Hydrodynamic Outcomes. Transitional Discs. of Planet Scattering in. Nick Moeckel IoA. Phil Armitage Colorado
|
|
- Bernice Leonard
- 6 years ago
- Views:
Transcription
1 Hydrodynamic Outcomes of Planet Scattering in Transitional Discs Nick Moeckel IoA Phil Armitage Colorado
2 Messy Transitional Dynamics Hydro to Gravitational transition HR 8799 Marois+ HST imaging of Orion
3 Messy Dynamics Question: what happens planet-planet to scattering outcomes in a Mon. Not. R. Astron. Soc. (211) doi:1.1111/j x Hydrodynamic outcomes of planet scattering in transitional discs Nickolas Moeckel 1 and Philip J. Armitage 2,3 1 Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 HA 2 JILA, 44 UCB, University of Colorado, Boulder, CO , USA 3 Department of Astrophysical and Planetary Sciences, University of Colorado, Boulder, CO 839, USA Accepted 211 August 25. Received 211 August 24; in original form 211 August 1 ABSTRACT Asignificantfractionofunstablemultipleplanetsystemsarelikelytoscatterduringthe transitional disc phase as gas damping becomes ineffectual. Using a large ensemble of FARGO hydrodynamic simulations and MERCURY N-body integrations, we directly follow the dynamics of planet disc and planet planet interactions through the clearing phase and through 5 Myr of planetary system evolution. Disc clearing is assumed to occur as a result of X-ray-driven photoevaporation. We find that the hydrodynamic evolution of individual scattering systems is complex, and can involve phases in which massive planets orbit within eccentric gaps, or accrete directly from the disc without a gap. Comparing the results to a reference gas-free model, we find that the N-body dynamics and hydrodynamics of scattering into one- and two-planet final states are almost identical. The eccentricity distributions in these channels are almost unaltered by the presence of gas. The hydrodynamic simulations, however, also form a population of low-eccentricity three-planet systems in long-term stable configurations, which are not found in N-body runs. The admixture of these systems results in modestly lower eccentricities in hydrodynamic as opposed to gas-free simulations. The precise incidence of these three-planet systems is likely a function of the initial conditions; different planet setups (number or spacing) may change the quantitative character of this result. We analyse the properties of surviving multiple planet systems, and show that only a small fraction (a few per cent) enter mean motion resonances after scattering, while a larger fraction form stable resonant chains and avoid scattering entirely. Our results remain consistent with the hypothesis that exoplanet eccentricity results from scattering, though the detailed agreement between observations and gas-free simulation results is likely coincidental. We discuss the prospects for further tests of scattering models by observing planets or non-axisymmetric gas structure in transitional discs. Key words: hydrodynamics scattering planets and satellites: dynamical evolution and stability planet disc interactions protoplanetary discs planetary systems. gas disk? 1 INTRODUCTION Prior to gap opening, gravitational interactions between planets and their surrounding gas discs act to efficiently damp planetary ec- 1996; Lin & Ida 1997). Extensive N-body experiments have shown that with realistic mass functions, the dynamics of unstable twoplanet (Ford & Rasio 28), three-planet (Chatterjee et al. 28) or richer systems (Jurić&Tremaine 28)can successfullyreproduce
4 exoplanets in a and e Semi-major axis [AU] Eccentricity from Hanno Rein s ios app Semi-major axis [AU] 1 cumulative fraction eccentricity
5 dynamical origin of eccentricities Instability in multi-planet systems yields ejection, mergers, eccentricity Rasio & Ford 1996 Weidenschilling & Marzari 1996 Lin & Ida 1997 with realistic mass spectrum, excellent agreement to observations n = 2 n = 3 n = 1+ Ford & Rasio 28 Chatterjee+ 28 Juric & Tremaine 28
6 what about the disc? 1D 1 5 Log (Density) at t = 5133yrs 2D Marzari+ 21 y -5 Moeckel x 3D Matsumura+ 21, Chatterjee+ 28
7 hydro X-ray photoevaporation prescription (Owen+) to gravity FARGO (Masset) with modifications MERCURY (Chambers)
8 disc and au 5 MJ Owen+ 211 planet setup Surface Density [g cm ] g cm -2.2 g cm -2 ~1 5 yr Radius [AU].3 5. MJ, f(m) ~ m -1.1 aj = ai + 4 RHij RHij = ( mi + mj) 3Mo 1/3 ai + aj 2
9 disc mass evolution 5 disc mass M J time yr
10 collision example
11 1 15 yr yr 2 another collision example 15 yr a AU 1 mass M J eccentricity disk mass M J time years time years
12 instability outcomes disc lifetime after 5 Myr N N tot disc no disc not stable n p 3 n p 2 n p log t i yr disc no disc
13 eccentricity distributions significant differences triple when systems included cumulative fraction cumulative fraction 1..5 single and Hill stable double systems.3 disc no disc observed pks=.1 pad=.37 eccentricity N N tot.2.1 all scattered systems.3 pks<1-3 pad<1-3 disc no disc observed eccentricity N N tot eccentricity eccentricity
14 scattered and circularized not stable n p n p disc no disc n p x x a AU a AU
15 1 135 yr yr 2 scattered and circularized 57 yr a AU 1 mass M J eccentricity disk mass M J time years time years
16 φ 1, φ 2, ϖ 2 ϖ 1 2 Π Π 2 Π Π 6:3:2 middle inner: 3: Π Π outer middle: 2:1 outer inner: 3: triple resonance example 27 out of 1 never scattered 6 of these have two planets in MMR 12 are in triple resonance 2 Π 2Λ 1 4Λ 2 2Λ 3 φ L Π time years
17 conclusions modestly lower eccentricities when gas included ICs that yield good observational agreement with no gas no longer work as well. 1 and 2 planet outcomes similar to gas-free case- addition of 3 planet outcomes is the difference. however: difference comparable to what you see using different mass functions. IC tuning to reach agreement seems likely. resonance outcomes may be a more sensitive probe fewer 2 body resonances than in previous work, lots of 3 body chains. uncertainties in resonance disruption need to be resolved
Dynamically Unstable Planetary Systems Emerging Out of Gas Disks
EXTREME SOLAR SYSTEMS ASP Conference Series, Vol. 398, 2008 D. Fischer, F. A. Rasio, S. E. Thorsett, and A. Wolszczan Dynamically Unstable Planetary Systems Emerging Out of Gas Disks Soko Matsumura, Edward
More information2 Ford, Rasio, & Yu. 2. Two Planets, Unequal Masses
2 Ford, Rasio, & Yu unlikely to have developed such a large eccentricity, since dissipation in the disk tends to circularize orbits. Dynamical instabilities leading to the ejection of one planet while
More informationPlanetesimal Migration and the Curious Trend in the Period Ratio Distribution of the Kepler Multis
Planetesimal Migration and the Curious Trend in the Period Ratio Distribution of the Kepler Multis Sourav Chatterjee Eric B. Ford University of Florida April 5, 2013 University of Florida Kepler multiple
More informationTesting Theories of Planet Formation & Dynamical Evolution of Planetary Systems using Orbital Properties of Exoplanets
Testing Theories of Planet Formation & Dynamical Evolution of Planetary Systems using Orbital Properties of Exoplanets Eric B. Ford Harvard-Smithsonian Center for Astrophysics (Starting at UF in August
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 informationHabitability in the Upsilon Andromedae System
Habitability in the Upsilon Andromedae System Adrienne Dove University of Missouri Columbia Institute for Astronomy University of Hawaii Mentor: Nader Haghighipour ABSTRACT We investigate the habitability
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 informationarxiv: v1 [astro-ph.ep] 8 Dec 2016
Astronomy & Astrophysics manuscript no. draft_arxiv c ESO March, Highly inclined and eccentric massive planets II. Planet-planet interactions during the disc phase Sotiris Sotiriadis, Anne-Sophie Libert,
More informationThe dynamical evolution of exoplanet systems. Melvyn B. Davies Department of Astronomy and Theoretical Physics Lund University
The dynamical evolution of exoplanet systems Melvyn B. Davies Department of Astronomy and Theoretical Physics Lund University Today s Talk 1) Begin with our Solar System. 2) Then consider tightly-packed
More informationSolar 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 informationDisc-Planet Interactions during Planet Formation
Disc-Planet Interactions during Planet Formation Richard Nelson Queen Mary, University of London Collaborators: Paul Cresswell (QMUL), Martin Ilgner (QMUL), Sebastien Fromang (DAMTP), John Papaloizou (DAMTP),
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 informationEccentricity pumping of a planet on an inclined orbit by a disc
Mon. Not. R. Astron. Soc. 44, 49 414 21) doi:1.1111/j.1365-2966.21.16295.x Eccentricity pumping of a planet on an inclined orbit by a disc Caroline Terquem 1,2 and Aikel Ajmia 1 1 Institut d Astrophysique
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 informationarxiv:astro-ph/ v2 15 May 2008
Draft version May 15, 2008 Preprint typeset using L A TEX style emulateapj v. 10/09/06 DYNAMICAL OUTCOMES OF PLANET PLANET SCATTERING Sourav Chatterjee, 1 Eric B. Ford, 2,3,4 Soko Matsumura, 1 and Frederic
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 informationThe Dynamical Evolution of Exoplanet Systems
The Dynamical Evolution of Exoplanet Systems Melvyn B. Davies Department of Astronomy and Theoretical Physics Lund Observatory Collaborators: Clément Bonnerot, John Chambers, Ross Church, Francesca de
More informationPossible commensurabilities among pairs of extrasolar planets
Mon. Not. R. Astron. Soc. 333, L26 L30 (2002) Possible commensurabilities among pairs of extrasolar planets Richard P. Nelson P and John C. B. Papaloizou Astronomy Unit, Queen Mary, University of London,
More informationarxiv: v1 [astro-ph.ep] 13 Sep 2017
Astronomical Journal, manuscript. Preprint typeset using L A TEX style emulateapj v. 03/07/07 THE SCATTERING OUTCOMES OF KEPLER CIRCUMBINARY PLANETS: PLANET MASS RATIO Yan-Xiang Gong 1,2, Jianghui Ji 1
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 informationPredictions for a planet just inside Fomalhaut s eccentric ring
Mon. Not. R. Astron. Soc. 372, L14 L18 (2006) doi:10.1111/j.1745-3933.2006.00216.x Predictions for a planet just inside Fomalhaut s eccentric ring Alice C. Quillen Department of Physics and Astronomy,
More informationKozai-Lidov oscillations
Kozai-Lidov oscillations Kozai (1962 - asteroids); Lidov (1962 - artificial satellites) arise most simply in restricted three-body problem (two massive bodies on a Kepler orbit + a test particle) e.g.,
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 informationFORMING DIFFERENT PLANETARY ARCHITECTURES. I. FORMATION EFFICIENCY OF HOT JUPITES FROM HIGH-ECCENTRICITY MECHANISMS
Draft version February 7, Preprint typeset using L A TEX style AASTeX v.. FORMING DIFFERENT PLANETARY ARCHITECTURES. I. FORMATION EFFICIENCY OF HOT JUPITES FROM HIGH-ECCENTRICITY MECHANISMS Ying Wang,
More informationPlanetary Systems in Stellar Clusters
Planetary Systems in Stellar Clusters Melvyn B. Davies Department of Astronomy and Theoretical Physics Lund Observatory Collaborators: John Chambers, Ross Church, Francesca de Angeli, Douglas Heggie, Thijs
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. p star planet Orange
More informationPLANETARY MIGRATION. Review presented at the Protostars & Planets VI conference in Heidelberg, september 2013 (updated).
PLANETARY MIGRATION Review presented at the Protostars & Planets VI conference in Heidelberg, september 2013 (updated). Reference : Baruteau et al. (2014) (arxiv:1312.4293) see also : https://www.youtube.com/watch?v=_hmw4lh7ioo
More informationModeling interactions between a debris disc and planet: which initial conditions?
Modeling interactions between a debris disc and planet: which initial conditions? Elodie Thilliez @ET_astro Supervisors : Prof Sarah Maddison (Swinburne) Prof Jarrod Hurley (Swinburne) Crédit : NASA/JPL-Caltech
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 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 informationHow do we model each process of planet formation? How do results depend on the model parameters?
How do we model each process of planet formation? How do results depend on the model parameters? Planetary Population Synthesis: The Predictive Power of Planet Formation Theory, Ringberg, Nov 29, 2010
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 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 informationarxiv: v2 [astro-ph.ep] 10 Feb 2015
Draft version February 11, 215 Preprint typeset using L A TEX style emulateapj v. 5/2/11 PLANETESIMAL INTERACTIONS CAN EXPLAIN THE MYSTERIOUS PERIOD RATIOS OF SMALL NEAR-RESONANT PLANETS Sourav Chatterjee
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 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 informationOrigins of Gas Giant Planets
Origins of Gas Giant Planets Ruth Murray-Clay Harvard-Smithsonian Center for Astrophysics Image Credit: NASA Graduate Students Piso Tripathi Dawson Undergraduates Wolff Lau Alpert Mukherjee Wolansky Jackson
More informationVortices in planetary migration
Vortices in planetary migration Min-Kai Lin John Papaloizou DAMTP University of Cambridge October 20, 2009 Outline Introduction: planet migration types Numerical methods, first results and motivation Type
More informationEvolution of protoplanetary discs
Evolution of protoplanetary discs and why it is important for planet formation Bertram Bitsch Lund Observatory April 2015 Bertram Bitsch (Lund) Evolution of protoplanetary discs April 2015 1 / 41 Observations
More informationGlobal models of planetary system formation. Richard Nelson Queen Mary, University of London
Global models of planetary system formation Richard Nelson Queen Mary, University of London Hot Jupiters Cold Jupiters Super-Earths/ Neptunes 2 Sumi et al (2016) Occurence rates 30-50% of FGK stars host
More informationThe dynamical evolution of transiting planetary systems including a realistic collision prescription
The dynamical evolution of transiting planetary systems including a realistic collision prescription Alexander James Mustill Melvyn B. Davies Anders Johansen MNRAS submitted, arxiv.org/abs/1708.08939 Alexander
More informationplanet 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
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 informationThe effects of fly-bys on planetary systems
Mon. Not. R. Astron. Soc. 411, 859 877 (2011) doi:10.1111/j.1365-2966.2010.17730.x The effects of fly-bys on planetary systems Daniel Malmberg, 1 Melvyn B. Davies 1 and Douglas C. Heggie 2 1 Lund Observatory,
More informationSuper-Earths as Failed Cores in Orbital Migration Traps
Super-Earths as Failed Cores in Orbital Migration Traps Yasuhiro Hasegawa (Jet Propulsion Laboratory, California Institute of Technology) Hasegawa 2016, ApJ, 832, 83 Copyright 2017. All rights reserved.
More informationOutward migration of extrasolar planets to large orbital radii
Mon. Not. R. Astron. Soc. 347, 613 624 (2004) Outward migration of extrasolar planets to large orbital radii Dimitri Veras 1,2 and Philip J. Armitage 1,2 1 JILA, University of Colorado, 440 UCB, Boulder,
More informationarxiv: v1 [astro-ph.ep] 18 Jul 2013
Astronomy & Astrophysics manuscript no. ms c ESO 23 July 9, 23 arxiv:37.4864v [astro-ph.ep] 8 Jul 23 Theoretical models of planetary system formation: mass vs semi-major axis Y. Alibert,2, F. Carron, A.
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 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 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 informationDr G. I. Ogilvie Lent Term 2005 INTRODUCTION
Accretion Discs Mathematical Tripos, Part III Dr G. I. Ogilvie Lent Term 2005 INTRODUCTION 0.1. Accretion If a particle of mass m falls from infinity and comes to rest on the surface of a star of mass
More informationThe dynamics of extra-solar planets
Institute for Advanced Study The dynamics of extra-solar planets Hanno Rein @ Franklin Institute, November 2011 Planet formation Planet formation Credit: NASA/JPL-Caltech/T. Pyle (SSC) Planet Migration
More informationIntroduction. Convergence of the fragmentation boundary in self-gravitating discs
Convergence of the fragmentation boundary in self-gravitating discs Collaborators : Phil Armitage - University of Colorado Duncan Forgan- University of St Andrews Sijme-Jan Paardekooper Queen Mary, University
More informationNon-ideal hydrodynamics in protoplanetary discs
Non-ideal hydrodynamics in protoplanetary discs Min-Kai Lin Steward Theory Fellow University of Arizona March 15 2016 Example: disc asymmetries Vortices at planetary gap edges (HD142527, Casassus et al.,
More informationPLANET-DISC INTERACTIONS and EARLY EVOLUTION of PLANETARY SYSTEMS
PLANET-DISC INTERACTIONS and EARLY EVOLUTION of PLANETARY SYSTEMS C. Baruteau, A. Crida, B. Bitsch, J. Guilet, W. Kley, F. Masset, R. Nelson, S-J. Paardekooper, J. Papaloizou INTRODUCTION Planets form
More informationTHE ORIGIN AND EVOLUTION OF FREE-FLOATING PLANETS IN STAR CLUSTERS
THE ORIGIN AND EVOLUTION OF FREE-FLOATING PLANETS IN STAR CLUSTERS M.B.N. (Thijs) Kouwenhoven Kavli Institute for Astronomy and Astrophysics, Peking University Hao Wei (MPIA), Li Yun (KIAA), Wang Long
More informationPREDICTIONS FOR THE CORRELATION BETWEEN GIANT AND TERRESTRIAL EXTRASOLAR PLANETS IN DYNAMICALLY EVOLVED SYSTEMS
The Astrophysical Journal, 645:1509 1515, 2006 July 10 # 2006. The American Astronomical Society. All rights reserved. Printed in U.S.A. PREDICTIONS FOR THE CORRELATION BETWEEN GIANT AND TERRESTRIAL EXTRASOLAR
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 informationType III migration in a low viscosity disc
Type III migration in a low viscosity disc Min-Kai Lin John Papaloizou mkl23@cam.ac.uk, minkailin@hotmail.com DAMTP University of Cambridge KIAA, Beijing, December 13, 2009 Outline Introduction: type III
More informationarxiv: v1 [astro-ph.ep] 23 Mar 2010
Formation of Terrestrial Planets from Protoplanets under a Realistic Accretion Condition arxiv:1003.4384v1 [astro-ph.ep] 23 Mar 2010 Eiichiro Kokubo Division of Theoretical Astronomy, National Astronomical
More informationGas Disks to Gas Giants: Simulating the Birth of Planetary Systems
arxiv:0808.1439v1 [astro-ph] 11 Aug 2008 Gas Disks to Gas Giants: Simulating the Birth of Planetary Systems Edward W. Thommes, 1,2 Soko Matsumura, 2 Frederic A. Rasio 2 1 University of Guelph, Guelph,
More informationPlanetary system dynamics. Planetary migration Kozai resonance Apsidal resonance and secular theories Mean motion resonances Gravitational scattering
Planetary system dynamics Planetary migration Kozai resonance Apsidal resonance and secular theories Mean motion resonances Gravitational scattering How should the planets of a typical planetary system
More informationFormation of the Solar System Chapter 8
Formation of the Solar System Chapter 8 To understand the formation of the solar system one has to apply concepts such as: Conservation of angular momentum Conservation of energy The theory of the formation
More informationA REGION VOID OF IRREGULAR SATELLITES AROUND JUPITER
The Astronomical Journal, 136:909 918, 2008 September c 2008. The American Astronomical Society. All rights reserved. Printed in the U.S.A. doi:10.1088/0004-6256/136/3/909 A REGION VOID OF IRREGULAR SATELLITES
More informationABSTACT KUIPER BINARY OBJECT FORMATION
KUIPER BINARY OBJECT FORMATION R. C. Nazzario, K Orr, C. Covington, D. Kagan, and T. W. Hyde Center for Astrophysics, Space Physics and Engineering Research, Baylor University, Waco, TX 76798-7310, USA,
More informationThe Dispersal of Protoplanetary Disks
The Dispersal of Protoplanetary Disks R. Alexander 1, I. Pascucci 2, S. Andrews 3, P. Armitage 4, L. Cieza 5 1 University of Leicester, 2 The University of Arizona 3 Harvard-Smithsonian Center for Astrophysics
More informationThe migration and growth of protoplanets in protostellar discs
Mon. Not. R. Astron. Soc. 318, 18 36 (2000) The migration and growth of protoplanets in protostellar discs Richard P. Nelson, 1 John C. B. Papaloizou, 1 Frédéric Masset 1 and Willy Kley 2,3 1 Astronomy
More informationNew results on the formation of the Moon
New results on the formation of the Moon Julien Salmon 1, Robin M. Canup 1 ESLAB Symposium - Formation and Evolution of Moons 26 June 2012 ESTEC, Noordwijk, The Netherlands 1 Southwest Research Institute,
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 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 informationMars 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
More informationTidal Dissipation in Binaries
Tidal Dissipation in Binaries From Merging White Dwarfs to Exoplanetary Systems Dong Lai Cornell University March 14, 2013, Harvard ITC Colloquium Tidal Dissipation in Binaries I. Merging White Dwarf Binaries
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 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 informationFrom pebbles to planetesimals and beyond
From pebbles to planetesimals... and beyond (Lund University) Origins of stars and their planetary systems Hamilton, June 2012 1 / 16 Overview of topics Size and time Dust µ m Pebbles cm Planetesimals
More informationPLANET FORMATION BY GRAVITATIONAL INSTABILITY? Kaitlin Kratter University of Arizona. Sagan Summer Workshop, July 2015
PLANET FORMATION BY GRAVITATIONAL INSTABILITY? Kaitlin Kratter University of Arizona Sagan Summer Workshop, July 2015 PLANET FORMATION BY in GAS! GRAVITATIONAL INSTABILITY? Kaitlin Kratter University of
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 informationFORMATION OF HOT PLANETS BY A COMBINATION OF PLANET SCATTERING, TIDAL CIRCULARIZATION, AND THE KOZAI MECHANISM
The Astrophysical Journal, 678:498Y508, 008 May 1 # 008. The American Astronomical Society. All rights reserved. Printed in U.S.A. FORMATION OF HOT PLANETS BY A COMBINATION OF PLANET SCATTERING, TIDAL
More informationPlanetary Formation and Orbital Stability in Binary Star Systems
Mem. S.A.It. Suppl. Vol. 6, 172 c SAIt 2005 Memorie della Supplementi Planetary Formation and Orbital Stability in Binary Star Systems D. Turrini 1, M. Barbieri 1, F. Marzari 2, P. Thebault 3, and P. Tricarico
More informationSubstellar companions and isolated planetary-mass objects from protostellar disc fragmentation
Mon. Not. R. Astron. Soc. 346, L36 L40 (2003) Substellar companions and isolated planetary-mass objects from protostellar disc fragmentation W. K. M. Rice, 1 P. J. Armitage, 2,3 I. A. Bonnell, 1 M. R.
More informationSubstellar companions and isolated planetary-mass objects from protostellar disc fragmentation
Mon. Not. R. Astron. Soc. 346, L36 L40 (2003) Substellar companions and isolated planetary-mass objects from protostellar disc fragmentation W. K. M. Rice, 1 P. J. Armitage, 2,3 I. A. Bonnell, 1 M. R.
More informationDynamical Evolution of Planets in Disks
Dynamical Evolution of Planets in Disks Planets in resonant Orbits W. Kley (wilhelm.kley@uni-tuebingen.de) Astronomie und Astrophysik, Abt. Computational Physics, Universität Tübingen, D-72076 Tübingen,
More informationDetecting Terrestrial Planets in Transiting Planetary Systems
Detecting Terrestrial Planets in Transiting Planetary Systems Jason H. Steffen Brinson Postdoctoral Fellow, Fermilab Northwestern University May 3, 2007 Fermilab Planetary Science Team Jason H. Steffen
More informationFrom pebbles to planets
. (Lund University) with Michiel Lambrechts, Katrin Ros, Andrew Youdin, Yoram Lithwick From Atoms to Pebbles Herschel s View of Star and Planet Formation Grenoble, March 2012 1 / 11 Overview of topics
More informationarxiv: v2 [astro-ph.ep] 30 Nov 2013
Extreme orbital evolution from hierarchical secular coupling of two giant planets Jean Teyssandier,, Smadar Naoz 2,3, Ian Lizarraga 4, Frederic A. Rasio 3,5 arxiv:3.548v2 [astro-ph.ep] 3 Nov 23 ABSTRACT
More informationThe Solar Nebula Theory
Reading: Chap. 21, Sect.21.1, 21.3 Final Exam: Tuesday, December 12; 4:30-6:30PM Homework 10: Due in recitation Dec. 1,4 Astro 120 Fall 2017: Lecture 25 page 1 Astro 120 Fall 2017: Lecture 25 page 2 The
More informationExtrasolar Planets: Dynamics and Formation - Numerical Simulations for Terrestrial Planet Formation
Extrasolar Planets: Dynamics and Formation - Numerical Simulations for Terrestrial Planet Formation Jianghui JI 1, 3 Collaborators: Lin LIU 2, H. Kinoshita 4, H. Nakai 4, G. LI 1, 3 J. E. Chambers 5, R.
More informationarxiv: v1 [astro-ph.ep] 21 Jun 2011
Dynamical evolution of planetary systems Alessandro Morbidelli Dep. Cassiopee, University of Nice - Sophia Antipolis, CNRS, Observatoire de la Côte d Azur; Nice, France arxiv:1106.4114v1 [astro-ph.ep]
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 informationThe TRAPPIST-1 system: Orbital evolution, tidal dissipation, formation and habitability
Mon. Not. R. Astron. Soc. 000, 000 000 0000 Printed 22 November 2017 MN LATEX style file v2.2 The TRAPPIST-1 system: Orbital evolution, tidal dissipation, formation and habitability As the system is likely
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 informationPlanet Formation. XIII Ciclo de Cursos Especiais
Planet Formation Outline 1. Observations of planetary systems 2. Protoplanetary disks 3. Formation of planetesimals (km-scale bodies) 4. Formation of terrestrial and giant planets 5. Evolution and stability
More informationSTABILITY OF HYPOTHETICAL TROJAN PLANETS IN EXOPLANETARY SYSTEMS
STABILITY OF HYPOTHETICAL TROJAN PLANETS IN EXOPLANETARY SYSTEMS Bálint Érdi, Georgina Fröhlich, Imre Nagy and Zsolt Sándor Department of Astronomy Loránd Eötvös University Pázmány Péter sétány 1/A H-1117
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 informationFormation and evolution of the two 4/3 resonant giants planets in HD
DOI: 10.1051/0004-6361/201424820 c ESO 2014 Astronomy & Astrophysics Formation and evolution of the two 4/3 resonant giants planets in HD 200964 M. Tadeu dos Santos, J. A. Correa-Otto, T. A. Michtchenko,
More informationC. Mordasini & G. Bryden. Sagan Summer School 2015
Hands-on Session I C. Mordasini & G. Bryden Sagan Summer School 2015 Population synthesis Monday Tuesday Wednesday Thursday Thursday GlobalPFE model Minimum physical processes to consider GlobalPFE: Toy
More informationOther planetary systems
Exoplanets are faint! Other planetary systems Planets are seen only by reflected light at optical wavelengths At the distance of another star the faint light of a planet is lost in the glare of the star
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 informationLecture 20: Planet formation II. Clues from Exoplanets
Lecture 20: Planet formation II. Clues from Exoplanets 1 Outline Definition of a planet Properties of exoplanets Formation models for exoplanets gravitational instability model core accretion scenario
More informationKepler Planets back to the origin
Kepler Planets back to the origin Acknowledgements to the Kepler Team Yanqin Wu (Toronto) + Yoram Lithwick, James Owen, Ji-Wei Xie, Nikhil Mahajan, Bonan Pu, Ari Silburt Kepler planets: an Unexpected population
More information