Pluto and the 'Planet Problem': Folk Concepts and Natural Kinds In
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Surface Characteristics of Transneptunian Objects and Centaurs from Photometry and Spectroscopy
Barucci et al.: Surface Characteristics of TNOs and Centaurs 647 Surface Characteristics of Transneptunian Objects and Centaurs from Photometry and Spectroscopy M. A. Barucci and A. Doressoundiram Observatoire de Paris D. P. Cruikshank NASA Ames Research Center The external region of the solar system contains a vast population of small icy bodies, be- lieved to be remnants from the accretion of the planets. The transneptunian objects (TNOs) and Centaurs (located between Jupiter and Neptune) are probably made of the most primitive and thermally unprocessed materials of the known solar system. Although the study of these objects has rapidly evolved in the past few years, especially from dynamical and theoretical points of view, studies of the physical and chemical properties of the TNO population are still limited by the faintness of these objects. The basic properties of these objects, including infor- mation on their dimensions and rotation periods, are presented, with emphasis on their diver- sity and the possible characteristics of their surfaces. 1. INTRODUCTION cally with even the largest telescopes. The physical char- acteristics of Centaurs and TNOs are still in a rather early Transneptunian objects (TNOs), also known as Kuiper stage of investigation. Advances in instrumentation on tele- belt objects (KBOs) and Edgeworth-Kuiper belt objects scopes of 6- to 10-m aperture have enabled spectroscopic (EKBOs), are presumed to be remnants of the solar nebula studies of an increasing number of these objects, and signifi- that have survived over the age of the solar system. The cant progress is slowly being made. connection of the short-period comets (P < 200 yr) of low We describe here photometric and spectroscopic studies orbital inclination and the transneptunian population of pri- of TNOs and the emerging results. -
Geological Timeline
Geological Timeline In this pack you will find information and activities to help your class grasp the concept of geological time, just how old our planet is, and just how young we, as a species, are. Planet Earth is 4,600 million years old. We all know this is very old indeed, but big numbers like this are always difficult to get your head around. The activities in this pack will help your class to make visual representations of the age of the Earth to help them get to grips with the timescales involved. Important EvEnts In thE Earth’s hIstory 4600 mya (million years ago) – Planet Earth formed. Dust left over from the birth of the sun clumped together to form planet Earth. The other planets in our solar system were also formed in this way at about the same time. 4500 mya – Earth’s core and crust formed. Dense metals sank to the centre of the Earth and formed the core, while the outside layer cooled and solidified to form the Earth’s crust. 4400 mya – The Earth’s first oceans formed. Water vapour was released into the Earth’s atmosphere by volcanism. It then cooled, fell back down as rain, and formed the Earth’s first oceans. Some water may also have been brought to Earth by comets and asteroids. 3850 mya – The first life appeared on Earth. It was very simple single-celled organisms. Exactly how life first arose is a mystery. 1500 mya – Oxygen began to accumulate in the Earth’s atmosphere. Oxygen is made by cyanobacteria (blue-green algae) as a product of photosynthesis. -
Modern Astronomical Optics - Observing Exoplanets 2
Modern Astronomical Optics - Observing Exoplanets 2. Brief Introduction to Exoplanets Olivier Guyon - [email protected] – Jim Burge, Phil Hinz WEBSITE: www.naoj.org/staff/guyon → Astronomical Optics Course » → Observing Exoplanets (2012) Definitions – types of exoplanets Planet (& exoplanet) definitions are recent, as, prior to discoveries of exoplanets around other stars and dwarf planets in our solar system, there was no need to discuss lower and upper limits of planet masses. Asteroid < dwarf planet < planet < brown dwarf < star Upper limit defined by its mass: < 13 Jupiter mass 1 Jupiter mass = 317 Earth mass = 1/1000 Sun mass Mass limit corresponds to deuterium limit: a planet is not sufficiently massive to start nuclear fusion reactions, of which deuterium burning is the easiest (lowest temperature) Lower limit recently defined (now excludes Pluto) for our solar system: has cleared the neighbourhood around its orbit Distinction between giant planets (massive, large, mostly gas) and rocky planets also applies to exoplanets Habitable planet: planet on which life as we know it (bacteria, planets or animals) could be sustained = rocky + surface temperature suitable for liquid water Formation Planet and stars form (nearly) together, within first few x10 Myr of system formation Gravitational collapse of gas + dust cloud Star is formed at center of disk Planets form in the protoplanetary disk Planet embrios form first Adaptive Optics image of Beta Pic Large embrios (> few Earth mass) can Shows planet + debris disk accrete large quantity of -
Introduction to Astronomy from Darkness to Blazing Glory
Introduction to Astronomy From Darkness to Blazing Glory Published by JAS Educational Publications Copyright Pending 2010 JAS Educational Publications All rights reserved. Including the right of reproduction in whole or in part in any form. Second Edition Author: Jeffrey Wright Scott Photographs and Diagrams: Credit NASA, Jet Propulsion Laboratory, USGS, NOAA, Aames Research Center JAS Educational Publications 2601 Oakdale Road, H2 P.O. Box 197 Modesto California 95355 1-888-586-6252 Website: http://.Introastro.com Printing by Minuteman Press, Berkley, California ISBN 978-0-9827200-0-4 1 Introduction to Astronomy From Darkness to Blazing Glory The moon Titan is in the forefront with the moon Tethys behind it. These are two of many of Saturn’s moons Credit: Cassini Imaging Team, ISS, JPL, ESA, NASA 2 Introduction to Astronomy Contents in Brief Chapter 1: Astronomy Basics: Pages 1 – 6 Workbook Pages 1 - 2 Chapter 2: Time: Pages 7 - 10 Workbook Pages 3 - 4 Chapter 3: Solar System Overview: Pages 11 - 14 Workbook Pages 5 - 8 Chapter 4: Our Sun: Pages 15 - 20 Workbook Pages 9 - 16 Chapter 5: The Terrestrial Planets: Page 21 - 39 Workbook Pages 17 - 36 Mercury: Pages 22 - 23 Venus: Pages 24 - 25 Earth: Pages 25 - 34 Mars: Pages 34 - 39 Chapter 6: Outer, Dwarf and Exoplanets Pages: 41-54 Workbook Pages 37 - 48 Jupiter: Pages 41 - 42 Saturn: Pages 42 - 44 Uranus: Pages 44 - 45 Neptune: Pages 45 - 46 Dwarf Planets, Plutoids and Exoplanets: Pages 47 -54 3 Chapter 7: The Moons: Pages: 55 - 66 Workbook Pages 49 - 56 Chapter 8: Rocks and Ice: -
Science in Nasa's Vision for Space Exploration
SCIENCE IN NASA’S VISION FOR SPACE EXPLORATION SCIENCE IN NASA’S VISION FOR SPACE EXPLORATION Committee on the Scientific Context for Space Exploration Space Studies Board Division on Engineering and Physical Sciences THE NATIONAL ACADEMIES PRESS Washington, D.C. www.nap.edu THE NATIONAL ACADEMIES PRESS 500 Fifth Street, N.W. Washington, DC 20001 NOTICE: The project that is the subject of this report was approved by the Governing Board of the National Research Council, whose members are drawn from the councils of the National Academy of Sciences, the National Academy of Engineering, and the Institute of Medicine. The members of the committee responsible for the report were chosen for their special competences and with regard for appropriate balance. Support for this project was provided by Contract NASW 01001 between the National Academy of Sciences and the National Aeronautics and Space Administration. Any opinions, findings, conclusions, or recommendations expressed in this material are those of the authors and do not necessarily reflect the views of the sponsors. International Standard Book Number 0-309-09593-X (Book) International Standard Book Number 0-309-54880-2 (PDF) Copies of this report are available free of charge from Space Studies Board National Research Council The Keck Center of the National Academies 500 Fifth Street, N.W. Washington, DC 20001 Additional copies of this report are available from the National Academies Press, 500 Fifth Street, N.W., Lockbox 285, Washington, DC 20055; (800) 624-6242 or (202) 334-3313 (in the Washington metropolitan area); Internet, http://www.nap.edu. Copyright 2005 by the National Academy of Sciences. -
An Overview of New Worlds, New Horizons in Astronomy and Astrophysics About the National Academies
2020 VISION An Overview of New Worlds, New Horizons in Astronomy and Astrophysics About the National Academies The National Academies—comprising the National Academy of Sciences, the National Academy of Engineering, the Institute of Medicine, and the National Research Council—work together to enlist the nation’s top scientists, engineers, health professionals, and other experts to study specific issues in science, technology, and medicine that underlie many questions of national importance. The results of their deliberations have inspired some of the nation’s most significant and lasting efforts to improve the health, education, and welfare of the United States and have provided independent advice on issues that affect people’s lives worldwide. To learn more about the Academies’ activities, check the website at www.nationalacademies.org. Copyright 2011 by the National Academy of Sciences. All rights reserved. Printed in the United States of America This study was supported by Contract NNX08AN97G between the National Academy of Sciences and the National Aeronautics and Space Administration, Contract AST-0743899 between the National Academy of Sciences and the National Science Foundation, and Contract DE-FG02-08ER41542 between the National Academy of Sciences and the U.S. Department of Energy. Support for this study was also provided by the Vesto Slipher Fund. Any opinions, findings, conclusions, or recommendations expressed in this publication are those of the authors and do not necessarily reflect the views of the agencies that provided support for the project. 2020 VISION An Overview of New Worlds, New Horizons in Astronomy and Astrophysics Committee for a Decadal Survey of Astronomy and Astrophysics ROGER D. -
Composition and Accretion of the Terrestrial Planets
Lunar and Planetary Science XXXI 1546.pdf COMPOSITION AND ACCRETION OF THE TERRESTRIAL PLANETS. Edward R. D. Scott and G. Jeffrey Taylor, Hawai’i Institute of Geophysics and Planetology, School of Ocean and Earth Science and Technology, Univer- sity of Hawai’i at Manoa, Honolulu, Hawai’i 96822, USA; [email protected] Abstract: Compositional variations among the spread gravitational mixing of the embryos and their four terrestrial planets are generally attributed to giant 20 impacts [1] rather than to primordial chemical varia- Fig. 2 tions among planetesimals [e.g., 2]. This is largely be- Mars cause modeling suggests that each terrestrial planet ac- 15 creted material from the whole of the inner solar sys- tem [1], and because Mercury’s high density is attrib- 10 Venus Earth uted to mantle stripping in a giant impact [3] and not to its position as the innermost planet [4]. However, Mer- Mercury cury’s high concentration of metallic iron and low con- 5 centration of oxidized iron are comparable to those in recently discovered metal-rich chondrites [5-7]. Since E 0 chondrites are linked isotopically with the Earth, we 0 0.5 1 1.5 2 suggest that Mercury may have formed from metal-rich chondritic material. Venus and Earth have similar con- Semi-major Axis (AU) centrations of metallic and oxidized iron that are inter- fragments, which ensured that each terrestrial planet mediate between those of Mercury and Mars consistent formed from material originally located throughout the with wide, overlapping accretion zones [1]. However, inner solar system (0.5 to 2.5 AU). -
POSSIBLE STRUCTURE MODELS for the TRANSITING SUPER-EARTHS:KEPLER-10B and 11B
43rd Lunar and Planetary Science Conference (2012) 1290.pdf POSSIBLE STRUCTURE MODELS FOR THE TRANSITING SUPER-EARTHS:KEPLER-10b AND 11b. P. Futó1 1 Department of Physical Geography, University of West Hungary, Szombathely, Károlyi Gáspár tér, H- 9700, Hungary ([email protected]) Introduction:Up to january of 2012,10 super- The planet Kepler-11b has a large radius (1.97 R⊕) for Earths have been announced by Kepler-mission [1] its mass (4.3 M⊕),therefore this planet must have a that is designed to detect hundreds of transiting exo- spherical shell that is composed of low-density materi- planets.Kepler was launched on 6th March,2009 and the als.Considering the planet's average density,it must primary purpose of its scientific program is to search have a metallic core with different possible fractional for terrestrial-sized planets in the habitable zone of mass.Accordinghly,I have made a possible structure Solar-like stars.For the case of high number of discov- model for Kepler-11b in which the selected core mass eries we will be able to estimate the frequency of fraction is 32.59% (similarly to that of Earth) and the Earth-sized planets in our galaxy.Results of the Kepler- water ice layer has a relatively great fractional 's measurements show that the small-sized planets are volume.For case of the selected composition, the icy frequent in the spiral galaxies.A catalog of planetary surface sublimated to form a water vapor as the planet candidates,including objects with small-sized candidate moved inward the central star during its migration. -
Exploration of the Kuiper Belt by High-Precision Photometric Stellar Occultations: First Results F
Exploration of the Kuiper Belt by High-Precision Photometric Stellar Occultations: First Results F. Roques, A. Doressoundiram, V. Dhillon, T. Marsh, S. Bickerton, J. J. Kavelaars, M. Moncuquet, M. Auvergne, I. Belskaya, M. Chevreton, et al. To cite this version: F. Roques, A. Doressoundiram, V. Dhillon, T. Marsh, S. Bickerton, et al.. Exploration of the Kuiper Belt by High-Precision Photometric Stellar Occultations: First Results. Astronomical Journal, Amer- ican Astronomical Society, 2006, 132, pp.819-822. 10.1086/505623. hal-00640050 HAL Id: hal-00640050 https://hal.archives-ouvertes.fr/hal-00640050 Submitted on 10 Nov 2011 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. The Astronomical Journal, 132:819Y822, 2006 August # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. EXPLORATION OF THE KUIPER BELT BY HIGH-PRECISION PHOTOMETRIC STELLAR OCCULTATIONS: FIRST RESULTS F. Roques,1,2 A. Doressoundiram,1 V. Dhillon,3 T. Marsh,4 S. Bickerton,5,6 J. J. Kavelaars,5 M. Moncuquet,1 M. Auvergne,1 I. Belskaya,7 M. Chevreton,1 F. Colas,1 A. Fernandez,1 A. Fitzsimmons,8 J. Lecacheux,1 O. Mousis,9 S. -
Constraints on the Spin Evolution of Young Planetary-Mass Companions Marta L
Constraints on the Spin Evolution of Young Planetary-Mass Companions Marta L. Bryan1, Björn Benneke2, Heather A. Knutson2, Konstantin Batygin2, Brendan P. Bowler3 1Cahill Center for Astronomy and Astrophysics, California Institute of Technology, 1200 East California Boulevard, MC 249-17, Pasadena, CA 91125, USA. 2Division of Geological and Planetary Sciences, California Institute of Technology, Pasadena, CA 91125, USA. 3McDonald Observatory and Department of Astronomy, University of Texas at Austin, Austin, TX 78712, USA. Surveys of young star-forming regions have discovered a growing population of planetary- 1 mass (<13 MJup) companions around young stars . There is an ongoing debate as to whether these companions formed like planets (that is, from the circumstellar disk)2, or if they represent the low-mass tail of the star formation process3. In this study we utilize high-resolution spectroscopy to measure rotation rates of three young (2-300 Myr) planetary-mass companions and combine these measurements with published rotation rates for two additional companions4,5 to provide a look at the spin distribution of these objects. We compare this distribution to complementary rotation rate measurements for six brown dwarfs with masses <20 MJup, and show that these distributions are indistinguishable. This suggests that either that these two populations formed via the same mechanism, or that processes regulating rotation rates are independent of formation mechanism. We find that rotation rates for both populations are well below their break-up velocities and do not evolve significantly during the first few hundred million years after the end of accretion. This suggests that rotation rates are set during late stages of accretion, possibly by interactions with a circumplanetary disk. -
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. -
Outer Planets: the Ice Giants
Outer Planets: The Ice Giants A. P. Ingersoll, H. B. Hammel, T. R. Spilker, R. E. Young Exploring Uranus and Neptune satisfies NASA’s objectives, “investigation of the Earth, Moon, Mars and beyond with emphasis on understanding the history of the solar system” and “conduct robotic exploration across the solar system for scientific purposes.” The giant planet story is the story of the solar system (*). Earth and the other small objects are leftovers from the feast of giant planet formation. As they formed, the giant planets may have migrated inward or outward, ejecting some objects from the solar system and swallowing others. The giant planets most likely delivered water and other volatiles, in the form of icy planetesimals, to the inner solar system from the region around Neptune. The “gas giants” Jupiter and Saturn are mostly hydrogen and helium. These planets must have swallowed a portion of the solar nebula intact. The “ice giants” Uranus and Neptune are made primarily of heavier stuff, probably the next most abundant elements in the Sun – oxygen, carbon, nitrogen, and sulfur. For each giant planet the core is the “seed” around which it accreted nebular gas. The ice giants may be more seed than gas. Giant planets are laboratories in which to test our theories about geophysics, plasma physics, meteorology, and even oceanography in a larger context. Their bottomless atmospheres, with 1000 mph winds and 100 year-old storms, teach us about weather on Earth. The giant planets’ enormous magnetic fields and intense radiation belts test our theories of terrestrial and solar electromagnetic phenomena.