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Autobiography of Sir George Biddell Airy by George Biddell Airy 1
Autobiography of Sir George Biddell Airy by George Biddell Airy 1 CHAPTER I. CHAPTER II. CHAPTER III. CHAPTER IV. CHAPTER V. CHAPTER VI. CHAPTER VII. CHAPTER VIII. CHAPTER IX. CHAPTER X. CHAPTER I. CHAPTER II. CHAPTER III. CHAPTER IV. CHAPTER V. CHAPTER VI. CHAPTER VII. CHAPTER VIII. CHAPTER IX. CHAPTER X. Autobiography of Sir George Biddell Airy by George Biddell Airy The Project Gutenberg EBook of Autobiography of Sir George Biddell Airy by George Biddell Airy This eBook is for the use of anyone anywhere at no cost and with almost no restrictions whatsoever. You may copy it, give it away or re-use it under the terms of the Project Gutenberg Autobiography of Sir George Biddell Airy by George Biddell Airy 2 License included with this eBook or online at www.gutenberg.net Title: Autobiography of Sir George Biddell Airy Author: George Biddell Airy Release Date: January 9, 2004 [EBook #10655] Language: English Character set encoding: ISO-8859-1 *** START OF THIS PROJECT GUTENBERG EBOOK SIR GEORGE AIRY *** Produced by Joseph Myers and PG Distributed Proofreaders AUTOBIOGRAPHY OF SIR GEORGE BIDDELL AIRY, K.C.B., M.A., LL.D., D.C.L., F.R.S., F.R.A.S., HONORARY FELLOW OF TRINITY COLLEGE, CAMBRIDGE, ASTRONOMER ROYAL FROM 1836 TO 1881. EDITED BY WILFRID AIRY, B.A., M.Inst.C.E. 1896 PREFACE. The life of Airy was essentially that of a hard-working, business man, and differed from that of other hard-working people only in the quality and variety of his work. It was not an exciting life, but it was full of interest, and his work brought him into close relations with many scientific men, and with many men high in the State. -
Martian Crater Morphology
ANALYSIS OF THE DEPTH-DIAMETER RELATIONSHIP OF MARTIAN CRATERS A Capstone Experience Thesis Presented by Jared Howenstine Completion Date: May 2006 Approved By: Professor M. Darby Dyar, Astronomy Professor Christopher Condit, Geology Professor Judith Young, Astronomy Abstract Title: Analysis of the Depth-Diameter Relationship of Martian Craters Author: Jared Howenstine, Astronomy Approved By: Judith Young, Astronomy Approved By: M. Darby Dyar, Astronomy Approved By: Christopher Condit, Geology CE Type: Departmental Honors Project Using a gridded version of maritan topography with the computer program Gridview, this project studied the depth-diameter relationship of martian impact craters. The work encompasses 361 profiles of impacts with diameters larger than 15 kilometers and is a continuation of work that was started at the Lunar and Planetary Institute in Houston, Texas under the guidance of Dr. Walter S. Keifer. Using the most ‘pristine,’ or deepest craters in the data a depth-diameter relationship was determined: d = 0.610D 0.327 , where d is the depth of the crater and D is the diameter of the crater, both in kilometers. This relationship can then be used to estimate the theoretical depth of any impact radius, and therefore can be used to estimate the pristine shape of the crater. With a depth-diameter ratio for a particular crater, the measured depth can then be compared to this theoretical value and an estimate of the amount of material within the crater, or fill, can then be calculated. The data includes 140 named impact craters, 3 basins, and 218 other impacts. The named data encompasses all named impact structures of greater than 100 kilometers in diameter. -
The Solar Wind Prevents Re-Accretion of Debris After Mercury's Giant Impact
Draft version February 21, 2020 Preprint typeset using LATEX style emulateapj v. 12/16/11 THE SOLAR WIND PREVENTS RE-ACCRETION OF DEBRIS AFTER MERCURY'S GIANT IMPACT Christopher Spalding1 & Fred C. Adams2;3 1Department of Astronomy, Yale University, New Haven, CT 06511 2Department of Physics, University of Michigan, Ann Arbor, MI 48109 and 3Department of Astronomy, University of Michigan, Ann Arbor, MI 48109 Draft version February 21, 2020 ABSTRACT The planet Mercury possesses an anomalously large iron core, and a correspondingly high bulk density. Numerous hypotheses have been proposed in order to explain such a large iron content. A long-standing idea holds that Mercury once possessed a larger silicate mantle which was removed by a giant impact early in the the Solar system's history. A central problem with this idea has been that material ejected from Mercury is typically re-accreted onto the planet after a short ( Myr) timescale. Here, we show that the primordial Solar wind would have provided sufficient drag∼ upon ejected debris to remove them from Mercury-crossing trajectories before re-impacting the planet's surface. Specifically, the young Sun likely possessed a stronger wind, fast rotation and strong magnetic field. Depending upon the time of the giant impact, the ram pressure associated with this wind would push particles outward into the Solar system, or inward toward the Sun, on sub-Myr timescales, depending upon the size of ejected debris. Accordingly, the giant impact hypothesis remains a viable pathway toward the removal of planetary mantles, both on Mercury and extrasolar planets, particularly those close to young stars with strong winds. -
Specials Resign Witb Stomach and Liver Trouble?
DRY GOODH DRY GOODS. but has promised to issue a étalement ÍR6INIA TO-DAY'S TELEGRAPHIC NEWí* ^KOM WASHINGTON. alter tbe eeeeion of the convention to¬ IffiWfi of the Alexandria Oaaett·,] Holt F. ha* been appointed The Situation at Martinique LANSBURGH & BRO., f orr«»p-i'd»Ticw day. But, j'., 16 .M. gover¬ Wasbingtan, D. C , May 16. An csu-ed a sc-nnutional postmaster at Puitimoutb. Parie, May L'Heurre, Favorite Store. Englishman tele¬ Washington'* Dr. Jung, the physician of Lord some among aristocratic sped it« r-» of a Confederate Memorial Day was ob¬ nor pro tem of Mart.nique, today Pauricefote, tbe British Ambassador, circus io Madrid, yesterdav, 0] ti e Ing served at Norfolk yettarday witb ap¬ graphed the minia »r of colonies that Business Hours 8 a. rn. to ß p. na. «aid Ibis morning tbat bis patient wee the Duke of Arion with a laid« ? w bip. propriât» ceremonies. all the city achieves of St. Pierre were Saturdays 9 o'clock. from the disease man wanted to a club of «Lieh 10th, llthtBtlFSts.. N.W. in no serious danger The join Tbomas Savege bas been appointed los*, in the destruction of tbat be is sull-ring, and that the Duke is a member. A council of re¬ city. with wbicb postmaster to succeed W. L. Taylor, Mount tbe Governor reports that be wa9 thing were un¬ bonor, witb tbe Doke as president, signed, at Aebgrove, Fairfax county. Pelee, acting says, founded. "He bas gout io aa acute considered his application, and rejeve'ed Judge B. -
Journal of Geophysical Research: Planets
Journal of Geophysical Research: Planets RESEARCH ARTICLE On the relative importance of thermal and chemical buoyancy 10.1002/2016JE005221 in regular and impact-induced melting Key Points: in a Mars-like planet • Compositional buoyancy stabilizes melting-induced anomalies at the base of the lithosphere Thomas Ruedas1,2 and Doris Breuer2 • The anomalies may be detectable by gravimetry but not by seismics with a 1Institute of Planetology, Westfälische Wilhelms-Universität Münster, Münster, Germany, 2Institute of Planetary Research, sparse station network • Neglecting impact-induced mantle German Aerospace Center (DLR), Berlin, Germany anomalies results in overestimation of the local crustal thickness Abstract We ran several series of two-dimensional numerical mantle convection simulations representing in idealized form the thermochemical evolution of a Mars-like planet. In order to study the Supporting Information: • Supporting Information S1 importance of compositional buoyancy of melting mantle, the models were set up in pairs of one including •MovieS1 all thermal and compositional contributions to buoyancy and one accounting only for the thermal •MovieS2 contributions. In several of the model pairs, single large impacts were introduced as causes of additional strong local anomalies, and their evolution in the framework of the convecting mantle was tracked. The Correspondence to: models confirm that the additional buoyancy provided by the depletion of the mantle by regular melting T. Ruedas, can establish a global stable stratification of the convecting mantle and throttle crust production. [email protected] Furthermore, the compositional buoyancy is essential in the stabilization and preservation of local compositional anomalies directly beneath the lithosphere and offers a possible explanation for the Citation: Ruedas, T. -
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, -
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 -
Strategies for Detecting Biological Molecules on Titan
ASTROBIOLOGY Volume 18, Number 5, 2018 ª Mary Ann Liebert, Inc. DOI: 10.1089/ast.2017.1758 Strategies for Detecting Biological Molecules on Titan Catherine D. Neish,1 Ralph D. Lorenz,2 Elizabeth P. Turtle,2 Jason W. Barnes,3 Melissa G. Trainer,4 Bryan Stiles,5 Randolph Kirk,6 Charles A. Hibbitts,2 and Michael J. Malaska5 Abstract Saturn’s moon Titan has all the ingredients needed to produce ‘‘life as we know it.’’ When exposed to liquid water, organic molecules analogous to those found on Titan produce a range of biomolecules such as amino acids. Titan thus provides a natural laboratory for studying the products of prebiotic chemistry. In this work, we examine the ideal locales to search for evidence of, or progression toward, life on Titan. We determine that the best sites to identify biological molecules are deposits of impact melt on the floors of large, fresh impact craters, specifically Sinlap, Selk, and Menrva craters. We find that it is not possible to identify biomolecules on Titan through remote sensing, but rather through in situ measurements capable of identifying a wide range of biological molecules. Given the nonuniformity of impact melt exposures on the floor of a weathered impact crater, the ideal lander would be capable of precision targeting. This would allow it to identify the locations of fresh impact melt deposits, and/or sites where the melt deposits have been exposed through erosion or mass wasting. Determining the extent of prebiotic chemistry within these melt deposits would help us to understand how life could originate on a world very different from Earth. -
MAFIC ANOMOLIES in the LUNAR HIGHLANDS. T. A. Giguere1,2, B
Lunar and Planetary Science XXXI 1760.pdf MAFIC ANOMOLIES IN THE LUNAR HIGHLANDS. T. A. Giguere1,2, B. Ray Hawke1, G. A. Smith, G. Jeffrey Taylor1, D. T. Blewett1, P. G. Lucey1, and P. D. Spudis3, 1Hawai’i Inst. of Geophys. and Planetology, University of Hawai`i, 2525 Correa Rd., Honolulu, HI 96822, 2Intergraph Corporation, 2828 Pa’a St. Ste. 2150, Honolulu, HI 96819, 3Lunar and Planetary Institute, Houston, TX 77058. Introduction Results and Discussion Ancient mare basalts deposits that have been hidden Southern Central Highlands. Most of the southern or obscured by superposed higher albedo material are portion of the lunar central highlands exhibit FeO referred to as cryptomaria [1, 2, 3]. They represent a values that range between 5 and 9 wt. % and TiO2 record of the earliest mare volcanism. Earlier remote values less than 1 wt. %. However, a small area with sensing and geologic studies have provided evidence anomalously high FeO values has been identified near for the distribution of ancient mare volcanism. the 114 km Maurolycus crater at the crater Buch B. Schultz and Spudis [4] studied the distribution of dark-haloed impact craters in the lunar highlands. Maurolycus is located at 14.0° E, 41.8° S and Buch B They suggested that basaltic volcanism predated the is located at 17.0° E, 39.9° S. last major basin-forming impacts and that early mare volcanism may have been widespread. Hawke and Bell [5, 6] used near-IR spectra to demonstrate that many dark-haloed impact craters excavated ancient mare units buried by basin and crater ejecta. -
Summary of Sexual Abuse Claims in Chapter 11 Cases of Boy Scouts of America
Summary of Sexual Abuse Claims in Chapter 11 Cases of Boy Scouts of America There are approximately 101,135sexual abuse claims filed. Of those claims, the Tort Claimants’ Committee estimates that there are approximately 83,807 unique claims if the amended and superseded and multiple claims filed on account of the same survivor are removed. The summary of sexual abuse claims below uses the set of 83,807 of claim for purposes of claims summary below.1 The Tort Claimants’ Committee has broken down the sexual abuse claims in various categories for the purpose of disclosing where and when the sexual abuse claims arose and the identity of certain of the parties that are implicated in the alleged sexual abuse. Attached hereto as Exhibit 1 is a chart that shows the sexual abuse claims broken down by the year in which they first arose. Please note that there approximately 10,500 claims did not provide a date for when the sexual abuse occurred. As a result, those claims have not been assigned a year in which the abuse first arose. Attached hereto as Exhibit 2 is a chart that shows the claims broken down by the state or jurisdiction in which they arose. Please note there are approximately 7,186 claims that did not provide a location of abuse. Those claims are reflected by YY or ZZ in the codes used to identify the applicable state or jurisdiction. Those claims have not been assigned a state or other jurisdiction. Attached hereto as Exhibit 3 is a chart that shows the claims broken down by the Local Council implicated in the sexual abuse. -
Analyses of High-Iron Sedimentary Bedrock and Diagenetic Features Observed with Chemcam at Vera Rubin Ridge, Gale Crater, Mars: Calibration and Characterization G
Analyses of High-Iron Sedimentary Bedrock and Diagenetic Features Observed With ChemCam at Vera Rubin Ridge, Gale Crater, Mars: Calibration and Characterization G. David, A. Cousin, O. Forni, P.-y. Meslin, E. Dehouck, N. Mangold, J. l’Haridon, W. Rapin, O. Gasnault, J. R. Johnson, et al. To cite this version: G. David, A. Cousin, O. Forni, P.-y. Meslin, E. Dehouck, et al.. Analyses of High-Iron Sedimentary Bedrock and Diagenetic Features Observed With ChemCam at Vera Rubin Ridge, Gale Crater, Mars: Calibration and Characterization. Journal of Geophysical Research. Planets, Wiley-Blackwell, 2020, 125 (10), 10.1029/2019JE006314. hal-03093150 HAL Id: hal-03093150 https://hal.archives-ouvertes.fr/hal-03093150 Submitted on 16 Jan 2021 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. David Gaël (Orcid ID: 0000-0002-2719-1586) Cousin Agnès (Orcid ID: 0000-0001-7823-7794) Forni Olivier (Orcid ID: 0000-0001-6772-9689) Meslin Pierre-Yves (Orcid ID: 0000-0002-0703-3951) Dehouck Erwin (Orcid ID: 0000-0002-1368-4494) Mangold Nicolas (Orcid ID: 0000-0002-0022-0631) Rapin William (Orcid ID: 0000-0003-4660-8006) Gasnault Olivier (Orcid ID: 0000-0002-6979-9012) Johnson Jeffrey, R.