THE ST. LUKE LETTER April 2021

Total Page:16

File Type:pdf, Size:1020Kb

THE ST. LUKE LETTER April 2021 THE ST. LUKE LETTER April 2021 Dear Siblings in Christ, Alleluia, Christ is risen! Christ is risen indeed, alleluia! I am simply loving spring this year. Looking at my gardens and seeing buds emerge from the ground and enjoying the blooms as they begin to open and fill the brown ground with a colorful palate has provided me with a reminder of the rebirth, we all experience and are gifted through Christ our Lord. The past year has provided us with ample opportunity to reflect and reassess our lives and how we spend our time, our money and use our talents and gifts. As we move forward into the celebration of Christ’s resurrection, we have a new opportunity to be renewed, refreshed in this spring’s rebirth along with Christ’s emergence from death to life. We are promised new life through Christ – eternal life through the grace and love of God. I pray that the flowers, the sunshine, the celebration of Christ’s resurrection inspire in you a new heart, a new joy through God. May this newness help us all to share God’s love with one another – with all people. May we gather together (using safe practices) to renew and refresh in God’s love and call to worship, prayer and praise. And may you know that you are loved by Christ our risen Lord! Yours In Christ, Pr. Becky Horn Are you or a loved one desiring a visit from the pastor? Please contact Pastor Becky if you would like her to call or visit you at home, in the hospital, or another location. (office: 364-9154, cell: 215-208-5535, email: [email protected]) *If you desire Communion at home, please contact Pr. Becky so that arrangements can be made. St. Luke Contact Numbers: Church Office 814-364-9154 or email at [email protected] Pastor, Rev. Becky Horn 215-208-5535 or email [email protected] Church Secretary, Patty Lehman 814-933-6296 or email: [email protected] Council President, Susan Stover 814-349-5173 or email: [email protected] St. Luke Mailing Address PO Box 331, Centre Hall, PA 16828 St. Luke Website http://StLukeCentreHall.org QUESTIONS TO PONDER – Where does our Mission Support Go? Mission Support: A Deep Dive Did you know that ELCA members in more than 8,900 congregations in the United States and Caribbean give approximately $1.7 billion in regular offerings annually to support ELCA ministries in their local communities and worldwide? When members give through their congregations, about 5.5% of that money is shared with the local synod, which then shares a portion with the national churchwide office. This unrestricted giving from congregations is called Mission Support. Mission Support gives the ELCA both the foundation and the fuel to do God’s work in the world locally, nationally and internationally. Thank you for your faithful support! 41% OF MISSION SUPPORT GROWS THE ELCA IN THE UNITED STATES: Plant and support hundreds of new congregations. Enable congregations to renew their ministries and reach out to their surrounding communities. Develop and share resources for faith, discipleship, prayer, stewardship and worship. Work together with our African-descent, American Indian, Alaska Native, Arab, Middle Eastern, Asian, Pacific Islander and Latino/Latina leaders and members. Invest in technology and communication. Grow and sustain financial resources. Engage in research and strategic planning. 22% OF MISSION SUPPORT GROWS THE LUTHERAN CHURCH AND ADDRESSES ISSUES AROUND THE WORLD: As a member of the Lutheran World Federation, the ELCA is in communion with 147 other churches. ELCA synods relate directly to 65 companion churches through a total of 127 official relationships. The ELCA accompanies new Lutheran churches, expands ministries and trains leaders and evangelists. The ELCA sends missionaries — including Young Adults in Global Mission — who are the hands and feet of Jesus around the world. The ELCA addresses social issues and works for justice. 37% OF MISSION SUPPORT HELPS DEVELOP CURRENT AND FUTURE LEADERS IN THE ELCA: Prepare and implement a system for recruitment and assignment of rostered ministers. Identify and provide ministry resources and opportunities to lay leaders for networking. Offer events and leadership opportunities for youth and young adults. Support the work of seven ELCA seminaries and 26 ELCA colleges and universities. Provide coordination and support for churchwide ministries. Provide governance and leadership. Sustain ecumenical and interfaith relations. For additional resources, go to ELCA.org/SOFIA In Person Worship at St. Luke: In Person Worship has resumed. We are holding one In Person worship service on Sundays at 10:30am. Covid-19 procedures will continue to be in place with your temperature taken and a limited attendance of 45 people. Please enter the main entrance doors which will open at approximately 10:15am. Please do not attend if you are not feeling well or have been exposed to someone with covid-19, are awaiting test results, or have tested positive in the past 14 days. Please wear a mask and social distance in designated pew spaces. St. Luke's Worship Service will also continue to be posted weekly to St. Luke’s YouTube Channel https://www.youtube.com/channel/UCndvYdWpi7qSKld6Y8cnHMg Live Worship on Zoom - In addition to St. Luke returning to In Person Worship on Sundays at 10:30am, and St. Luke's pre-recorded online YouTube Service, St. Luke will also offer Live streaming of our Sunday Worship Service over Zoom at 10:30am. Please see the link below to participate: Topic: Sunday Morning Worship Join Zoom Meeting https://us02web.zoom.us/j/82737550247?pwd=LzNSTmdVWFU3enlaOEJ2Q0wwaTF4QT09 Meeting ID: 827 3755 0247 Passcode: 201808 One tap mobile +13126266799,,82737550247#,,,,*201808# US (Chicago) +16468769923,,82737550247#,,,,*201808# US (New York) *A weekly bulletin will be sent via email for those who choose to join via Zoom. It is slightly different than the YouTube Worship at Home bulletin. Groups in St. Luke - The St. Luke Council voted to allow groups to use the building for activities and events. Groups that wish to resume using the building must schedule through the Church office and follow the protocols established for worship including wearing masks, remaining physically distant, answering health questions, and taking attendance for contact tracing. Groups must also designate a person to be the 'Cleaning Person.' Prior to the group's use of the building, the Cleaning Person must contact Pastor Becky, Derek Shaffer or Larry Frazier to set up a time to meet and discuss where the cleaning supplies are and learn the cleaning protocols. Once this meeting has occurred, the group may proceed with in person meetings that abide by current St. Luke policy. Currently the limit is up to 15% capacity for indoor events and gatherings. *Please be sure to see all policies and procedures for groups and in person worship that is posted in the narthex of St. Luke. Worship At Home—The Worship At Home service continues to be posted on the St. Luke Centre Hall YouTube Channel https://www.youtube.com/channel/UCndvYdWpi7qSKld6Y8cnHMg for the foreseeable future. If you desire Communion at home, please contact Pr. Becky so that arrangements can be made. IMPORTANT - Please Note—If you do not have email or online access and would like to receive the printed Worship At Home Mailing, please speak with Pastor Becky or Patty or leave a message at the Church Office at 814-364-9154. Worship Plan: The 8:00 am has been temporarily suspended while we continue to navigate the pandemic. There are several required procedures that we are instituting in order to provide the least risk for gathering as a group. We ask that those who plan to attend any gatherings, including worship, at the church agree to abide by the recommendations for the health of all. Currently, Gov. Wolf has recommended 15% capacity for indoor events and gatherings and Council has agreed to follow the recommendations from the governor’s office. Procedure for In House Worship: A. Entry to the building will be limited to the main front doors. Doors will open approximately 15 minutes before the start of the service. Requirements will include: temperature check via an infrared thermometer, answering a few questions about any symptoms or exposure to Covid-19, a mask covering the nose and mouth, and having their name recorded for the potential of contact tracing. If a person has a fever over 100F, we will ask them to not join us inside for worship. If a person answers 'Yes' to any of the following questions, they will be asked to not join us inside for worship. They may be given a copy of the bulletin and reminded that virtual worship is available on St. Luke's YouTube channel. a. Do you have any cold, flu or COVID-19 symptoms? b. In the last 14 days have you been in close contact with anyone who has had COVID-19 or COVID- 19-like symptoms? c. In the last 10 days have you tested positive or are you awaiting results of a COVID-19 test? B. If a person meets the temperature and question requirements, but does not have a mask, one will be provided. C. People are asked to use hand sanitizer upon entry to the building. There is an automatic hand sanitizer stand in the narthex. D. Once in the sanctuary, people may sit by household or ‘pods’ in physically distanced pews. Bulletins are in each pew. Worshipers are asked to take bulletins with them and either deposit in the recycling bin on their way out or to bring them home. E. The worship service will be modified to limit time, congregational responses, and singing.
Recommended publications
  • 166 AEOLIAN PROCESSES in PROCTOR CRATER on MARS: 2. MESOSCALE MODELING of DUNE-FORMING WINDS Lori K. Fenton and Mark I. Richards
    166 Chapter 4 AEOLIAN PROCESSES IN PROCTOR CRATER ON MARS: 2. MESOSCALE MODELING OF DUNE-FORMING WINDS Lori K. Fenton and Mark I. Richardson Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California Anthony D. Toigo Center for Radiophysics and Space Research, Cornell University, Ithaca, New York Abstract. Both atmospheric modeling and spacecraft imagery of Mars are now of sufficient quality that the two can be used in conjunction to acquire an understanding of regional- and local-scale aeolian processes on Mars. We apply a mesoscale atmospheric model adapted for use on Mars to Proctor Crater, a 150 km diameter crater in the southern highlands. Proctor Crater contains numerous aeolian features that indicate wind direction, including a large dark dunefield with reversing transverse and star dunes containing three different slipface orientations, small and older bright duneforms that are most likely transverse granule ripples, and seasonally erased dust devil tracks. Results from model runs spanning an entire year with a horizontal grid spacing of 10 km predict winds aligned with two of the three dune slipfaces as well as spring and summer winds matching the dust devil track orientations. The primary (most prevalent) dune slipface direction corresponds to a fall and winter westerly wind created by geostrophic forces. The tertiary dune slipface direction is caused by spring and summer evening katabatic flows down the eastern rim of the crater, influencing only the eastern portion of the crater floor. The dunes are trapped in 167 the crater because the tertiary winds, enhanced by topography, counter transport from the oppositely oriented primary winds, which originally carried sand into the crater.
    [Show full text]
  • Imagining Outer Space Also by Alexander C
    Imagining Outer Space Also by Alexander C. T. Geppert FLEETING CITIES Imperial Expositions in Fin-de-Siècle Europe Co-Edited EUROPEAN EGO-HISTORIES Historiography and the Self, 1970–2000 ORTE DES OKKULTEN ESPOSIZIONI IN EUROPA TRA OTTO E NOVECENTO Spazi, organizzazione, rappresentazioni ORTSGESPRÄCHE Raum und Kommunikation im 19. und 20. Jahrhundert NEW DANGEROUS LIAISONS Discourses on Europe and Love in the Twentieth Century WUNDER Poetik und Politik des Staunens im 20. Jahrhundert Imagining Outer Space European Astroculture in the Twentieth Century Edited by Alexander C. T. Geppert Emmy Noether Research Group Director Freie Universität Berlin Editorial matter, selection and introduction © Alexander C. T. Geppert 2012 Chapter 6 (by Michael J. Neufeld) © the Smithsonian Institution 2012 All remaining chapters © their respective authors 2012 All rights reserved. No reproduction, copy or transmission of this publication may be made without written permission. No portion of this publication may be reproduced, copied or transmitted save with written permission or in accordance with the provisions of the Copyright, Designs and Patents Act 1988, or under the terms of any licence permitting limited copying issued by the Copyright Licensing Agency, Saffron House, 6–10 Kirby Street, London EC1N 8TS. Any person who does any unauthorized act in relation to this publication may be liable to criminal prosecution and civil claims for damages. The authors have asserted their rights to be identified as the authors of this work in accordance with the Copyright, Designs and Patents Act 1988. First published 2012 by PALGRAVE MACMILLAN Palgrave Macmillan in the UK is an imprint of Macmillan Publishers Limited, registered in England, company number 785998, of Houndmills, Basingstoke, Hampshire RG21 6XS.
    [Show full text]
  • 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.
    [Show full text]
  • Widespread Crater-Related Pitted Materials on Mars: Further Evidence for the Role of Target Volatiles During the Impact Process ⇑ Livio L
    Icarus 220 (2012) 348–368 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Widespread crater-related pitted materials on Mars: Further evidence for the role of target volatiles during the impact process ⇑ Livio L. Tornabene a, , Gordon R. Osinski a, Alfred S. McEwen b, Joseph M. Boyce c, Veronica J. Bray b, Christy M. Caudill b, John A. Grant d, Christopher W. Hamilton e, Sarah Mattson b, Peter J. Mouginis-Mark c a University of Western Ontario, Centre for Planetary Science and Exploration, Earth Sciences, London, ON, Canada N6A 5B7 b University of Arizona, Lunar and Planetary Lab, Tucson, AZ 85721-0092, USA c University of Hawai’i, Hawai’i Institute of Geophysics and Planetology, Ma¯noa, HI 96822, USA d Smithsonian Institution, Center for Earth and Planetary Studies, Washington, DC 20013-7012, USA e NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA article info abstract Article history: Recently acquired high-resolution images of martian impact craters provide further evidence for the Received 28 August 2011 interaction between subsurface volatiles and the impact cratering process. A densely pitted crater-related Revised 29 April 2012 unit has been identified in images of 204 craters from the Mars Reconnaissance Orbiter. This sample of Accepted 9 May 2012 craters are nearly equally distributed between the two hemispheres, spanning from 53°Sto62°N latitude. Available online 24 May 2012 They range in diameter from 1 to 150 km, and are found at elevations between À5.5 to +5.2 km relative to the martian datum. The pits are polygonal to quasi-circular depressions that often occur in dense clus- Keywords: ters and range in size from 10 m to as large as 3 km.
    [Show full text]
  • Recent Channel Systems Emanating from Hale Crater Ejecta: Implications for the Noachian Landscape Evolution of Mars
    Lunar and Planetary Science XXXIX (2008) 2180.pdf RECENT CHANNEL SYSTEMS EMANATING FROM HALE CRATER EJECTA: IMPLICATIONS FOR THE NOACHIAN LANDSCAPE EVOLUTION OF MARS. L. L. Tornabene1, 2, A. S. McEwen1, and the HiRISE Team1, 1Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, [email protected] Introduction: Impact cratering is a fundamental into linear elements that do not appear to be typical crater geologic process that dominated the distant geologic past rays, but like rays lie radial to Hale (e.g., 315°E, 32°S; of the terrestrial planets. Thereby, impacts played a 323.6°E, 35.7°S). Further, Hale has pristine morphologic significant role in the formation and evolution of planetary features at the decameter scale such as a sharp but crusts in the form of impact effects and byproducts (e.g., complexly terraced rim, a prominent central peak and only ejecta, breccias, impact melts, etc.). On Mars, impacts may small (<1 km) and few superimposed craters. The ejecta have liberated subsurface volatiles that, in the form of and secondaries from Hale are superimposed over liquid water, modified both surface morphology and surrounding terrains covering a large expanse of Mars, composition (e.g., phyllosilicates [e.g., 1]), and possibly with one swath of secondaries spanning >500 km wide. influenced early habitable environments. Although such an Hale also possesses ponded materials and channelized interaction has been inferred by studies of crater flows, which is an indication of the presence of impact- morphology [e.g., 2] and impact models [e.g., 3], direct melt bearing materials, as well as a testament to the evidence for the release of liquid water or other volatiles youthfulness and excellent state of preservation of the by Martian impacts was lacking [4].
    [Show full text]
  • Crater Geometry and Ejecta Thickness of the Martian Impact Crater Tooting
    Meteoritics & Planetary Science 42, Nr 9, 1615–1625 (2007) Abstract available online at http://meteoritics.org Crater geometry and ejecta thickness of the Martian impact crater Tooting Peter J. MOUGINIS-MARK and Harold GARBEIL Hawai‘i Institute of Geophysics and Planetology, University of Hawai‘i, Honolulu, Hawai‘i 96822, USA (Received 25 October 2006; revision accepted 04 March 2007) Abstract–We use Mars Orbiter Laser Altimeter (MOLA) topographic data and Thermal Emission Imaging System (THEMIS) visible (VIS) images to study the cavity and the ejecta blanket of a very fresh Martian impact crater ~29 km in diameter, with the provisional International Astronomical Union (IAU) name Tooting crater. This crater is very young, as demonstrated by the large depth/ diameter ratio (0.065), impact melt preserved on the walls and floor, an extensive secondary crater field, and only 13 superposed impact craters (all 54 to 234 meters in diameter) on the ~8120 km2 ejecta blanket. Because the pre-impact terrain was essentially flat, we can measure the volume of the crater cavity and ejecta deposits. Tooting crater has a rim height that has >500 m variation around the rim crest and a very large central peak (1052 m high and >9 km wide). Crater cavity volume (i.e., volume below the pre-impact terrain) is ~380 km3 and the volume of materials above the pre-impact terrain is ~425 km3. The ejecta thickness is often very thin (<20 m) throughout much of the ejecta blanket. There is a pronounced asymmetry in the ejecta blanket, suggestive of an oblique impact, which has resulted in up to ~100 m of additional ejecta thickness being deposited down-range compared to the up-range value at the same radial distance from the rim crest.
    [Show full text]
  • Seasonal Movement of Material on Dunes in Proctor Crater, Mars: Possible Present-Day Sand Saltation
    Lunar and Planetary Science XXXVI (2005) 2169.pdf SEASONAL MOVEMENT OF MATERIAL ON DUNES IN PROCTOR CRATER, MARS: POSSIBLE PRESENT-DAY SAND SALTATION. L. K. Fenton, Arizona State University (Mars Space Flight Facility, Mail Code 6305, Tempe, AZ, 85287, [email protected]). Introduction: Much of the martian surface is cov- inspection reveals another set of slipfaces on the north- ered with dune fields, ventifacts, yardangs, and other eastern sides of the dunes (see esp. Fig. 2a). This is a aeolian features that require sand saltation to form morphology not observed in terrestrial dunes, where [e.g., 1]. However, there is little evidence for present- oppositely oriented slipfaces lead to reversing trans- day sand saltation. Images of dunes since the Viking verse dunes [6,7]. It is possible that the martian dunes mission and during the Mars Global Surveyor (MGS) are somewhat indurated (providing resistance to wind mission show no visible dune migration [1,2]. Lander erosion), preventing each slipface from being erased experiments rarely, if ever, measure winds strong by opposing winds. enough to saltate sand [3,4]. Yet, MOC NA (Mars Finding the bright material becomes a study in dis- Orbiter Camera Narrow Angle) images of sand dunes criminating between surfaces that have a higher albedo show sharp, uneroded crests [e.g., 1], suggesting that from those that are lit by sunlight. Figure 2a shows these dunes may still be active. mid-fall (possibly frosted) dune surfaces with apparent Investigation of MOC NA images of an intercrater bright material on the northeast slopes. Figure 2b dune field has led to the discovery of possible evi- shows an overlapping image from the following year dence for dune activity and sand saltation during the during the late spring, with fully defrosted dune sur- MGS mission.
    [Show full text]
  • In Pdf Format
    lós 1877 Mik 88 ge N 18 e N i h 80° 80° 80° ll T 80° re ly a o ndae ma p k Pl m os U has ia n anum Boreu bal e C h o A al m re u c K e o re S O a B Bo l y m p i a U n d Planum Es co e ria a l H y n d s p e U 60° e 60° 60° r b o r e a e 60° l l o C MARS · Korolev a i PHOTOMAP d n a c S Lomono a sov i T a t n M 1:320 000 000 i t V s a Per V s n a s l i l epe a s l i t i t a s B o r e a R u 1 cm = 320 km lkin t i t a s B o r e a a A a A l v s l i F e c b a P u o ss i North a s North s Fo d V s a a F s i e i c a a t ssa l vi o l eo Fo i p l ko R e e r e a o an u s a p t il b s em Stokes M ic s T M T P l Kunowski U 40° on a a 40° 40° a n T 40° e n i O Va a t i a LY VI 19 ll ic KI 76 es a As N M curi N G– ra ras- s Planum Acidalia Colles ier 2 + te .
    [Show full text]
  • This Article Appeared in a Journal Published by Elsevier. the Attached
    (This is a sample cover image for this issue. The actual cover is not yet available at this time.) This article appeared in a journal published by Elsevier. The attached copy is furnished to the author for internal non-commercial research and education use, including for instruction at the authors institution and sharing with colleagues. Other uses, including reproduction and distribution, or selling or licensing copies, or posting to personal, institutional or third party websites are prohibited. In most cases authors are permitted to post their version of the article (e.g. in Word or Tex form) to their personal website or institutional repository. Authors requiring further information regarding Elsevier’s archiving and manuscript policies are encouraged to visit: http://www.elsevier.com/copyright Author's personal copy Aeolian Research 8 (2013) 29–38 Contents lists available at SciVerse ScienceDirect Aeolian Research journal homepage: www.elsevier.com/locate/aeolia Review Article Summary of the Third International Planetary Dunes Workshop: Remote Sensing and Image Analysis of Planetary Dunes, Flagstaff, Arizona, USA, June 12–15, 2012 ⇑ Lori K. Fenton a, , Rosalyn K. Hayward b, Briony H.N. Horgan c, David M. Rubin d, Timothy N. Titus b, Mark A. Bishop e,f, Devon M. Burr g, Matthew Chojnacki g, Cynthia L. Dinwiddie h, Laura Kerber i, Alice Le Gall j, Timothy I. Michaels a, Lynn D.V. Neakrase k, Claire E. Newman l, Daniela Tirsch m, Hezi Yizhaq n, James R. Zimbelman o a Carl Sagan Center at the SETI Institute, 189 Bernardo Ave., Suite 100, Mountain View, CA 94043, USA b United States Geological Survey, Astrogeology Science Center, 2255 N.
    [Show full text]
  • Abstracts of the Annual Meeting of Planetary Geologic Mappers, Flagstaff, AZ 2014
    Abstracts of the Annual Meeting of Planetary Geologic Mappers, Flagstaff, AZ 2014 Edited by: James A. Skinner, Jr. U. S. Geological Survey, Flagstaff, AZ David Williams Arizona State University, Tempe, AZ NOTE: Abstracts in this volume can be cited using the following format: Graupner, M. and Hansen, V.L., 2014, Structural and Geologic Mapping of Tellus Region, Venus, in Skinner, J. A., Jr. and Williams, D. A., eds., Abstracts of the Annual Meeting of Planetary Geologic Mappers, Flagstaff, AZ, June 23-25, 2014. SCHEDULE OF EVENTS Monday, June 23– Planetary Geologic Mappers Meeting Time Planet/Body Topic 8:30 am Arrive/Set-up – 2255 N. Gemini Drive (USGS) 9:00 Welcome/Logistics 9:10 NASA HQ and Program Remarks (M. Kelley) 9:30 USGS Map Coordinator Remarks (J. Skinner) 9:45 GIS and Web Updates (C. Fortezzo) 10:00 RPIF Updates (J. Hagerty) 10:15 BREAK / POSTERS 10:40 Venus Irnini Mons (D. Buczkowski) 11:00 Moon Lunar South Pole (S. Mest) 11:20 Moon Copernicus Quad (J. Hagerty) 11:40 Vesta Iterative Geologic Mapping (A. Yingst) 12:00 pm LUNCH / POSTERS 1:30 Vesta Proposed Time-Stratigraphy (D. Williams) 1:50 Mars Global Geology (J. Skinner) 2:10 Mars Terra Sirenum (R. Anderson) 2:30 Mars Arsia/Pavonis Montes (B. Garry) 2:50 Mars Valles Marineris (C. Fortezzo) 3:10 BREAK / POSTERS 3:30 Mars Candor Chasma (C. Okubo) 3:50 Mars Hrad Vallis (P. Mouginis-Mark) 4:10 Mars S. Margaritifer Terra (J. Grant) 4:30 Mars Ladon basin (C. Weitz) 4:50 DISCUSSION / POSTERS ~5:15 ADJOURN Tuesday, June 24 - Planetary Geologic Mappers Meeting Time Planet/Body Topic 8:30 am Arrive/Set-up/Logistics 9:00 Mars Upper Dao and Niger Valles (S.
    [Show full text]
  • 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.
    [Show full text]
  • Bedform Migration on Mars: Current Results and Future Plans
    Aeolian Research xxx (2013) xxx–xxx Contents lists available at SciVerse ScienceDirect Aeolian Research journal homepage: www.elsevier.com/locate/aeolia Review Article Bedform migration on Mars: Current results and future plans ⇑ Nathan Bridges a, , Paul Geissler b, Simone Silvestro c, Maria Banks d a Johns Hopkins University, Applied Physics Laboratory, 200-W230, 11100 Johns Hopkins Road, Laurel, MD 20723, USA b US Geological Survey, Astrogeology Science Center, 2255 N. Gemini Drive, Flagstaff, AZ 86001-1698, USA c SETI Institute, 189 Bernardo Ave., Suite 100, Mountain View, CA 94043, USA d Center for Earth and Planetary Studies, Smithsonian National Air and Space Museum, Washington, DC 20013-7012, USA article info abstract Article history: With the advent of high resolution imaging, bedform motion can now be tracked on the Martian surface. Received 30 July 2012 HiRISE data, with a pixel scale as fine as 25 cm, shows displacements of sand patches, dunes, and ripples Revised 19 February 2013 up to several meters per Earth year, demonstrating that significant landscape modification occurs in the Accepted 19 February 2013 current environment. This seems to consistently occur in the north polar erg, with variable activity at Available online xxxx other latitudes. Volumetric dune and ripple changes indicate sand fluxes up to several cubic meters per meter per year, similar to that found in some dune fields on Earth. All ‘‘transverse aeolian ridges’’ Keywords: are immobile. There is no relationship between bedform activity and coarse-scale global circulation mod- Mars els, indicating that finer scale topography and wind gusts, combined with the predicted low impact Dunes Ripples threshold on Mars, are the primary drivers.
    [Show full text]