-METER DASH 1992 Seth Wetzel, Jesuit ............................................ 1:53.20 1978 Byron Howell, Central Catholic................................. 10.5 1993 Jon Ryan, Crook County ..................................... 1:52.44 300-METER INTERMEDIATE HURDLES 1979 Byron Howell, Central Catholic............................... 10.67 1994 Jon Ryan, Crook County ..................................... 1:54.93 1978 Rourke Lowe, Aloha .............................................. 38.01 1980 Byron Howell, Central Catholic............................... 10.64 1995 Bryan Berryhill, Crater ....................................... 1:53.95 1979 Ken Scott, Aloha .................................................. 36.10 1981 Kevin Vixie, South Eugene .................................... 10.89 1996 Bryan Berryhill, Crater ....................................... 1:56.03 1980 Jerry Abdie, Sunset ................................................ 37.7 1982 Kevin Vixie, South Eugene .................................... 10.64 1997 Rob Vermillion, Glencoe ..................................... 1:55.49 1981 Romund Howard, Madison ....................................... 37.3 1983 John Frazier, Jefferson ........................................ 10.80w 1998 Tim Meador, South Medford ............................... 1:55.21 1982 John Elston, Lebanon ............................................ 39.02 1984 Gus Envela, McKay............................................. 10.55w 1999 -
On the Moon with Apollo 16. a Guidebook to the Descartes Region. INSTITUTION National Aeronautics and Space Administration, Washington, D.C
DOCUMENT RESUME ED 062 148 SE 013 594 AUTHOR Simmons, Gene TITLE On the Moon with Apollo 16. A Guidebook to the Descartes Region. INSTITUTION National Aeronautics and Space Administration, Washington, D.C. REPORT NO NASA-EP-95 PUB DATE Apr 72 NOTE 92p. AVAILABLE FROM Superintendent of Documents, Government Printing Office, Washington, D. C. 20402 (Stock Number 3300-0421, $1.00) EDRS PRICE MF-$0.65 HC-$3.29 DESCRIPTORS *Aerospace Technology; Astronomy; *Lunar Research; Resource Materials; Scientific Research; *Space Sciences IDENTIFIERS NASA ABSTRACT The Apollo 16 guidebook describes and illustrates (with artist concepts) the physical appearance of the lunar region visited. Maps show the planned traverses (trips on the lunar surface via Lunar Rover); the plans for scientific experiments are described in depth; and timelines for all activities are included. A section on uThe Crewn is illustrated with photos showing training and preparatory activities. (Aathor/PR) ON THE MOON WITH APOLLO 16 A Guidebook to the Descartes Region U.S. DEPARTMENT OF HEALTH. EDUCATION & WELFARE OFFICE OF EDUCATION THIS DOCUMENT HAS BEEN REPRO- DUCED EXACTLY AS RECEIVED FROM THE PERSON OR ORGANIZATION ORIG- grIl INATING IT POINTS OF VIEW OR OPIN- IONS STATED DO NOT NECESSARILY REPRESENT OFFICIAL OFFICE OF EDU- CATION POSITION on POLICY. JAI -0110 44 . UP. 16/11.4LI NATIONAL AERONAUTICS AND SPACE ADMINISTRATION April 1972 EP-95 kr) ON THE MOON WITH APOLLO 16 A Guidebook to the Descartes Region by Gene Simmons A * 40. 7 NATIONAL AERONAUTICS AND SPACE ADMINISTRATION April 1972 2 Gene Simmons was Chief Scientist of the Manned Spacecraft Center in Houston for two years and isnow Professor of Geophysics at the Mas- sachusetts Institute of Technology. -
NEAR INFRARED REFLECTANCE DATA. C. M. Pieters, Dept. Geo. Sci., Brown Univ., Providence, RI 0291 2
COMPOSITION OF THE UPPER LUNAR CRUST: PRELIMINARY RESULTS FROM NEAR INFRARED REFLECTANCE DATA. C. M. Pieters, Dept. Geo. Sci., Brown Univ., Providence, RI 0291 2. A data acquisition program has been in progress for three years to ob- tain mineralogical information about unsampl ed areas of the nearside 1 unar crust using near-infrared reflectance measurements of surface material. A sufficient number of areas have now been re1 iably measured to provide an es- timation of the type and variety of mineralogical rock types to expect for the upper 10 km of lunar crust. Although earthbased data are not adequate for a global survey it is clear 1 ) that distinct rock assemblages do exist at the observed scale for the upper kilometer of highland material and similar miner- al assemblages occur at widely separated regions, and 2) that material exca- vated from 5 to 10 km depth exhibit a different array of rock types, only some of which have been suspected from lunar sample studies. Data Ac uisi tion. Near-infrared ref1 ectance spectra (120 channels from .7 to_4__ 2.5 vm have been acquired for about 60 specific targets on the lunar nearside high1 ands. The observed areas (fresh simp1 e craters, massifs, and large craters with central peaks) are 4 to 10 km in diameter and were chosen because they do not exhibit a we1 1 developed soil . A1 1 data were acquired with an infrared spectrometer and an InSb detector (McCord --et al., 1981) using the 2.2m telescope of Mauna Kea Observatory. Independent measurements were repeated for at least a third of the areas observed. -
Volcanism on Mercury
SPECIALSECTION theLRMarealsoseenintheMASCSdata(30). References and Notes 22. P. G. Lucey, D. T. Blewett, B. L. Jolliff, J. Geophys. Res. From these observations and previous work 1. S. E. Hawkins III et al., Space Sci. Rev. 131, 247 (2007). 105, 20297 (2000). 2–7 10 18 21 ’ 2. T. B. McCord, J. B. Adams, Icarus 17, 585 (1972). 23. G. Heiken, D. T. Vaniman, B. M. French, Lunar ( , , , ), we propose that Mercury scrust 3. B. Hapke, G. E. Danielson Jr., K. Klaasen, L. Wilson, Sourcebook: A User's Guide to the Moon (Cambridge is composed of iron-poor calcium-magnesium sili- J. Geophys. Res. 80, 2431 (1975). Univ. Press, New York, 1991). cates (e.g., plagioclase, enstatite, pigeonite, and diop- 4. J. Warell, Icarus 161, 199 (2003). 24. S. K. Noble, C. M. Pieters, Sol. Syst. Res. 37, 31 (2003). side) with a detectable component of spectrally 5. F. Vilas, in Mercury,F.Vilas,C.R.Chapman,M.S.Mathews, 25. M. J. Cintala, J. Geophys. Res. 97, 947 (1992). – Meteorit. Planet. neutral opaque minerals. Ilmenite (FeTiO )isthe Eds. (Univ. of Arizona Press, Tucson, 1988), pp. 59 76. 26. D. T. Blewett, B. R. Hawke, P. G. Lucey, 3 6. A. L. Sprague, T. L. Roush, Icarus 133, 174 (1998). Sci. 37, 1245 (2002). most likely candidate based on lunar analogy and 7. J. Warell, D. T. Blewett, Icarus 168, 257 (2004). 27. B. R. Hawke, P. G. Lucey, J. F. Bell, R. Jaumann, G. Neukum, cosmochemical abundance considerations. This 8. B. Hapke, J. Geophys. Res. 106, 10039 (2001). Lunar Planet.