Mars Growth Stunted by an Early Orbital Instability between the Giant Planets
|
|
- Cameron Steven Mosley
- 5 years ago
- Views:
Transcription
1 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
2 My Past Life
3 Studying Planetary Dynamics with N- Body Integrators Two Bodies: Can be solved exactly. Many Bodies: Approximations: Circularly Restricted 3 Body. Computer Integration: Midpoint Method. Euler Method. Leapfrog Method
4 Complications Integration Time: Solar System formed from millions of small bodies colliding over Myr- Gyr timescales. Close Encounters: Approximations such as circularly restrictive 3-body break down during close encounters. Collisional Fragmentation: What happens when things collide. Energy and Momentum conservation: How much error is acceptable? Relativity: ~2 degrees/century precession in Mercury s orbit. Images: nasa.gov
5 Solutions Hamiltonian Splitting: Symplectic Integration scheme. Split Hamiltonian into a purely Keplerian and an Interaction component. Switch integration schemes for close encounters. Perturbative methods to handle relativity. Map parameter space for collisions: Perfectly accretionary. Erosive. Hit and Run. Hit and re-accrete. Figure: Chambers, 1999
6 The Evolution of the Outer Solar System AFTER dissipation of gas and dust in the primordial disk. Saturn, Uranus and Neptune interact with the primordial Kuiper Belt. Scatter Objects inward. Fernandez and Ip (1984). Jupiter interacts with these scattered objects: Ejects them from the Solar System. Over time, Jupiter s Orbit moves in and Saturn s moves out. Cross a 2:1 (3:2) MMR and destabilizes the entire system. Figure: Gomes et al (2005)
7 Levison et al, 2008
8 Small Mars Problem Images: nasa.gov Mars analogues are rare in embryo accretion models, Mercurys are almost non-existent. (Chambers and Wetherill 1998; Chambers, 2001; O Brien et al, 2006; Raymond et al, 2009) Possible Solutions: Extra Eccentric Jupiter and Saturn (Raymond et al, 2009) AU annulus (Hansen, 2009) Grand Tack Model (Walsh et al, 2011) Local Depletion (Izidoro et al, 2015)
9
10
11 Mars Formed
12 Mars Formed
13 Control
14 Planets Formed
15 Summary/Future Work An early instability significantly REDUCES the MASS of MARS ANALOGUES. When the instability occurs ~1-10 Myr after gas disk dispersal: Mars is left behind as a stranded embryo. Significant amount of material from > 2 AU is scattered towards the forming Earth. BLUE WATERS: Include Collisional Fragmentation. Could Mercury be formed by a high velocity impact with Venus? Thoroughly investigate consequences for the Asteroid Belt.
16 Questions
17 Motivation for an Early Instability Timing of instability dependent on initial disk properties (Gomes et al, 2005). Difficult for terrestrial planets to survive a late instability (Brasser et al, 2009, Kaib & Chambers, 2016). Projectile size distribution for a late instability different than observed (Morbidelli et al, 2017). Self Interacting Disks unlikely to last 400 Myr (Quarles & Kaib, in prep). New lunar data from LRO and better dating of samples. (Zeller et al, 2017) Fassett and Minton (2012)
18 How would an early instability affect the forming Terrestrial Planets? Integrate a resonant configuration of Giant Planets right up to the instability: 3:2 3:2 3:2 3:2 Evolve the terrestrial planets, take snapshots of the system at 104,105,106 and 107 yrs: 3:2 Imbed the forming terrestrial planets in the instability and integrate for 200 Myr:
19 Simulation Parameters Mercury6 Hybrid Integrator, 6.0 day time-step (Chambers, 1999). Inner Disk: 100 embryos/1000 planetesimals/ r -3/2 surface density profile: Outer Disk: 1000 bodies/ r -1 surface density profile (Nesvorny & Morbidelli, 2012):
20 Results 70.9% of all Mars analogues formed small. 38.9% of systems form no Mars (82% no or small). Most successful when instability is delayed 10 Myr in to terrestrial planetary formation: 20% correct architecture of inner planets. 25% form Mars in less than 15 Myr. 95% form Earth in greater than 50 Myr. 39% leave behind an Asteroid Belt with no Embryos. 83% sufficiently deliver volatiles to Earth.
21 Planets Formed
22 Earliest Instabilities and Collisional Fragmentation The earliest instabilities we look at often look nothing like the solar system: No Mars. Only one planet. All planets too small. System s with the most violent instabilities are most likely to finish with a few small, or no terrestrial planets. Collisional Fragmentation can play a large role in embryo accretion and must be accounted for (Chambers, 2013). Collisional velocities in our runs are LOW for Earth and Mars analogues and HIGH for Venus analogues.
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,
More informationA few points on the dynamical evolution of the young solar system. Renu Malhotra The University of Arizona
A few points on the dynamical evolution of the young solar system Renu Malhotra The University of Arizona A few points on the dynamical evolution of the young solar system Renu Malhotra The University
More informationTerrestrial 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?
More informationOrbital 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
More informationarxiv: 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
More informationAccretion 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,
More informationPlanetary 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
More informationThe 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
More informationPlanet 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
More informationMinimum Mass Solar Nebulae, Nice model, & Planetary Migration.
Minimum Mass Solar Nebulae, Nice model, & Planetary Migration. Aurélien CRIDA 1) MMSN : definition, recipe Minimum Mass Solar Nebula Little reminder : It is not a nebula, but a protoplanetary disc. Solar
More informationDetectability 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
More informationAstronomy 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,
More informationPLANETARY 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
More informationThe Empty Primordial Asteroid Belt
The Empty Primordial Asteroid Belt arxiv:1709.04242v1 [astro-ph.ep] 13 Sep 2017 Sean N. Raymond 1, Andre Izidoro 1,2 1 Laboratoire d Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, allée Geoffroy
More informationPlanetary 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
More informationThe 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
More informationMeteorite 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.
More informationLecture 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
More informationASTEROIDS, 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
More informationKuiper 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
More informationarxiv: 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,
More informationThe 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
More informationarxiv: 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.
More informationFormation of the Solar System. What We Know. What We Know
Formation of the Solar System Many of the characteristics of the planets we discussed last week are a direct result of how the Solar System formed Until recently, theories for solar system formation were
More informationAstronomy 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,
More informationarxiv: v1 [astro-ph.ep] 27 Dec 2015
Draft version August 23, 218 Preprint typeset using L A TEX style emulateapj v. 5/2/11 EFFECTS OF DYNAMICAL EVOLUTION OF GIANT PLANETS ON THE DELIVERY OF ATMOPHILE ELEMENTS DURING TERRESTRIAL PLANET FORMATION
More informationINVESTIGATION 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,
More informationEXCITATION 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
More informationDefinitions. 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
More informationarxiv: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
More informationDynamical water delivery: how Earth and rocky exoplanets get wet
Dynamical water delivery: how Earth and rocky exoplanets get wet Sean Raymond Laboratoire d Astrophysique de Bordeaux with Andre Izidoro and Alessandro Morbidelli Is Earth dry or wet? Surface water = 1
More informationDynamic 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
More informationAstronomy 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
More informationWed. 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
More informationarxiv: 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
More informationPlanets: 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
More informationLecture 16. How did it happen? How long did it take? Where did it occur? Was there more than 1 process?
Planet formation in the Solar System Lecture 16 How did it happen? How long did it take? Where did it occur? Was there more than 1 process? Planet formation How do planets form?? By what mechanism? Planet
More informationWho was here? How can you tell? This is called indirect evidence!
1 Who was here? How can you tell? This is called indirect evidence! 2 How does a planetary system form? The one we can study in the most detail is our solar system. If we want to know whether the solar
More informationDynamical 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
More informationWhat 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
More informationon it, can still ripen a bunch of grapes as though it had nothing else in the Universe to do. Galileo Galilei
The Sun, with all the planets revolving around it, and depending on it, can still ripen a bunch of grapes as though it had nothing else in the Universe to do. Galileo Galilei What We Will Learn Today Where
More informationas 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
More informationarxiv: v1 [astro-ph.ep] 16 Sep 2016
Preprint typeset using LATEX style emulateapj v. 04/17/13 THE ASTEROID BELT AS A RELIC FROM A CHAOTIC EARLY SOLAR SYSTEM ANDRÉ IZIDORO Laboratoire d astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N,
More informationFROM 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
More informationChapter 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
More informationF. 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
More informationPlanetary 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
More informationWhat 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
More informationSolar 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
More informationDynamical behaviour of the primitive asteroid belt
Mon. Not. R. Astron. Soc. 293, 405 410 (1998) Dynamical behaviour of the primitive asteroid belt Adrián Brunini Observatorio Astronómico de La Plata, Profoeg, Paseo del Bosque, (1900) La Plata, Argentina
More informationDebris discs, exoasteroids and exocomets. Mark Wyatt Institute of Astronomy, University of Cambridge
Debris discs, exoasteroids and exocomets Mark Wyatt Institute of Astronomy, University of Cambridge The Solar System s outer and inner debris belts Outer debris: Kuiper belt Inner debris: Asteroid belt
More informationOrigin 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;
More informationAccretion of Planets. Bill Hartmann. Star & Planet Formation Minicourse, U of T Astronomy Dept. Lecture 5 - Ed Thommes
Accretion of Planets Bill Hartmann Star & Planet Formation Minicourse, U of T Astronomy Dept. Lecture 5 - Ed Thommes Overview Start with planetesimals: km-size bodies, interactions are gravitational (formation
More informationThe 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
More informationYes, inner planets tend to be and outer planets tend to be.
1. Planet Density Make some general comments about inner and outer planets density Inner Planets Density Outer Planets Density Is there a pattern or a trend in planet density? Yes, inner planets tend to
More informationEffect 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
More informationClass Exercise. Today s Class: The Origin & Evolution of the Moon. Space in the News: NASA and Russia Partner Up for Crewed Deep-Space Missions
Today s Class: The Origin & Evolution of the Moon 1. 2. 3. 4. Homework. Read: Sections 9.2-9.3 in Cosmic Perspective. Next class is at Fiske Planetarium! Need volunteers for Space in the News. Exam #2
More informationThe 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
More informationEVOLUTIONS 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
More informationForming habitable planets on the computer
Forming habitable planets on the computer Anders Johansen Lund University, Department of Astronomy and Theoretical Physics 1/9 Two protoplanetary discs (Andrews et al., 2016) (ALMA Partnership, 2015) Two
More informationInitial Conditions: The temperature varies with distance from the protosun.
Initial Conditions: The temperature varies with distance from the protosun. In the outer disk it is cold enough for ice to condense onto dust to form large icy grains. In the inner solar system ice can
More informationWILLIAM I. NEWMAN, UCLA PHILIP W. SHARP, U. OF AUCKLAND BRUCE G. BILLS, JPL
CATASTROPHIC METEORITE 1 IMPACTS ON EARTH WILLIAM I. NEWMAN, UCLA PHILIP W. SHARP, U. OF AUCKLAND BRUCE G. BILLS, JPL Solar system with different scales for distance and for size: presents role of giant
More informationRuth Murray-Clay University of California, Santa Barbara
A Diversity of Worlds: Toward a Theoretical Framework for the Structures of Planetary Systems Ruth Murray-Clay University of California, Santa Barbara Strange New Worlds. Slide credit: Scott Gaudi ~1500
More informationEXOPLANET LECTURE PLANET FORMATION. Dr. Judit Szulagyi - ETH Fellow
EXOPLANET LECTURE PLANET FORMATION Dr. Judit Szulagyi - ETH Fellow (judits@ethz.ch) I. YOUNG STELLAR OBJECTS AND THEIR DISKS (YSOs) Star Formation Young stars born in 10 4 10 6 M Sun Giant Molecular Clouds.
More informationClass Exercise. Today s Class: The History & Evolution of the Moon
Today s Class: The History & Evolution of the Moon 1. Homework. Read: Sections 9.2-9.3 in Cosmic Perspective. 2. Homework #6 due next Monday, March 19 th. 3. Exam 2 on Wednesday, March 21, covers telescopes
More informationThe Long-Term Dynamical Evolution of Planetary Systems
The Long-Term Dynamical Evolution of Planetary Systems Melvyn B. Davies Department of Astronomy and Theoretical Physics Lund University Co-authors: Fred Adams, Philip Armitage, John Chambers, Eric Ford,
More informationThe Formation of Mars: Building Blocks and Accretion Time Scale
Space Sci Rev (2013) 174:11 25 DOI 10.1007/s11214-012-9904-2 The Formation of Mars: Building Blocks and Accretion Time Scale Ramon Brasser Received: 4 December 2011 / Accepted: 28 May 2012 / Published
More informationForming 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
More informationClass 15 Formation of the Solar System
Class 16 Extra-solar planets The radial-velocity technique for finding extrasolar planets Other techniques for finding extrasolar planets Class 15 Formation of the Solar System What does a successful model
More informationAstro 1: Introductory Astronomy
Astro 1: Introductory Astronomy David Cohen Class 16: Thursday, March 20 Spring 2014 large cloud of interstellar gas and dust - giving birth to millions of stars Hubble Space Telescope: Carina Nebula
More information-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
More informationOn 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?
More informationMoon 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
More informationForming terrestrial planets & impacts
Lecture 11 Forming terrestrial planets & impacts Lecture Universität Heidelberg WS 11/12 Dr. C. Mordasini Based partially on script of Prof. W. Benz Mentor Prof. T. Henning Lecture 11 overview 1. Terrestrial
More informationIntroduction to the Solar System
Introduction to the Solar System Sep. 11, 2002 1) Introduction 2) Angular Momentum 3) Formation of the Solar System 4) Cowboy Astronomer Review Kepler s Laws empirical description of planetary motion Newton
More informationAstronomy 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,
More informationAstronomy. 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
More information1star 1 star 9 8 planets 63 (major) moons asteroids, comets, meteoroids
The Solar System 1star 1 star 9 8 planets 63 (major) moons asteroids, comets, meteoroids The distances to planets are known from Kepler s Laws (once calibrated with radar ranging to Venus) How are planet
More informationForma&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
More informationChapter 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
More informationPlanet 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
More informationCentaurs (scatterers) as a Probe of the Inner Oort Cloud. Nathan Kaib University of Oklahoma
Centaurs (scatterers) as a Probe of the Inner Oort Cloud Nathan Kaib University of Oklahoma Outline Scatterer dynamics background/motivation OSSOS / survey simulator Numerical simulations of scatterer
More informationHow inner planetary systems relate to inner and outer debris belts. Mark Wyatt Institute of Astronomy, University of Cambridge
How inner planetary systems relate to inner and outer debris belts Mark Wyatt Institute of Astronomy, University of Cambridge The Solar System s outer and inner debris belts Outer debris: Kuiper belt Inner
More informationThe Solar System consists of
The Universe The Milky Way Galaxy, one of billions of other galaxies in the universe, contains about 400 billion stars and countless other objects. Why is it called the Milky Way? Welcome to your Solar
More informationarxiv: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
More informationCosmology 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
More informationExoplanets: a dynamic field
Exoplanets: a dynamic field Alexander James Mustill Amy Bonsor, Melvyn B. Davies, Boris Gänsicke, Anders Johansen, Dimitri Veras, Eva Villaver The (transiting) exoplanet population Solar System Hot Jupiters:
More informationOrigin 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
More informationUnit 12 Lesson 1 What Objects Are Part of the Solar System?
Unit 12 Lesson 1 What Objects Are Part of the Solar System? The Solar System Earth, other planets, and the moon are part of a solar system. A solar system is made up of a star and the planets and other
More informationResonant Planets: From Stability to Violent Upheaval
EXTREME SOLAR SYSTEMS ASP Conference Series, Vol. 398, 28 D. Fischer, F. A. Rasio, S. E. Thorsett, and A. Wolszczan Resonant Planets: From Stability to Violent Upheaval E. W. Thommes, 1 G. Bryden, 2 Y.
More informationLETTER. Collisionless encounters and the origin of the lunar inclination
doi:10.1038/nature16137 Collisionless encounters and the origin of the lunar inclination Kaveh Pahlevan 1 & Alessandro Morbidelli 1 The Moon is generally thought to have formed from the debris ejected
More informationDynamical 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
More informationChapter 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
More informationWhich of the following planets are all made up of gas? When a planets orbit around the Sun looks like an oval, it s called a(n)
When a planets orbit around the Sun looks like an oval, it s called a(n) - ellipse - circle - axis - rotation Which of the following planets are all made up of gas? - Venus, Mars, Saturn and Pluto - Jupiter,
More informationDYNAMICS 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
More informationWritten by G. Jeffrey Taylor
1 of 8 March 31, 2010 --- Planetary compositions allow us to test computer models of planet formation. Written by G. Jeffrey Taylor Hawai i Institute of Geophysics and Planetology ophisticated calculations
More informationPLANETARY MIGRATION A. CRIDA
PLANETARY MIGRATION A. CRIDA (the migration of Jupiter carrying its satellites. Alegory.) 1 INTRODUCTION A planet orbiting in a protoplanetary disk launches a one-armed, spiral wake. Ωp star planet Orange
More informationarxiv: 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
More informationPluto, 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
More informationTHE ROLE OF GIANT PLANETS IN TERRESTRIAL PLANET FORMATION Harold F. Levison 1 and Craig Agnor 2
The Astronomical Journal, 125:2692 2713, 23 May # 23. The American Astronomical Society. All rights reserved. Printed in U.S.A. E THE ROLE OF GIANT PLANETS IN TERRESTRIAL PLANET FORMATION Harold F. Levison
More information