A few points on the dynamical evolution of the young solar system. Renu Malhotra The University of Arizona
|
|
|
- Frank Henderson
- 5 years ago
- Views:
Transcription
1 A few points on the dynamical evolution of the young solar system Renu Malhotra The University of Arizona
2 A few points on the dynamical evolution of the young solar system Renu Malhotra The University of Arizona Late stages of planet formation - planetesimal-driven migration
3 A few points on the dynamical evolution of the young solar system Renu Malhotra The University of Arizona Late stages of planet formation - planetesimal-driven migration Kuiper belt & asteroid belt extent, timescale of Jupiter-Neptune migration
4 A few points on the dynamical evolution of the young solar system Renu Malhotra The University of Arizona Late stages of planet formation - planetesimal-driven migration Kuiper belt & asteroid belt extent, timescale of Jupiter-Neptune migration - appears to be nearly incompatible with stability of terrestrial planets
5 A few points on the dynamical evolution of the young solar system Renu Malhotra The University of Arizona Late stages of planet formation - planetesimal-driven migration Kuiper belt & asteroid belt extent, timescale of Jupiter-Neptune migration - appears to be nearly incompatible with stability of terrestrial planets - how to save Earth?
6 Jupiter,...,Neptune + trillions of leftover planetesimals Jupiter migrates inward, Neptune migrates outward Fernandez & Ip 1984
7 1993 Nature Publishing Group Pluto s resonance and eccentricity g Group ep = 0.25 Neptune s migration an 5 AU time
8 More observational evidence in Kuiper Belt dynamical structure Inclination (degrees) eccentricity semimajor axis, a (AU)
9 More observational evidence in Kuiper Belt dynamical structure Inclination (degrees) eccentricity semimajor axis, a (AU) resonances eccentricities inclinations
10 More observational evidence in Kuiper Belt dynamical structure Inclination (degrees) eccentricity semimajor axis, a (AU) Resonance sweeping during outward migration of Neptune smooth migration adiabatic invariant (3:2 MMR): a 1/2 [2-3(1-e 2 ) 1/2 cos i] Neptune migrated out 10AU
11 More observational evidence in Kuiper Belt dynamical structure Inclination (degrees) eccentricity semimajor axis, a (AU)
12 More observational evidence in Kuiper Belt dynamical structure Inclination (degrees) eccentricity semimajor axis, a (AU) Planetesimal-driven migration Angular momentum conservation: (m pl a) (m N a N ) m pl 30 m planetesimal disk fueled Neptune s ~10 AU migration Energy conservation Jupiter: (m J /a J ) (m pl /a) a J -0.2AU
13 More observational evidence in Kuiper Belt dynamical structure Inclination (degrees) eccentricity semimajor axis, a (AU) Resonance sweeping during outward migration of Neptune smooth migration adiabatic invariant (3:2 MMR): a 1/2 [2-3(1-e 2 ) 1/2 cos i] Neptune migrated out 10AU m(planetesimals) 30 M Jupiter migrated inward~0.2 AU BUT: This constraint fails if planets encounter MMRs
14 time
15 The initial conditions were carefully chosen to... time
16 The initial conditions were carefully chosen to... time Nice Model (2005)
17 More observational evidence in Kuiper Belt dynamical structure Inclination (degrees) eccentricity semimajor axis, a (AU) Resonance sweeping during outward migration of Neptune smooth migration adiabatic invariant (3:2 MMR): a 1/2 [2-3(1-e 2 ) 1/2 cos i] Neptune migrated out 10 AU m(planetesimals) 30 M Jupiter migrated inward~0.2 AU BUT: This constraint fails if planets encounter MMRs. Does that mean we have NO constraints on Neptune/Jupiter migration?
18 Distribution of asteroids observationally complete primordial set: H<9.7 (D>50 km), N 950 Minton & Malhotra, 2009
19 Distribution of asteroids observationally complete primordial set: H<9.7 (D>50 km), N 950 3:1 5:2 7:3 2:1 Minton & Malhotra, 2009
20 Distribution of asteroids observationally complete primordial set: H<9.7 (D>50 km), N 950 ν6 3:1 5:2 7:3 2:1 Minton & Malhotra, 2009
21 Distribution of asteroids observationally complete primordial set: H<9.7 (D>50 km), N 950 ν6 3:1 5:2 7:3 2:1 Minton & Malhotra, 2009 dynamically stable regions are not uniformly filled distribution reflects the last major dynamical event
22 Sculpting of the Asteroid Belt simulated 4 gyr of planetary perturbations Minton & Malhotra, 2009
23 Sculpting of the Asteroid Belt simulated 4 gyr of planetary perturbations compared to observed belt Minton & Malhotra, 2009 ν6 3:1 5:2 2:1
24 Sculpting of the Asteroid Belt simulated 4 gyr of planetary perturbations compared to observed belt Minton & Malhotra, 2009 ν6 3:1 5:2 2:1 Missing asteroids: explained by effects of Jupiter-Saturn migration a Jupiter -0.2AU, a Saturn +1.0AU migration timescale a few megayears
25 Saturn s migration ν6 secular resonance sweeping eccentricity (c) excites asteroid eccentricities Numerical time Integration (myr) Minton & Malhotra, 2011 eccentricity vector: ef = ei+δe δe : controlled by e6 da6/dt needs a deeper look Saturn: Δa 1 AU, da/dt 0.15 (e 6 /e 6c ) 2 AU/myr
26 Effects of Jupiter-Saturn migration on terrestrial planets Agnor & Lin, 2012 Brasser et al., 2012 Brasser et al., 2013 Mars Earth Venus Mercury ν5 secular resonance - excite eccentricities - multiple crossings - low probability of cancellation - low probability of successful outcomes in numerical sims, even with very fast migration, jumping Jupiter style This is disturbing!
27 How to save the terrestrial planets? Options? Agnor & Lin suggest that the terrestrial planets formed after giant planet migration was completed Strom et al., But missing asteroids left their imprint in the crater record - ~3.9 Ga
28 How to save the terrestrial planets? Options? Agnor & Lin suggest that the terrestrial planets formed after giant planet migration was completed Strom et al., But missing asteroids left their imprint in the crater record - ~3.9 Ga - Size distribution of impactors - same as Main belt asteroids but different than younger impactors
29 How to save the terrestrial planets? Options? - other missing mass to kill ν5? - different arrangement of terrestrial planets? - 5th terrestrial planet? - massive leftover planetesimal population in the inner solar system?
Mars Growth Stunted by an Early Orbital Instability between the Giant Planets
Mars Growth Stunted by an Early Orbital Instability between the Giant Planets M.S. Clement University of Oklahoma Advisor: Professor N.A. Kaib Collaborators: S.N. Raymond, K.J. Walsh 19 September 2017
Orbital Structure and Dynamical Evolution of. TNOs. Patryk Sofia Lykawka ( )
Orbital Structure and Dynamical Evolution of TNOs Patryk Sofia Lykawka ( ) patryksan@gmail.com Outline I: Introduction and motivation II: III: IV: Dynamical stability and planet migration Stable TNO populations
Solar System evolution and the diversity of planetary systems
Solar System evolution and the diversity of planetary systems Alessandro Morbidelli (OCA, Nice) Work in collaboration with: R. Brasser, A. Crida, R. Gomes, H. Levison, F. Masset, D. O brien, S. Raymond,
Planetary migration and the Late Heavy Bombardment (better late than never)
Planetary migration and the Late Heavy Bombardment (better late than never) S. Goldman April 2007 The early history of the Solar System, though still shrouded in mystery, is slowly being pieced together
The primordial excitation and clearing of the asteroid belt Revisited
Icarus 191 (2007) 434 452 www.elsevier.com/locate/icarus The primordial excitation and clearing of the asteroid belt Revisited David P. O Brien a,b,, Alessandro Morbidelli a, William F. Bottke c a Observatoire
arxiv: v2 [astro-ph.ep] 4 Mar 2011
![arxiv: v2 [astro-ph.ep] 4 Mar 2011](/thumbs/89/97548280.jpg "arxiv: v2 [astro-ph.ep] 4 Mar 2011")
32 pages, 7 figures. Accepted for publication in ApJ on March 1, 2011 arxiv:1102.3131v2 [astro-ph.ep] 4 Mar 2011 Secular resonance sweeping of the main asteroid belt during planet migration David A. Minton
arxiv: v1 [astro-ph.ep] 10 Sep 2009
![arxiv: v1 [astro-ph.ep] 10 Sep 2009](/thumbs/72/67787690.jpg "arxiv: v1 [astro-ph.ep] 10 Sep 2009")
Astronomy & Astrophysics manuscript no. secterr c ESO 9 September 1, 9 Constructing the secular architecture of the solar system II: The terrestrial planets R. Brasser 1, A. Morbidelli 1, R. Gomes, K.
PLANETARY FORMATION 5) THE SOLAR SYSTEM : GRAND TAK & NICE MODEL. Aurélien CRIDA
PLANETARY FORMATION 5) THE SOLAR SYSTEM : GRAND TAK & NICE MODEL Aurélien CRIDA Has the Solar System always been as now? So far, you know that Mercury ia at 0,4 AU from the Sun Venus at 0,7 the Earth at
Kuiper Belt Dynamics and Interactions
Kuiper Belt Dynamics and Interactions Minor Planet Center Ruth Murray-Clay Harvard-Smithsonian Center for Astrophysics Kuiper belt µm ejected by radiation pressure larger grains migrate in via PR drag
What is it like? When did it form? How did it form. The Solar System. Fall, 2005 Astronomy 110 1
What is it like? When did it form? How did it form The Solar System Fall, 2005 Astronomy 110 1 Fall, 2005 Astronomy 110 2 The planets all orbit the sun in the same direction. The Sun spins in the same
Effect of sun s mass loss in the dynamical evolution of the Solar System
Effect of sun s mass loss in the dynamical evolution of the Solar System Despoina K. Skoulidou Harry Varvoglis & Kleomenis Tsiganis Aristotle University of Thessaloniki 12 th Hellenic Astronomical Conference
Lecture Outlines. Chapter 15. Astronomy Today 7th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 15 Astronomy Today 7th Edition Chaisson/McMillan Chapter 15 The Formation of Planetary Systems Units of Chapter 15 15.1 Modeling Planet Formation 15.2 Terrestrial and Jovian Planets
Astronomy 405 Solar System and ISM
Astronomy 405 Solar System and ISM Lecture 17 Planetary System Formation and Evolution February 22, 2013 grav collapse opposed by turbulence, B field, thermal Cartoon of Star Formation isolated, quasi-static,
Secular resonance sweeping of the main asteroid belt during planet migration
27 pages, 7 figures; submitted to ApJ on May 27, 2010 Secular resonance sweeping of the main asteroid belt during planet migration David A. Minton Southwest Research Institute and NASA Lunar Science Institute
Terrestrial planet formation: planetesimal mixing KEVIN WALSH (SWRI)
Terrestrial planet formation: planetesimal mixing KEVIN WALSH (SWRI) Questions How are terrestrial planets put together? Where do they get their material? Questions How are terrestrial planets put together?
Dynamical Evolution of the Early Solar System
Dynamical Evolution of the Early Solar System David Nesvorný 1 arxiv:1807.06647v1 [astro-ph.ep] 17 Jul 2018 Xxxx. Xxx. Xxx. Xxx. YYYY. AA:1 40 This article s doi: 10.1146/((please add article doi)) Copyright
Linking NEAs to their main-belt source regions
Near-Earth (NEAs) Department of Astronomy, University of Belgrade Stardust ITN: Opening Training School 21st November 2013, Glasgow, Scotland Near-Earth (NEAs) Table of contents 1 Main phases during the
Forming the Kuiper Belt by the Outward Transport of Objects During Neptune s Migration
Forming the Kuiper Belt by the Outward Transport of Objects During Neptune s Migration Harold F. Levison and Alessandro Morbidelli Southwest Research Institute, Boulder, CO 80302, USA Observatoire de la
F. Marzari, Dept. Physics, Padova Univ. Planetary migration
F. Marzari, Dept. Physics, Padova Univ. Planetary migration Standard model of planet formation based on Solar system exploration Small semimajor axes Large eccentricities The standard model Protostar +Disk
Astronomy 405 Solar System and ISM
Astronomy 405 Solar System and ISM Lecture 18 Planetary System Formation and Evolution February 25, 2013 grav collapse opposed by turbulence, B field, thermal Cartoon of Star Formation isolated, quasi-static,
What Have We Found? 1978 planets in 1488 systems as of 11/15/15 (http://exoplanet.eu/ ) 1642 planets candidates (http://exoplanets.
Exoplanets. II What Have We Found? 1978 planets in 1488 systems as of 11/15/15 (http://exoplanet.eu/ ) 1642 planets + 3787 candidates (http://exoplanets.org) Detected by radial velocity/astrometry: 621
The dynamical evolution of the asteroid belt in the pebble accretion scenario
The dynamical evolution of the asteroid belt in the pebble accretion scenario S. Pirani 1, A. Johansen 1, B. Bitsch 1, A. J. Mustill 1 and D. Turrini 2,3 1 Lund Observatory, Department of Astronomy and
ASTEROIDS, COMETS, AND TRANS-NEPTUNIAN OBJECTS:
ASTEROIDS, COMETS, AND TRANS-NEPTUNIAN OBJECTS: SMALL BODIES IN THE SOLAR SYSTEM Rosemary E. Pike ASIAA TIARA Summer School 2018 On the Origins of the Solar System SMALL BODIES IN THE SOLAR SYSTEM Formation
DYNAMICS OF THE KUIPER BELT
To appear in Protostars and Planets IV Preprint (Jan 1999): http://www.lpi.usra.edu/science/renu/home.html DYNAMICS OF THE KUIPER BELT Renu Malhotra (1), Martin Duncan (2), and Harold Levison (3) (1) Lunar
The Collisional Evolution of Small Bodies in the Solar System
The Collisional Evolution of Small Bodies in the Solar System David P. O'Brien* Planetary Science Institute Tucson, AZ Invited Review CD '07 Alicante, Spain * with Don Davis, Scott Kenyon and Benjamin
arxiv: v1 [astro-ph.ep] 18 Dec 2018
![arxiv: v1 [astro-ph.ep] 18 Dec 2018](/thumbs/92/109205497.jpg "arxiv: v1 [astro-ph.ep] 18 Dec 2018")
Icarus; accepted Preprint typeset using L A TEX style emulateapj v. 12/16/11 THE EARLY INSTABILITY SCENARIO: TERRESTRIAL PLANET FORMATION DURING THE GIANT PLANET INSTABILITY, AND THE EFFECT OF COLLISIONAL
-Melissa Greenberg, Arielle Hoffman, Zachary Feldmann, Ryan Pozin, Elizabeth Weeks, Christopher Pesota, & Sara Pilcher
-Melissa Greenberg, Arielle Hoffman, Zachary Feldmann, Ryan Pozin, Elizabeth Weeks, Christopher Pesota, & Sara Pilcher Formation Overview All explanations as to how the solar system was formed are only
Detectability of extrasolar debris. Mark Wyatt Institute of Astronomy, University of Cambridge
Detectability of extrasolar debris Mark Wyatt Institute of Astronomy, University of Cambridge Why image extrasolar debris? Emission spectrum shows dust thermal emission, used to infer radius of parent
Accretion of Uranus and Neptune
Accretion of Uranus and Neptune by collisions among planetary embryos Jakubík M., Morbidelli A., Neslušan L., Brasser R. Astronomical Institute SAS, Tatranska Lomnica Observatoire de la Côte d Azur, Nice,
planet migration driven by a planetesimal disk Solar System & extra solar planets: evidence for/against planet migration?
2 planet migration driven by a gas disk: type I & type II planet migration driven by a planetesimal disk Solar System & extra solar planets: evidence for/against planet migration? 3 Type I migration: follow
Meteorite Shock Ages, Early Bombardment, and the Age of the Moon
Meteorite Shock Ages, Early Bombardment, and the Age of the Moon William Bottke 1, David Vokrouhlicky 1, Simone Marchi 1, Tim Swindle (U. Arizona), Ed Scott (U. Hawaii), A. Jackson (ASU) John Weirich (U.
arxiv:astro-ph/ v2 14 Jan 1999
DYNAMICS OF THE KUIPER BELT RENU MALHOTRA Lunar and Planetary Institute arxiv:astro-ph/9901155v2 14 Jan 1999 MARTIN DUNCAN Queen s University and HAROLD LEVISON Southwest Research Institute ABSTRACT Our
Planetary Embryos Never Formed in the Kuiper Belt
Icarus 157, 241 248 (2002) doi:10.1006/icar.2002.6832, available online at http://www.idealibrary.com on Planetary Embryos Never Formed in the Kuiper Belt A. Morbidelli and C. Jacob Observatoire de la
The Secular Evolution of the Primordial Kuiper Belt
The Secular Evolution of the Primordial Kuiper Belt Joseph M. Hahn (LPI) March 20, 2003 What Happened to the Kuiper Belt? KBO orbits indicate that some process stirred up the KB Neptune s outward migration
Planets: Name Distance from Sun Satellites Year Day Mercury 0.4AU yr 60 days Venus yr 243 days* Earth 1 1 yr 1 day Mars 1.
The Solar System (Ch. 6 in text) We will skip from Ch. 6 to Ch. 15, only a survey of the solar system, the discovery of extrasolar planets (in more detail than the textbook), and the formation of planetary
Chapter 15 The Formation of Planetary Systems
Chapter 15 The Formation of Planetary Systems Units of Chapter 15 15.1 Modeling Planet Formation 15.2 Formation of the Solar System 15.3 Terrestrial and Jovian Planets 15.4 Interplanetary Debris 15.5 Solar
Planetary Interiors. Earth s Interior Structure Hydrostatic Equilibrium Heating Constituent Relations Gravitational Fields Isostasy Magnetism
Planetary Interiors Earth s Interior Structure Hydrostatic Equilibrium Heating Constituent Relations Gravitational Fields Isostasy Magnetism Isostasy Courtesy of U of Leeds Now apply this idea to topography
Evidence from the asteroid belt for a violent past evolution of Jupiter s orbit
Evidence from the asteroid belt for a violent past evolution of Jupiter s orbit Alessandro Morbidelli, Ramon Brasser, Rodney Gomes, Harold F. Levison, Kleomenis Tsiganis To cite this version: Alessandro
Wed. Sept. 20, Today: For Monday Sept. 25 and following days read Chapter 4 (The Moon) of Christiansen and Hamblin (on reserve).
Wed. Sept. 20, 2017 Reading: For Friday: Connelly et al. 2012, "The Absolute Chronology and Thermal Processing of Solids in the Solar Protoplanetary Disk." 338: 651-665. Simon et al., 2011, "Oxygen Isotope
Planetary System Stability and Evolution. N. Jeremy Kasdin Princeton University
Planetary System Stability and Evolution N. Jeremy Kasdin Princeton University (Lots of help from Eric Ford, Florida and Robert Vanderbei, Princeton) KISS Exoplanet Workshop 10 November 2009 Motivation
Overview of the Solar System. Solar system contents one star, several planets, lots of debris.
Overview of the Solar System Solar system contents one star, several planets, lots of debris. Most of it is the Sun! 99.8% of the mass of the Solar System resides in the Sun. A hot ball of mostly hydrogen
Solar System Scales. PTYS/ASTR 206 The Golden Age of Planetary Exploration Shane Byrne
Solar System Scales PTYS/ASTR 206 The Golden Age of Planetary Exploration Shane Byrne shane@lpl.arizona.edu PYTS/ASTR 206 Solar System Scales 2 In this lecture Measuring length, mass and time Angular sizes
Moon Obs #1 Due! Moon visible: early morning through afternoon. 6 more due June 13 th. 15 total due June 25 th. Final Report Due June 28th
Moon Obs #1 Due! Moon visible: early morning through afternoon 6 more due June 13 th 15 total due June 25 th Final Report Due June 28th Our Solar System Objectives Overview of what is in our solar system
The Solar System - I. Alexei Gilchrist. [The Story of the Solar System]
![The Solar System - I. Alexei Gilchrist. [The Story of the Solar System]](/thumbs/89/99064825.jpg "The Solar System - I. Alexei Gilchrist. [The Story of the Solar System]")
The Solar System - I Alexei Gilchrist [The Story of the Solar System] Some resources Section 13.3 of Voyages (references and links at end) References noted in these slides The Story of the Solar System,
as the orbits of distant planetoids are expected to be randomized over billions of year by the gravity of the four giant planets.
Dynamics of Extreme Outer Solar System Objects Principle investigators/supervisors: Denis Gaidashev (Matematiska Institution); Erik Zackrisson (Institutionen fo r fysik och astronomi) 1. Purpose and aims
Chapter 15: The Origin of the Solar System
Chapter 15: The Origin of the Solar System The Solar Nebula Hypothesis Basis of modern theory of planet formation: Planets form at the same time from the same cloud as the star. Planet formation sites
The dynamics of Plutinos
The dynamics of Plutinos Qingjuan Yu and Scott Tremaine Princeton University Observatory, Peyton Hall, Princeton, NJ 08544-1001, USA ABSTRACT Plutinos are Kuiper-belt objects that share the 3:2 Neptune
Planetary system dynamics Part III Mathematics / Part III Astrophysics
Planetary system dynamics Part III Mathematics / Part III Astrophysics Lecturer: Prof. Mark Wyatt (Dr. Amy Bonsor on 9,11 Oct) Schedule: Michaelmas 2017 Mon, Wed, Fri at 10am MR11, 24 lectures, start Fri
Astronomy Test Review. 3 rd Grade
Astronomy Test Review 3 rd Grade Match the vocabulary word to its definition. Outer Planets The path a planet takes around the sun. Inner Planets Orbit Sun The center of our solar system. Small, rocky
arxiv: v1 [astro-ph.ep] 6 Aug 2015
![arxiv: v1 [astro-ph.ep] 6 Aug 2015](/thumbs/80/82276653.jpg "arxiv: v1 [astro-ph.ep] 6 Aug 2015")
Preprint typeset using L A TEX style emulateapj v. 5/2/11 TERRESTRIAL PLANET FORMATION CONSTRAINED BY MARS AND THE STRUCTURE OF THE ASTEROID BELT André Izidoro Université de Bordeaux, Laboratoire d Astrophysique
Origin of the Structure of the Kuiper Belt during a Dynamical Instability in the Orbits of Uranus and Neptune
Origin of the Structure of the Kuiper Belt during a Dynamical Instability in the Orbits of Uranus and Neptune Harold F. Levison Southwest Research Institute, USA Alessandro Morbidelli Observatoire de la
EVOLUTIONS OF SMALL BODIES IN OUR SOLAR SYSTEM
EVOLUTIONS OF SMALL BODIES IN OUR SOLAR SYSTEM Dynamics and collisional processes Dr. Patrick MICHEL Côte d'azur Observatory Cassiopée Laboratory, CNRS Nice, France 1 Plan Chapter I: A few concepts on
FROM THE SCATTERED DISK TO THE OORT CLOUD The Extended Scattered Disk
FROM THE SCATTERED DISK TO THE OORT CLOUD The Extended Scattered Disk Julio A. Fernández Departamento de Astronomía, Facultad de Ciencias, Montevideo, URUGUAY Adrián Brunini, Tabaré Gallardo, Rodney Gomes
Prospects for unseen planets beyond Neptune
Prospects for unseen planets beyond Neptune Renu Malhotra The University of Arizona, Tucson, Arizona, USA; renu@lpl.arizona.edu Abstract. Several anomalous features in the orbital distribution of distant
arxiv:astro-ph/ v1 10 Oct 2005
DRAFT VERSION FEBRUARY 5, 2008 Preprint typeset using L A TEX style emulateapj HIGH-RESOLUTION SIMULATIONS OF THE FINAL ASSEMBLY OF EARTH-LIKE PLANETS 1: TERRESTRIAL ACCRETION AND DYNAMICS SEAN N. RAYMOND
arxiv: v1 [astro-ph.ep] 10 Jun 2014
![arxiv: v1 [astro-ph.ep] 10 Jun 2014](/thumbs/88/115871694.jpg "arxiv: v1 [astro-ph.ep] 10 Jun 2014")
Lunar and Terrestrial Planet Formation in the Grand Tack Scenario arxiv:1406.2697v1 [astro-ph.ep] 10 Jun 2014 rspa.royalsocietypublishing.org Research Article submitted to journal Subject Areas: xxxxx,
Clicker Question: Clicker Question: Clicker Question:
Test results Last day to drop without a grade is Feb 29 Grades posted in cabinet and online F D C B A In which direction would the Earth move if the Sun s gravitational force were suddenly removed from
Dynamic Exoplanets. Alexander James Mustill
Dynamic Exoplanets Alexander James Mustill Exoplanets: not (all) like the Solar System Exoplanets: not (all) like the Solar System Solar System Lissauer et al 14 Key questions to bear in mind What is role
Astronomy November, 2016 Introduction to Astronomy: The Solar System. Mid-term Exam 3. Practice Version. Name (written legibly):
Astronomy 101 16 November, 2016 Introduction to Astronomy: The Solar System Mid-term Exam 3 Practice Version Name (written legibly): Honor Pledge: On my honor, I have neither given nor received unauthorized
Astronomy. physics.wm.edu/~hancock/171/ A. Dayle Hancock. Small 239. Office hours: MTWR 10-11am
Astronomy A. Dayle Hancock adhancock@wm.edu Small 239 Office hours: MTWR 10-11am Planetology II Key characteristics Chemical elements and planet size Radioactive dating Solar system formation Solar nebula
Planet Formation: theory and observations. Sean Raymond University of Colorado (until Friday) Observatoire de Bordeaux
Planet Formation: theory and observations Sean Raymond University of Colorado (until Friday) Observatoire de Bordeaux Outline Stages of Planet Formation Solar System Formation Cores to disks (c2d) Observational
Survey of the Solar System. The Sun Giant Planets Terrestrial Planets Minor Planets Satellite/Ring Systems
Survey of the Solar System The Sun Giant Planets Terrestrial Planets Minor Planets Satellite/Ring Systems Definition of a dwarf planet 1. Orbits the sun 2. Is large enough to have become round due to the
Outline. Question of Scale. Planets Dance. Homework #2 was due today at 11:50am! It s too late now.
Outline Homework #2 was due today at 11:50am! It s too late now. Planetarium observing is over. Switch Gears Solar System Introduction The Planets, the Asteroid belt, the Kupier objects, and the Oort cloud
Pluto, the Kuiper Belt, and Trans- Neptunian Objects
Pluto, the Kuiper Belt, and Trans- Neptunian Objects 1 What about Pluto? Pluto used to be considered a planet Pluto is one of a large number of Trans-Neptunian Objects, not even the largest one! Discovery
Planetarium observing is over. Nighttime observing starts next week.
Homework #2 was due today at 11:50am! It s too late now. Planetarium observing is over. Solar observing is over. Nighttime observing starts next week. Outline Switch Gears Solar System Introduction The
The Formation of the Solar System
The Formation of the Solar System Basic Facts to be explained : 1. Each planet is relatively isolated in space. 2. Orbits nearly circular. 3. All roughly orbit in the same plane. 4. Planets are all orbiting
Origin of high orbital eccentricity and inclination of asteroids
Earth Planets Space, 53, 85 9, 2 Origin of high orbital eccentricity and inclination of asteroids Makiko Nagasawa, Shigeru Ida, and Hidekazu Tanaka Department of Earth and Planetary Sciences, Tokyo Institute
Lecture Outlines. Chapter 15. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 15 Astronomy Today 8th Edition Chaisson/McMillan Chapter 15 Exoplanets Units of Chapter 15 15.1 Modeling Planet Formation 15.2 Solar System Regularities and Irregularities 15.3
Astronomy A BEGINNER S GUIDE TO THE UNIVERSE EIGHTH EDITION
Astronomy A BEGINNER S GUIDE TO THE UNIVERSE EIGHTH EDITION CHAPTER 4 The Solar System Lecture Presentation 4.0 What can be seen with the naked eye? Early astronomers knew about the Sun, Moon, stars, Mercury,
Which of the following statements best describes the general pattern of composition among the four jovian
Part A Which of the following statements best describes the general pattern of composition among the four jovian planets? Hint A.1 Major categories of ingredients in planetary composition The following
Solar System. Sun, 8 planets, hundred moons, thousand.dwarf.planets million asteroids, billion comets etc.
Solar System Sun, 8 planets, hundred moons, thousand.dwarf.planets million asteroids, billion comets etc. Comparative Planetology Compares planets and other solar system bodies to help understand how they
ASTR 200 : Lecture 6 Introduction to the Solar System Pearson Education Inc., publishing as Addison-Wesley
ASTR 200 : Lecture 6 Introduction to the Solar System 1 2004 Pearson Education Inc., publishing as Addison-Wesley Comparative Planetology Studying the similarities among and differences between the planets
Asteroids, Comets and NEOs. (Answers) Solar System Impacts. Author: Sarah Roberts
Asteroids, Comets and NEOs (Answers) Author: Sarah Roberts Asteroids, Comets and NEOs - Impact craters on the Earth 1. Using the data given below for real impact craters on the Earth, investigate the effect
Nature and Origin of Planetary Systems f p "
Nature and Origin of Planetary Systems f p " Our Solar System as Example" We know far more about our solar system than about any other" It does have (at least) one planet suitable for life" Start with
Dynamical evolution of asteroid fragments originating near the ν 6 resonance
Dynamical evolution of asteroid fragments originating near the ν 6 resonance Takashi Ito and Renu Malhotra Lunar & Planetary Laboratory, The University of Arizona, Tucson, AZ 85721 0092, USA Correspondence
Chapter 4 The Solar System
Chapter 4 The Solar System Comet Tempel Chapter overview Solar system inhabitants Solar system formation Extrasolar planets Solar system inhabitants Sun Planets Moons Asteroids Comets Meteoroids Kuiper
EXCITATION AND DEPLETION OF THE ASTEROID BELT IN THE EARLY INSTABILITY SCENARIO
AJ; accepted Preprint typeset using L A TEX style emulateapj v. 12/16/11 EXCITATION AND DEPLETION OF THE ASTEROID BELT IN THE EARLY INSTABILITY SCENARIO Matthew S. Clement 1,*, Sean N. Raymond 2, & Nathan
Paweł Kankiewicz, Ireneusz Włodarczyk
Meeting on Asteroids and Comets in Europe Vienna, Austria, 12-14.05.2006 The stability of orbits of effective Mars Crossers Paweł Kankiewicz, Ireneusz Włodarczyk Astrophysics Division, Institute of Physics,
Definitions. Stars: M>0.07M s Burn H. Brown dwarfs: M<0.07M s No Burning. Planets No Burning. Dwarf planets. cosmic composition (H+He)
Definitions Stars: M>0.07M s Burn H cosmic composition (H+He) Brown dwarfs: M
Forma&on of the Solar System
Forma&on of the Solar System Overview We can explain the observed trends in our solar system through the nebular theory The laws of physics (Chapter 4) come into play here. The major dis&nc&on between
23.1 The Solar System. Orbits of the Planets. Planetary Data The Solar System. Scale of the Planets The Solar System
23.1 The Solar System Orbits of the Planets The Planets: An Overview The terrestrial planets are planets that are small and rocky Mercury, Venus, Earth, and Mars. The Jovian planets are the huge gas giants
Chapter 06 Let s Make a Solar System
like? Big picture. Chapter 06 Let s Make a Solar System How did it come to be this way? Where did it come from? Will I stop sounding like the Talking Heads? The solar system exhibits clear patterns of
Planetary system dynamics Mathematics tripos part III / part III Astrophysics
Planetary system dynamics Mathematics tripos part III / part III Astrophysics Lecturer: Dr Mark Wyatt Schedule: Lent 2014 Mon Wed Fri 10am MR9, 24 lectures, start Fri 17 Jan, end Wed 12 Mar Problems: My
Which of the following correctly describes the meaning of albedo?
Which of the following correctly describes the meaning of albedo? A) The lower the albedo, the more light the surface reflects, and the less it absorbs. B) The higher the albedo, the more light the surface
Cosmology Vocabulary
Cosmology Vocabulary Vocabulary Words Terrestrial Planets The Sun Gravity Galaxy Lightyear Axis Comets Kuiper Belt Oort Cloud Meteors AU Nebula Solar System Cosmology Universe Coalescence Jovian Planets
Planetary Perturbations on the 2 : 3 Mean Motion Resonance with Neptune
PASJ: Publ. Astron. Soc. Japan 54, 493 499, 2002 June 25 c 2002. Astronomical Society of Japan. Planetary Perturbations on the 2 : 3 Mean Motion Resonance with Neptune Tetsuharu FUSE Subaru Telescope,
Planet formation in protoplanetary disks. Dmitry Semenov Max Planck Institute for Astronomy Heidelberg, Germany
Planet formation in protoplanetary disks Dmitry Semenov Max Planck Institute for Astronomy Heidelberg, Germany Suggested literature "Protoplanetary Dust" (2010), eds. D. Apai & D. Lauretta, CUP "Protostars
Origin of the Solar System
Origin of the Solar System Look for General Properties Dynamical Regularities Orbits in plane, nearly circular Orbit sun in same direction (CCW from N.P.) Rotation Axes to orbit plane (Sun & most planets;
How did it come to be this way? Will I stop sounding like the
Chapter 06 Let s Make a Solar System How did it come to be this way? Where did it come from? Will I stop sounding like the Talking Heads? What does the solar system look like? Big picture. The solar system
INVESTIGATION OF ORBITAL EVOLUTION OF INTERPLANETARY DUST PARTICLES ORIGINATING FROM KUIPER BELT AND ASTEROID BELT OBJECTS
INVESTIGATION OF ORBITAL EVOLUTION OF INTERPLANETARY DUST PARTICLES ORIGINATING FROM KUIPER BELT AND ASTEROID BELT OBJECTS 1 PALAK DHARSANDIA, 2 DR. JAYESH PABARI, 3 DR. CHARMY PATEL 1 Research Scholar,
Origin of the Solar System
Origin of the Solar System Current Properties of the Solar System Look for General Properties Dynamical Regularities Orbits in plane, nearly circular Orbit sun in same direction (CCW from North pole) Rotation
Origin of the Solar System
Origin of the Solar System and Solar System Debris 1 Debris comets meteoroids asteroids gas dust 2 Asteroids irregular, rocky hunks small in mass and size Ceres - largest, 1000 km in diameter (1/3 Moon)
THE STRUCTURE OF THE DISTANT KUIPER BELT IN A NICE MODEL SCENARIO
Accepted to the Astronomical Journal: January 21, 2017 Preprint typeset using L A TEX style AASTeX6 v. 1.0 THE STRUCTURE OF THE DISTANT KUIPER BELT IN A NICE MODEL SCENARIO R. E. Pike 1,2, S. Lawler 3,
The Solar Nebula Theory. This lecture will help you understand: Conceptual Integrated Science. Chapter 28 THE SOLAR SYSTEM
This lecture will help you understand: Hewitt/Lyons/Suchocki/Yeh Conceptual Integrated Science Chapter 28 THE SOLAR SYSTEM Overview of the Solar System The Nebular Theory The Sun Asteroids, Comets, and
The formation of Uranus and Neptune among Jupiter and Saturn
Submitted to AJ The formation of Uranus and Neptune among Jupiter and Saturn E. W. Thommes Astronomy Department, University of California, Berkeley, CA 94720 M. J. Duncan Physics Department, Queen s University,
THE KUIPER BELT: OVERVIEW
THE KUIPER BELT: OVERVIEW David Jewitt Institute for Astronomy, 2680 Woodlawn Drive, Honolulu, HI 96822, USA e-mail jewitt@ifa.hawaii.edu web www.ifa.hawaii.edu/faculty/jewitt Paper on the web at www.ifa.hawaii.edu/faculty/jewitt/papers/eso
Chapter 9 Remnants of Rock and Ice. Asteroids, Comets, and Pluto
Chapter 9 Remnants of Rock and Ice Asteroids, Comets, and Pluto 9.1 Asteroids and Meteorites Our Goals for Learning Why is there an asteroid belt? How are meteorites related to asteroids? Asteroid Facts
THE PLANE OF THE KUIPER BELT
The Astronomical Journal, 127:2418 2423, 2004 April # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. THE PLANE OF THE KUIPER BELT Michael E. Brown Division of Geological
(Accepted to The Astronomical Journal 11/Dec/2007) Title AN OUTER PLANET BEYOND PLUTO AND ORIGIN OF THE TRANS-NEPTUNIAN BELT ARCHITECTURE
(Accepted to The Astronomical Journal 11/Dec/2007) Title AN OUTER PLANET BEYOND PLUTO AND ORIGIN OF THE TRANS-NEPTUNIAN BELT ARCHITECTURE Proposed Running Head AN OUTER PLANET BEYOND PLUTO Authors Patryk
On the Origin of the Rocky Planets, Fugue in Venus Megacollision
On the Origin of the Rocky Planets, Fugue in Venus Megacollision Simon Porter October 30, 2009 And art thou, then, a world like ours, Flung from the orb that whirled our own A molten pebble from its zone?