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Astro2020 APC White Papers the Navy Precision Optical Interferometer
Astro2020 APC White Papers The Navy Precision Optical Interferometer Type of Activity: Ground Based Project Space Based Project Infrastructure Activity 4 Technological Development Activity State of the Professions Consideration4 Other Principal Author: Name: Gerard van Belle Institution: Lowell Observatory Email: [email protected] Phone: 928-255-7865 Co-authors: (names, institutions, emails) J. Thomas Armstrong (NRL, [email protected]), Ellyn Baines (NRL, [email protected]), Joe Llama (Lowell, [email protected]), Henrique Schmitt (NRL, [email protected]) Abstract: The Navy Precision Optical Interferometer (NPOI) is one of the premier U.S. long-baseline optical interferometric facilities, capable of providing sub-milliarcsecond imaging in the visible. We outline a plan for NPOI for 2020-2030 that will cement its leadership as the highest resolution optical system on the planet, with multi-kilometer baselines. This capability will serve a wide variety of Astro2020 science needs, resolving the sizes and shapes of stars, resolving AGNs, imaging protoplanetary disks, and observing the passage of exoplanets across their stellar disks. 1 1 Introduction The Navy Precision Optical Interferometer (NPOI), a long baseline optical interferometer located on Anderson Mesa, near Flagstaff, Arizona, is operated as a partnership between Lowell Observatory, the Naval Research Laboratory (NRL), and the US Naval Observatory (USNO). It features a Y-shaped layout with 250 m arms, telescopes that can be moved among 30 stations along the arms, visible-band beam combiners, and a vacuum feed system to avoid ground seeing and differential longitudinal dispersion. NPOI currently operates with up to six telescopes simultaneously feeding the beam combination laboratory with 12-cm effective apertures, on baselines (separations between the apertures) up to 98-m. -
What Is the Color of Pluto? - Universe Today
What is the Color of Pluto? - Universe Today space and astronomy news Universe Today Home Members Guide to Space Carnival Photos Videos Forum Contact Privacy Login NASA’s New Horizons spacecraft captured this high-resolution enhanced color view of http://www.universetoday.com/13866/color-of-pluto/[29-Mar-17 13:18:37] What is the Color of Pluto? - Universe Today Pluto on July 14, 2015. Credit: NASA/JHUAPL/SwRI WHAT IS THE COLOR OF PLUTO? Article Updated: 28 Mar , 2017 by Matt Williams When Pluto was first discovered by Clybe Tombaugh in 1930, astronomers believed that they had found the ninth and outermost planet of the Solar System. In the decades that followed, what little we were able to learn about this distant world was the product of surveys conducted using Earth-based telescopes. Throughout this period, astronomers believed that Pluto was a dirty brown color. In recent years, thanks to improved observations and the New Horizons mission, we have finally managed to obtain a clear picture of what Pluto looks like. In addition to information about its surface features, composition and tenuous atmosphere, much has been learned about Pluto’s appearance. Because of this, we now know that the one-time “ninth planet” of the Solar System is rich and varied in color. Composition: With a mean density of 1.87 g/cm3, Pluto’s composition is differentiated between an icy mantle and a rocky core. The surface is composed of more than 98% nitrogen ice, with traces of methane and carbon monoxide. Scientists also suspect that Pluto’s internal structure is differentiated, with the rocky material having settled into a dense core surrounded by a mantle of water ice. -
Jjmonl 1710.Pmd
alactic Observer John J. McCarthy Observatory G Volume 10, No. 10 October 2017 The Last Waltz Cassini’s final mission and dance of death with Saturn more on page 4 and 20 The John J. McCarthy Observatory Galactic Observer New Milford High School Editorial Committee 388 Danbury Road Managing Editor New Milford, CT 06776 Bill Cloutier Phone/Voice: (860) 210-4117 Production & Design Phone/Fax: (860) 354-1595 www.mccarthyobservatory.org Allan Ostergren Website Development JJMO Staff Marc Polansky Technical Support It is through their efforts that the McCarthy Observatory Bob Lambert has established itself as a significant educational and recreational resource within the western Connecticut Dr. Parker Moreland community. Steve Barone Jim Johnstone Colin Campbell Carly KleinStern Dennis Cartolano Bob Lambert Route Mike Chiarella Roger Moore Jeff Chodak Parker Moreland, PhD Bill Cloutier Allan Ostergren Doug Delisle Marc Polansky Cecilia Detrich Joe Privitera Dirk Feather Monty Robson Randy Fender Don Ross Louise Gagnon Gene Schilling John Gebauer Katie Shusdock Elaine Green Paul Woodell Tina Hartzell Amy Ziffer In This Issue INTERNATIONAL OBSERVE THE MOON NIGHT ...................... 4 SOLAR ACTIVITY ........................................................... 19 MONTE APENNINES AND APOLLO 15 .................................. 5 COMMONLY USED TERMS ............................................... 19 FAREWELL TO RING WORLD ............................................ 5 FRONT PAGE ............................................................... -
Orbital Evidence for More Widespread Carbonate- 10.1002/2015JE004972 Bearing Rocks on Mars Key Point: James J
PUBLICATIONS Journal of Geophysical Research: Planets RESEARCH ARTICLE Orbital evidence for more widespread carbonate- 10.1002/2015JE004972 bearing rocks on Mars Key Point: James J. Wray1, Scott L. Murchie2, Janice L. Bishop3, Bethany L. Ehlmann4, Ralph E. Milliken5, • Carbonates coexist with phyllosili- 1 2 6 cates in exhumed Noachian rocks in Mary Beth Wilhelm , Kimberly D. Seelos , and Matthew Chojnacki several regions of Mars 1School of Earth and Atmospheric Sciences, Georgia Institute of Technology, Atlanta, Georgia, USA, 2The Johns Hopkins University/Applied Physics Laboratory, Laurel, Maryland, USA, 3SETI Institute, Mountain View, California, USA, 4Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, California, USA, 5Department of Geological Sciences, Brown Correspondence to: University, Providence, Rhode Island, USA, 6Lunar and Planetary Laboratory, University of Arizona, Tucson, Arizona, USA J. J. Wray, [email protected] Abstract Carbonates are key minerals for understanding ancient Martian environments because they Citation: are indicators of potentially habitable, neutral-to-alkaline water and may be an important reservoir for Wray, J. J., S. L. Murchie, J. L. Bishop, paleoatmospheric CO2. Previous remote sensing studies have identified mostly Mg-rich carbonates, both in B. L. Ehlmann, R. E. Milliken, M. B. Wilhelm, Martian dust and in a Late Noachian rock unit circumferential to the Isidis basin. Here we report evidence for older K. D. Seelos, and M. Chojnacki (2016), Orbital evidence for more widespread Fe- and/or Ca-rich carbonates exposed from the subsurface by impact craters and troughs. These carbonates carbonate-bearing rocks on Mars, are found in and around the Huygens basin northwest of Hellas, in western Noachis Terra between the Argyre – J. -
Bio-Preservation Potential of Sediment in Eberswalde Crater, Mars
Western Washington University Western CEDAR WWU Graduate School Collection WWU Graduate and Undergraduate Scholarship Fall 2020 Bio-preservation Potential of Sediment in Eberswalde crater, Mars Cory Hughes Western Washington University, [email protected] Follow this and additional works at: https://cedar.wwu.edu/wwuet Part of the Geology Commons Recommended Citation Hughes, Cory, "Bio-preservation Potential of Sediment in Eberswalde crater, Mars" (2020). WWU Graduate School Collection. 992. https://cedar.wwu.edu/wwuet/992 This Masters Thesis is brought to you for free and open access by the WWU Graduate and Undergraduate Scholarship at Western CEDAR. It has been accepted for inclusion in WWU Graduate School Collection by an authorized administrator of Western CEDAR. For more information, please contact [email protected]. Bio-preservation Potential of Sediment in Eberswalde crater, Mars By Cory M. Hughes Accepted in Partial Completion of the Requirements for the Degree Master of Science ADVISORY COMMITTEE Dr. Melissa Rice, Chair Dr. Charles Barnhart Dr. Brady Foreman Dr. Allison Pfeiffer GRADUATE SCHOOL David L. Patrick, Dean Master’s Thesis In presenting this thesis in partial fulfillment of the requirements for a master’s degree at Western Washington University, I grant to Western Washington University the non-exclusive royalty-free right to archive, reproduce, distribute, and display the thesis in any and all forms, including electronic format, via any digital library mechanisms maintained by WWU. I represent and warrant this is my original work, and does not infringe or violate any rights of others. I warrant that I have obtained written permissions from the owner of any third party copyrighted material included in these files. -
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 -
Indigenous Astronomies and Progress in Modern Astronomy
Indigenous Astronomies and Progress in Modern Astronomy Clive Ruggles1 School of Archaeology and Ancient History, University of Leicester University Road, LEICESTER LE1 7RH, U.K. E-mail: [email protected] From an anthropological point of view, the whole concept of a ‘path of progress’ in astronomical discovery is anathema, since it implicitly downgrades other cultural perspectives, such as the many ‘indigenous cosmologies’ that still exist in the modern world. By doing so, one risks provoking those who hold them and—as is most obvious in places such as Hawaii where the two ‘world-views’ come into direct contact—creating avoidable resistance to that very progress. The problem is complicated by the existence of ‘fringe’ and ‘new-age’ views that are increasingly confused with, and even passed off as, indigenous perceptions. In a modern world where widespread public perceptions include many that are unscientific in the broadest sense of the term, I shall argue that there are actually a range of positive benefits for progress in scientific astronomy to be derived from the mutual awareness and comprehension of ‘genuine’ cultural world-views whose goals—in common with those of modern science—are to make sense of the cosmos within which people live. While two-way education is clearly a prerequisite, I shall argue that the necessary level of reconciliation can only be achieved through more fundamental attempts by modern astronomers to understand, and ultimately to respect, both the non-Western frameworks of thought that give rise to other cultural perspectives and the heritage associated with them. One of the most obvious potential benefits could derive from common attitudes towards the natural heritage of astronomy, namely dark skies. -
A Tale of Two Sides: Pluto's Opposition Surge in 2018 and 2019
EPSC Abstracts Vol. 14, EPSC2020-546, 2020, updated on 27 Sep 2021 https://doi.org/10.5194/epsc2020-546 Europlanet Science Congress 2020 © Author(s) 2021. This work is distributed under the Creative Commons Attribution 4.0 License. A Tale of Two Sides: Pluto's Opposition Surge in 2018 and 2019 Anne Verbiscer1, Paul Helfenstein2, Mark Showalter3, and Marc Buie4 1University of Virginia, Charlottesville, VA, USA ([email protected]) 2Cornell University, Ithaca, NY, USA ([email protected]) 3SETI Institute, Mountain View, CA, USA ([email protected]) 4Southwest Research Institute, Boulder, CO, USA ([email protected]) Near-opposition photometry employs remote sensing observations to reveal the microphysical properties of regolith-covered surfaces over a wide range of solar system bodies. When aligned directly opposite the Sun, objects exhibit an opposition effect, or surge, a dramatic, non-linear increase in reflectance seen with decreasing solar phase angle (the Sun-target-observer angle). This phenomenon is a consequence of both interparticle shadow hiding and a constructive interference phenomenon known as coherent backscatter [1-3]. While the size of the Earth’s orbit restricts observations of Pluto and its moons to solar phase angles no larger than α = 1.9°, the opposition surge, which occurs largely at α < 1°, can discriminate surface properties [4-6]. The smallest solar phase angles are attainable at node crossings when the Earth transits the solar disk as viewed from the object. In this configuration, a solar system body is at “true” opposition. When combined with observations acquired at larger phase angles, the resulting reflectance measurement can be related to the optical, structural, and thermal properties of the regolith and its inferred collisional history. -
Pluto's Far Side
Pluto’s Far Side S.A. Stern Southwest Research Institute O.L. White SETI Institute P.J. McGovern Lunar and Planetary Institute J.T. Keane California Institute of Technology J.W. Conrad, C.J. Bierson University of California, Santa Cruz C.B. Olkin Southwest Research Institute P.M. Schenk Lunar and Planetary Institute J.M. Moore NASA Ames Research Center K.D. Runyon Johns Hopkins University, Applied Physics Laboratory and The New Horizons Team 1 Abstract The New Horizons spacecraft provided near-global observations of Pluto that far exceed the resolution of Earth-based datasets. Most Pluto New Horizons analysis hitherto has focused on Pluto’s encounter hemisphere (i.e., the anti-Charon hemisphere containing Sputnik Planitia). In this work, we summarize and interpret data on Pluto’s “far side” (i.e., the non-encounter hemisphere), providing the first integrated New Horizons overview of Pluto’s far side terrains. We find strong evidence for widespread bladed deposits, evidence for an impact crater about as large as any on the “near side” hemisphere, evidence for complex lineations approximately antipodal to Sputnik Planitia that may be causally related, and evidence that the far side maculae are smaller and more structured than Pluto’s encounter hemisphere maculae. 2 Introduction Before the 2015 exploration of Pluto by New Horizons (e.g., Stern et al. 2015, 2018 and references therein) none of Pluto’s surface features were known except by crude (though heroically derived) albedo maps, with resolutions of 300-500 km obtainable from the Hubble Space Telescope (e.g., Buie et al. 1992, 1997, 2010) and Pluto-Charon mutual event techniques (e.g., Young & Binzel 1993, Young et al. -
Pluto's Atmosphere Dynamics: How the Nitrogen Heart Regulates The
Pluto System After New Horizons 2019 (LPI Contrib. No. 2133) 7017.pdf PLUTO’S ATMOSPHERE DYNAMICS: HOW THE NITROGEN HEART REGULATES THE CIRCULATION. T. Bertrand1, F. Forget2, A. Toigo3, D. Hinson4,5, 1Space Science Division, NASA Ames Re- search Center Moffett Field, CA 94035, USA ([email protected]), 2Laboratoire de Météorologie Dy- namique, IPSL, CNRS, Sorbonne Université, Paris, France ([email protected]), 3Johns Hopkins University Ap- plied Physics Laboratory, Laurel, MD 20723, United States ([email protected]), 4Carl Sagan Center, SETI Institute, Mountain View, CA 94043, USA,5Department of Electrical Engineering, Stanford University, Stanford, CA 94305, USA ([email protected]) Introduction: Pluto’s tenuous atmosphere is main- many Pluto years in order to be insensitive to the initial ly nitrogen and is in solid-gas equilibrium with the sur- state, which requires significant computing time. To face nitrogen ice [1]. Over the past three decades, solve this issue, a volatile transport model of Pluto is Earth-based stellar occultations have been an effective used to create initial states for the GCM which are the method to study the evolution of its temperature, com- results of 30 million years of volatile ice evolution and position, pressure, and density [e.g. 2-7]. In particular, contain equilibrated combinations of surface condi- these datasets revealed (1) a much warmer atmosphere tions, such as soil temperatures and ice distributions (70-100 K) than the surface (40 K), with a strong in- [23]. This approach enables 3D GCM simulations of version in the first 20 km above the surface, (2) a three- Pluto to be performed typically from 1984 to 2015, the fold increase of surface pressure since 1988, and (3) first 20 years corresponding to a spin-up time for the global-scale oscillations in the vertical density and atmosphere. -
The Astronomy of Many Cultures: a Resource Guide
The Astronomy of Many Cultures: A Resource Guide by Andrew Fraknoi (Fromm Institute, U. of San Francisco) Version 5.1; July 2020 © copyright 2020 by Andrew Fraknoi. The right to use or reproduce this guide for any nonprofit educational purpose is hereby granted. For permission to use in other ways, or to suggest additional materials, please contact the author at e-mail: fraknoi {at} fhda {dot} edu The teaching of astronomy in our colleges and high schools often sidesteps the contributions of cultures outside of Europe and the U.S. white mainstream. Few educators (formal or informal) receive much training in this area, and they therefore tend to stick to people and histories they know from their own training -- even when an increasing number of their students or audiences might be from cultures beyond those familiar to them. Luckily, a wealth of material is becoming available to help celebrate the ideas and contributions of non-European cultures regarding our views of the universe. This listing of resources about cultures and astronomy makes no claim to be comprehensive, but simply consists of some English-language materials that can be used both by educators and their students or audiences. We include published and web-based materials, plus videos and classroom activities. In this edition, we have made a particular effort to enlarge resources about African-American and Hispanic American astronomers. Note that there’s a separate listing about the role of women in astronomy at: http://bit.ly/astronomywomen Table of Contents: 1. General Resources on the Astronomy of Diverse Cultures 2. -
April Meeting with Jack Szelka & Dave Huestis
the vol. 37 no. 4 April Skyscraper 2010 Amateur Astronomical Society of Rhode Island 47 Peeptoad Road North Scituate, Rhode Island 02857 www.theSkyscrapers.org Seagrave Memorial Observatory is open April Meeting to the public weather permitting with Jack Szelka & Dave Huestis Saturdays 8pm - 10pm Please note that the observatory may be inac- Friday, April 2, 7:30pm cessible for several weeks following a winter North Scituate Community Center storm. See web site for updates. The Skyscrapers' Monthly Meeting on April 2, 2010 at the Scituate Community Center will feature two talks by Skyscrapers' members Dave Huestis and Jack Szelka. North Scituate Community Center Yerkes Observatory and Adler Planetarium by Jack Szelka All of our winter meetings (Dec-April) are held at the Community Center. From Seagrave Member Jack Szelka will present a Also presented, a tour of the Yerkes Observatory, the Community Center is the first Powerpoint presentation highlighting a visit Observatory including highlights of the building on the right side going south on Rt. to the Adler Planetarium in Chicago, Illinois buildings, equipment and history of the 116 after the intersection of Rt. 6 Bypass (also and Yerkes Observatory in Williams Bay, many great astronomers who have worked Rt. 101) and Rt. 116. Parking is across the street. Wisconsin. there. The main feature is the worlds largest He will cover some of the astronomical refractor, the 40-inch Alvan Clark lens and a exhibits at the Adler; the Telescope display, night of viewing with this scope. Atwood Sphere and the other astronomy In this issue… related displays. 2 President’s Message The Sesquicentennial Birthday of Frank Evans Seagrave (1860-1934) by Dave Huestis 2 Sirius Dave Huestis, a Skyscrapers member Skyscrapers purchased Frank’s observa- 3 Sesquicentennial Birthday of since 1975 and the society’s historian for tory and 8¼-inch Alvan Clark refractor Frank Evans Seagrave many years, will be presenting a talk to on Peeptoad Road back in 1936.