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March 2017 17Th a Religious Holiday
The Rocket Review Raritan High School’s Official Newspaper 39.6 million people claim to have Irish heritage, The Day of the Irish 127 million people will celebrate the holiday. That By: Thomas Grady is 7 times greater than Ireland’s population! March is a month full of holidays, but one that In Ireland, on the other hand, they did see St. stands out is St. Patrick’s Day. Every March 17th, Patrick’s Day as a religious holiday. In the 1970’s all of America celebrates their Irish heritage. the government would close the pubs in Ireland Though not a national holiday, many people take so they could get the people to go to church and off from work and studies to embrace the Irish pray for St. Patrick. But since the mid-90’s the spirit. The day of St. Pat’s isn’t really a celebra- government made it a joyous holiday, giving it a tion in Ireland, it’s more of a solemn affair. multi day festival in the capital of Dublin. They have festivals, dances, and a parade. Not only Ireland’s patron saint is recognized in America does this happen in Dublin, it happens all around because of Irish immigrants who made March Ireland. Careful because in the first paragraph, 2017 March 17th a religious holiday. The man for whom St. you state that it is serious in Ireland. Patrick’s Day is named was born into an aris- In closing, when you see March 17th coming up tocratic family in Roman Britain around the end in the calendar, grab your leprechaun hat, lucky of the fourth century. -
Impact Crater Collapse
P1: SKH/tah P2: KKK/mbg QC: KKK/arun T1: KKK March 12, 1999 17:54 Annual Reviews AR081-12 Annu. Rev. Earth Planet. Sci. 1999. 27:385–415 Copyright c 1999 by Annual Reviews. All rights reserved IMPACT CRATER COLLAPSE H. J. Melosh Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721; e-mail: [email protected] B. A. Ivanov Institute for Dynamics of the Geospheres, Russian Academy of Sciences, Moscow, Russia 117979 KEY WORDS: crater morphology, dynamical weakening, acoustic fluidization, transient crater, central peaks ABSTRACT The detailed morphology of impact craters is now believed to be mainly caused by the collapse of a geometrically simple, bowl-shaped “transient crater.” The transient crater forms immediately after the impact. In small craters, those less than approximately 15 km diameter on the Moon, the steepest part of the rim collapses into the crater bowl to produce a lens of broken rock in an otherwise unmodified transient crater. Such craters are called “simple” and have a depth- to-diameter ratio near 1:5. Large craters collapse more spectacularly, giving rise to central peaks, wall terraces, and internal rings in still larger craters. These are called “complex” craters. The transition between simple and complex craters depends on 1/g, suggesting that the collapse occurs when a strength threshold is exceeded. The apparent strength, however, is very low: only a few bars, and with little or no internal friction. This behavior requires a mechanism for tem- porary strength degradation in the rocks surrounding the impact site. Several models for this process, including acoustic fluidization and shock weakening, have been considered by recent investigations. -
Evolution of the Lunar Crust Recorded in the Meteoritic
EVOLUTION OF THE LUNAR CRUST RECORDED IN THE METEORITIC FELDSPATHIC REGOLITH BRECCIAS NORTHWEST AFRICA 10291 AND 11182: INSIGHTS INTO THE HETEROGENEITY AND PETROGENESIS OF CRUSTAL LITHOLOGIES USING PETROLOGY AND MINERAL CHEMISTRY By SHANNON BOYLE A thesis submitted to the School of Graduate Studies Rutgers, The State University of New Jersey In partial fulfillment of the requirements For the degree of Master of Science Graduate Program in Earth and Planetary Science Written under the direction of Doctor Juliane Gross And approved by _____________________________________ _____________________________________ _____________________________________ _____________________________________ New Brunswick, New Jersey October 2019 TITLE PAGE ABSTRACT OF THE THESIS Evolution of the lunar crust recorded in the meteoritic feldspathic regolith breccias Northwest Africa 10291 and 11182: Insights into the heterogeneity and petrogenesis of crustal lithologies using petrology and mineral chemistry by SHANNON BOYLE Thesis Director: Doctor Juliane Gross Abstract The geology of the Moon represents nearly a continuous geological record from its formation during the giant impact that resulted in the Earth-Moon system, to its state today. Therefore, it is a prime location for understanding one path of planetary evolution. Lunar meteorites are on average samples of rock and regolith from random areas on the lunar surface. As such, they represent our best available tools to study the crustal evolution of the Moon because they provide data on lunar petrology, geochemistry, and chronology, as well as data on the variety of existing lunar lithologies different from Apollo and Luna mission sample return sites. We investigated two lunar feldspathic regolith breccias found in 2017, Northwest Africa (NWA) 10291 and NWA 11182, to understand their petrogenetic origin and, more broadly, the evolution of lithologies present in unsampled areas of the Moon and place constraints on lunar crustal evolution in these areas. -
ANIC IMPACTS: MS and IRONMENTAL P ONS Abstracts Edited by Rainer Gersonde and Alexander Deutsch
ANIC IMPACTS: MS AND IRONMENTAL P ONS APRIL 15 - APRIL 17, 1999 Alfred Wegener Institute for Polar and Marine Research Bremerhaven, Germany Abstracts Edited by Rainer Gersonde and Alexander Deutsch Ber. Polarforsch. 343 (1999) ISSN 01 76 - 5027 Preface .......3 Acknowledgements .......6 Program ....... 7 Abstracts P. Agrinier, A. Deutsch, U. Schäre and I. Martinez: On the kinetics of reaction of CO, with hot Ca0 during impact events: An experimental study. .11 L. Ainsaar and M. Semidor: Long-term effect of the Kärdl impact crater (Hiiumaa, Estonia) On the middle Ordovician carbonate sedimentation. ......13 N. Artemieva and V.Shuvalov: Shock zones on the ocean floor - Numerical simulations. ......16 H. Bahlburg and P. Claeys: Tsunami deposit or not: The problem of interpreting the siliciclastic K/T sections in northeastern Mexico. ......19 R. Coccioni, D. Basso, H. Brinkhuis, S. Galeotti, S. Gardin, S. Monechi, E. Morettini, M. Renard, S. Spezzaferri, and M. van der Hoeven: Environmental perturbation following a late Eocene impact event: Evidence from the Massignano Section, Italy. ......21 I von Dalwigk and J. Ormö Formation of resurge gullies at impacts at sea: the Lockne crater, Sweden. ......24 J. Ebbing, P. Janle, J, Koulouris and B. Milkereit: Palaeotopography of the Chicxulub impact crater and implications for oceanic craters. .25 V. Feldman and S.Kotelnikov: The methods of shock pressure estimation in impacted rocks. ......28 J.-A. Flores, F. J. Sierro and R. Gersonde: Calcareous plankton stratigraphies from the "Eltanin" asteroid impact area: Strategies for geological and paleoceanographic reconstruction. ......29 M.V.Gerasimov, Y. P. Dikov, 0 . I. Yakovlev and F.Wlotzka: Experimental investigation of the role of water in the impact vaporization chemistry. -
Florida Units 7–12
Level 1 Florida Units 7–12 STUDENT BOOK Lesson 1 | Reading Louisa Moats, Ed.D., Author REVIEWER’S DRAFT Through the glass bottom of my tourist boat I see the dolphin pod afloat. I hear whistles as high as the Empire State And know they are trying to communicate. 5 Each dolphin has a unique sound That it wears like a name tag, while swimming around. Now I hear the sound of a quickly spinning wheel. It must be a dolphin trying to find its next meal. In murky water the dolphin’s as blind as a bat. 10 It uses clicks to “see” where it is at. Using sonar, the sounds bounce off what’s near. Distance, depth, and size are what the dolphin can hear. Moans and squeaks echo in the abyss. Dolphins alert each other of danger in their midst. 15 Atop their heads, the blowholes emit sound As if beautifully played instruments abound. In the boat I can hear many sounds from the sea. The music of the dolphin is like a song written for me. Unit 7 7 Level 1 Fl ida Units 7–12 STUDENT BOOK Louisa Moats, Ed.D., Author Lesson 1 | Reading Through the glass bottom of my tourist boat I see the dolphin pod afloat. I hear whistles as high as the Empire State And know they are trying to communicate. 5 Each dolphin has a unique sound That it wears like a name tag, while swimming around. Now I hear the sound of a quickly spinning wheel. It must be a dolphin trying to find its next meal. -
GRAIL Gravity Observations of the Transition from Complex Crater to Peak-Ring Basin on the Moon: Implications for Crustal Structure and Impact Basin Formation
Icarus 292 (2017) 54–73 Contents lists available at ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus GRAIL gravity observations of the transition from complex crater to peak-ring basin on the Moon: Implications for crustal structure and impact basin formation ∗ David M.H. Baker a,b, , James W. Head a, Roger J. Phillips c, Gregory A. Neumann b, Carver J. Bierson d, David E. Smith e, Maria T. Zuber e a Department of Geological Sciences, Brown University, Providence, RI 02912, USA b NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA c Department of Earth and Planetary Sciences and McDonnell Center for the Space Sciences, Washington University, St. Louis, MO 63130, USA d Department of Earth and Planetary Sciences, University of California, Santa Cruz, CA 95064, USA e Department of Earth, Atmospheric and Planetary Sciences, MIT, Cambridge, MA 02139, USA a r t i c l e i n f o a b s t r a c t Article history: High-resolution gravity data from the Gravity Recovery and Interior Laboratory (GRAIL) mission provide Received 14 September 2016 the opportunity to analyze the detailed gravity and crustal structure of impact features in the morpho- Revised 1 March 2017 logical transition from complex craters to peak-ring basins on the Moon. We calculate average radial Accepted 21 March 2017 profiles of free-air anomalies and Bouguer anomalies for peak-ring basins, protobasins, and the largest Available online 22 March 2017 complex craters. Complex craters and protobasins have free-air anomalies that are positively correlated with surface topography, unlike the prominent lunar mascons (positive free-air anomalies in areas of low elevation) associated with large basins. -
1 the Lifecycle of Hollows on Mercury
The Lifecycle of Hollows on Mercury: An Evaluation of Candidate Volatile Phases and a Novel Model of Formation. 1 1 2 3 M. S. Phillips , J. E. Moersch , C. E. Viviano , J. P. Emery 1Department of Earth and Planetary Sciences, University of Tennessee, Knoxville 2Planetary Exploration Group, Johns Hopkins University Applied Physics Laboratory 3Department of Astronomy and Planetary Sciences, Northern Arizona University Corresponding author: Michael Phillips ([email protected]) Keywords: Mercury, hollows, thermal model, fumarole. Abstract On Mercury, high-reflectance, flat-floored depressions called hollows are observed nearly globally within low-reflectance material, one of Mercury’s major color units. Hollows are thought to be young, or even currently active, features that form via sublimation, or a “sublimation-like” process. The apparent abundance of sulfides within LRM combined with spectral detections of sulfides associated with hollows suggests that sulfides may be the phase responsible for hollow formation. Despite the association of sulfides with hollows, it is still not clear whether sulfides are the hollow-forming phase. To better understand which phase(s) might be responsible for hollow formation, we calculated sublimation rates for 57 candidate hollow-forming volatile phases from the surface of Mercury and as a function of depth beneath regolith lag deposits of various thicknesses. We found that stearic acid (C18H36O2), fullerenes (C60, C70), and elemental sulfur (S) have the appropriate thermophysical properties to explain hollow formation. Stearic acid and fullerenes are implausible hollow-forming phases because they are unlikely to have been delivered to or generated on Mercury in high enough volume to account for hollows. -
Exploring Potential Water-Ice Occurrence on Asteroid 4 Vesta Using Orbital Radar Observations by the Dawn Mission
Western Michigan University ScholarWorks at WMU Dissertations Graduate College 12-2018 Exploring Potential Water-Ice Occurrence on Asteroid 4 Vesta Using Orbital Radar Observations by the Dawn Mission Elizabeth M. Palmer Follow this and additional works at: https://scholarworks.wmich.edu/dissertations Part of the Geology Commons Recommended Citation Palmer, Elizabeth M., "Exploring Potential Water-Ice Occurrence on Asteroid 4 Vesta Using Orbital Radar Observations by the Dawn Mission" (2018). Dissertations. 3359. https://scholarworks.wmich.edu/dissertations/3359 This Dissertation-Open Access is brought to you for free and open access by the Graduate College at ScholarWorks at WMU. It has been accepted for inclusion in Dissertations by an authorized administrator of ScholarWorks at WMU. For more information, please contact [email protected]. EXPLORING POTENTIAL WATER-ICE OCCURRENCE ON ASTEROID 4 VESTA USING ORBITAL RADAR OBSERVATIONS BY THE DAWN MISSION by Elizabeth M. Palmer A dissertation submitted to the Graduate College in partial fulfillment of the requirements for the degree of Doctor of Philosophy Geological and Environmental Sciences Western Michigan University December 2018 Doctoral Committee: William A. Sauck, Ph.D., Chair Essam Heggy, Ph.D. Wlodek Kofman, Ph.D. Johnson R. Haas, Ph.D. © 2018 Elizabeth M. Palmer ACKNOWLEDGEMENTS I would like to thank all of my peers who have supported me throughout the many stages of academic and personal growth that have led to the completion of this culminating document. I would also like to thank all those who acted as mentors along the way, especially Essam, who has shared considerable advice on charting the path toward a successful, fulfilling career in the Earth and planetary sciences. -
Science Concept 3: Key Planetary
Science Concept 6: The Moon is an Accessible Laboratory for Studying the Impact Process on Planetary Scales Science Concept 6: The Moon is an accessible laboratory for studying the impact process on planetary scales Science Goals: a. Characterize the existence and extent of melt sheet differentiation. b. Determine the structure of multi-ring impact basins. c. Quantify the effects of planetary characteristics (composition, density, impact velocities) on crater formation and morphology. d. Measure the extent of lateral and vertical mixing of local and ejecta material. INTRODUCTION Impact cratering is a fundamental geological process which is ubiquitous throughout the Solar System. Impacts have been linked with the formation of bodies (e.g. the Moon; Hartmann and Davis, 1975), terrestrial mass extinctions (e.g. the Cretaceous-Tertiary boundary extinction; Alvarez et al., 1980), and even proposed as a transfer mechanism for life between planetary bodies (Chyba et al., 1994). However, the importance of impacts and impact cratering has only been realized within the last 50 or so years. Here we briefly introduce the topic of impact cratering. The main crater types and their features are outlined as well as their formation mechanisms. Scaling laws, which attempt to link impacts at a variety of scales, are also introduced. Finally, we note the lack of extraterrestrial crater samples and how Science Concept 6 addresses this. Crater Types There are three distinct crater types: simple craters, complex craters, and multi-ring basins (Fig. 6.1). The type of crater produced in an impact is dependent upon the size, density, and speed of the impactor, as well as the strength and gravitational field of the target. -
Bibliography
❖ Bibliography Note: This bibliography contains the sources used in the text above. To assist readers with other projects, it also includes a broader list of publications that have been involved in the developing story of the crater. Abrahams, H.J., ed. (1983) Heroic Efforts at Meteor Crater, Arizona: Selected Correspondence between Daniel Moreau Barringer and Elihu Thomson. Associated University Press, East Brunswick, 322 p. Ackermann, H.D. and Godson, R.H. (1966) P-wave velocity and attenuation summary, FY-66. In Investigation of in situ physical properties of surface and subsurface site materials by engineering gephysical techniques, annual report, fiscal year 1966, edited by J.S. Watkins. NASA Contractor Report (CR)-65502 and USGS Open-File Report 67-272, pp. 305-317. Ackermann, H.D., Godson, R.H., and Watkins, J.S. (1975) A seismic refraction technique used for subsurface investigations at Meteor crater, Arizona. Journal of Geophysical Research, v. 80, pp. 765- 775. Adler, B., Whiteman, C.D., Hoch, S.W., Lehner, M., and Kalthoff, N. (2012) Warm-air intrusions in Arizona’s Meteor Crater. Journal of Applied Meteorology and Climatology, v. 51, pp. 1010-1025. Ai, H.-A. and Ahrens, T.J. (2004) Dynamic tensile strength of terrestrial rocks and application to impact cratering. Meteoritics and Planetary Science, v. 39, pp. 233-246. Alexander, E.C. Jr. and Manuel, O.K. (1958) Isotopic anomalies of krypton and xenon in Canyon Diablo graphite. Earth and Planetary Science Letters, v. 2, pp. 220-224. Altomare, C.M., Fagan, A.L., and Kring, D.A. (2014) Eolian deposits of pyroclastic volcanic debris in Meteor Crater. -
Page 1 of 53 American Mineralogist Manuscript #4837 – Revision 1 1 2
1 American Mineralogist Manuscript #4837 – Revision 1 2 3 4 The petrogenesis of impact basin melt rocks in lunar meteorite Shişr 161 5 6 Axel Wittmann1,*, Randy L. Korotev1, Bradley L. Jolliff1, Thomas J. Lapen2, and 7 Anthony J. Irving3 8 9 1 Department of Earth and Planetary Sciences, Washington University St. Louis, Campus 10 Box 1169, 1 Brookings Dr., St. Louis, MO 63130-4899, USA 11 2 Department of Earth and Atmospheric Sciences, University of Houston, 4800 Calhoun 12 Road, Houston, Texas 77004. 13 3 Department of Earth and Space Sciences, University of Washington, 4000 15th Avenue 14 NE, Seattle, Washington 98195. 15 *corresponding author e-mail address: [email protected] 16 Page 1 of 53 17 ABSTRACT 18 This study explores the petrogenesis of Shişr 161, an immature lunar regolith 19 breccia meteorite with low abundances of incompatible elements, a feldspathic affinity, 20 and a significant magnesian component. Our approach was to identify all clasts >0.5 mm 21 in size in a thin section, characterize their mineral and melt components, and reconstruct 22 their bulk major and minor element compositions. Trace element concentrations in 23 representative clasts of different textural and compositional types indicate that the clast 24 inventory of Shişr 161 is dominated by impact melts that include slowly cooled cumulate 25 melt rocks with mafic magnesian mineral assemblages. Minor exotic components are 26 incompatible-element-rich melt spherules and glass fragments, and a gas-associated 27 spheroidal precipitate. Our hypothesis for the petrologic setting of Shişr 161 is that the 28 crystallized melt clasts originate from the upper ~1 km of the melt sheet of a 300 to 500 29 km diameter lunar impact basin in the Moon’s feldspathic highlands. -
The MIT Folk Dance Club Songbook
The MIT Folk Dance Club Songbook Argentina VivaJujuy(Bailecito) ...................................... 1 Armenia Guhneega............................................. 2 Karun,karun........................................... 2 Darimena............................................. 3 Sirunakhchik(Sweetgirl).................................... 4 Assyrian Ainokchume........................................... 5 Bulgaria Hodih gore, hodih dolu (Cetvornoˇ ˇsopsko horo) . 6 SnoˇstisiRadapristana(Kjustendilskar˘uˇcenica). 7 Sadimoma............................................ 8 HodilamijeBojana(Pravo) .................................. 9 Gjurabelibeloplatno(Pajduˇsko). 9 Tr˘ugnalaRumjana........................................ 10 OkolPleven(Pravo)....................................... 11 Petruno,pileˇsareno ....................................... 12 MajkaRada(Pravo)....................................... 13 Karamfil ............................................. 13 Tr˘ugnal mi Jane Sandanski. 14 Molih ta, majˇco, i molih (Pravo). 14 Suvatarjakaodapriteˇce..................................... 15 Znzngankele(Pravo)...................................... 15 Kucinata.............................................. 16 Mjatalo Lenˇce jab˘ulka (R˘uˇcenica) . 17 Unaˇsetoselo........................................... 18 Trakijskar˘uˇcenica......................................... 19 Canada Labastringue........................................... 20 La Ziguezon (An dro). 21 Croatia Hopˇzicaˇzica........................................... 22 LepamojaMilena........................................