Debris Disks and the Formation and Evolution of Planetary Systems. Christine Chen October 14, 2010
|
|
- Rudolph McDonald
- 5 years ago
- Views:
Transcription
1 Debris Disks and the Formation and Evolution of Planetary Systems Christine Chen October 14,
2 Outline Dust Debris in our Solar System The Discovery of Dust Debris Around Other Stars The Connection Planet-Dust Connection Unsolved Problems in Planetary System Formation and Evolution JWST and the Future of Debris Disk Observations 2
3 Outline Dust Debris in our Solar System The Discovery of Dust Debris Around Other Stars The Connection Planet-Dust Connection Unsolved Problems in Planetary System Formation and Evolution JWST and the Future of Debris Disk Observations 3
4 Our Solar System Terrestrial Planets Asteroid Belt Jovian Planets Kuiper Belt Ice Dwarf Planets Oort Cloud 4
5 The Zodiacal Light M dust = g = M planets = 10-4 M MAB L IR (dust) = 100 L IR (planets) 5
6 Asteroid Families Distribution of the proper sine of inclination vs. semimajor axis for the first 1500 numbered asteroids. The Hirayama families Themis (T), Eos (E), and Koronis (K) are marked. Kirkwood gaps are visible. The detached Phocaea region is at upper left. Chapman et al. (1989) In 1918 Hirayama discovered concentrations of asteroids in a-e-i space (osculatory orbital semi-major axis, eccentricity and inclination) he named families. It is widely believed that these families resulted from the break up of larger parent bodies. 6
7 Origin of Dust Bands in the Zodiacal Light he,, dust bands in the Zodiacal Light are believed to have been generated by mutual collisions within the Themis, Koronis, and Eos families. Other dust bands are not found in association with other major asteroid families with the possible exception of the Io family. The Koronis family has a greater dust population than the larger Themis family. The majority of dust bands were probably produced by large random collisions among individual asteroids. 7
8 The Kuiper Belt More than one thousand km-sized KBOs have now been discovered. Although, no dusty disk has yet been detected, one 8 is believed to exist.
9 Outline Dust Debris in our Solar System The Discovery of Dust Debris Around Other Stars The Connection Planet-Dust Connection Unsolved Problems in Planetary System Formation and Evolution JWST and the Future of Debris Disk Observations 9
10 The Vega Phenomenon Routine calibration observations of Vega revealed 60 and 100 μm fluxes 10 times brighter than expected from the stellar photosphere alone. Subsequent coronagraphic images of Pic revealed an edge-on disk which extends beyond 1000 AU in radius. Infrared excess is well described by thermal emission from grains. Backman & Paresce
11 A Circumstellar Disk Around Pictoris! Spectral Type: A5V Distance: 19.3 pc T dust : 85 K L IR /L * : M dust : M R dust : 1400 AU Inclination: 2-4º Age: 20 ± 10 Myr Mouillet et al. (1997) 11
12 Radiation Effects Radiation Pressure If F rad > F grav (or > 1), then small grain will be radiatively driven from the system 3L * Q pr (a) 16 GM * ca Artymowicz (1988) Poynting-Robertson Drag Dust particles slowly spiral into the orbit center due to the Poynting-Robertson effect. The lifetime of grains in a circular orbit is given by t PR 4 a grc 2 D 2 (Burns et al. 1979). 3L * 12
13 Solar Wind Drag The solar wind is a stream of protons, electrons, and heavier ions that are produced in the solar corona and stream off the sun at 400 km/sec Typically, F sw << F grav ; therefore, stellar wind does not effectively drive dust out of the system radially. However, they do produce a drag force completely analogous to the Poynting- Robertson effect t sw 4 a gr D2 3Q sw Ý M sw (Plavchan et al. 2005) 13
14 Debris Disks are dusty disks around main sequence stars. Unseen planets are believed to gravitationally perturb asteroids and comets, causing them to collide with one another generating fine dust grains. Astronomical telescopes detect the starlight scattered by these dust grains and the heat emitted from the grains. 14
15 Outline Dust Debris in our Solar System The Discovery of Dust Debris Around Other Stars The Connection Planet-Dust Connection Unsolved Problems in Planetary System Formation and Evolution JWST and the Future of Debris Disk Observations 15
16 A Possible Planet in the Pic Disk D warp 2 2/ 7 ( M Pa tage) Observed D warp = 70 AU 48 M Jup brown dwarf at <3 AU Or 17.4 M Jup 0.17 M Jup planet at AU STIS/CCD coronagraphic images of the Pic disk. The half-width of the occulted region is 15 AU. At the top is the disk at a logarithmic stretch. At bottom is the disk normalized to the maximum flux, with the vertical scale 16 expanded by a factor of 4 (Heap et al. 2000)
17 Direct Detection of Pic b Standard Star HR 2435 Pic Target/ Standard Target - Standard Lagrange et al
18 A Planet Around Fomalhaut The Fomalhaut disk s brightness asymmetry which may be caused by secular perturbations of dust grain orbits by a planet with a = 40 AU and e = 0.15 Distance between planet and disk and thickness of disk suggest planet mass < 3M Jup Kalas et al. (2008) (Stapelfeldt et al. 2005) 18
19 or a circumplanetary dust disk? Kalas et al Planet is significantly brighter than expected at visual wavelengths Planet possesses same color as center star Planet light could be light scattered from circumplanetary dust grains that are forming a moon 19
20 An Orbiting Planetary System Around HR 8799? Marois et al (see APOD: Gemini North near-infrared ( m) images Reveal 3 objects with projected separations 24, 38, and 60 AU in nearly face-on orbit Around HR 8799, an 160 Myr old, nearby (39.4 pc), main sequence A5V star 20
21 An Asteroid Belt and a Kuiper Belt? The SED of HR 8799 is best fit using two single temperature black bodies with temperatures, T gr = 160 K and 40 K These temperatures correspond to distances of 8 AU and 110 AU, respectively. 21
22 Outline Dust Debris in our Solar System The Discovery of Dust Debris Around Other Stars The Connection Planet-Dust Connection Unsolved Problems in Planetary System Formation and Evolution JWST and the Future of Debris Disk Observations 22
23 Outstanding Science Questions Do terrestrial planets form via the same mechanisms in other solar systems? Are planetary embryos built up on the same timescales and via the same processes? Do large collisions occur, indicating possible moon forming events or water delivery? Do the giant planets in other solar systems migrate, creating periods like the Late Heavy Bombardment? Is the Solar System s composition and architecture (configuration of terrestrial planets, asteroid belt, Jovian planets, and Kuiper Belt) common? 23
24 Planet Formation in Our Solar System Terrestrial Planet Formation Formation of km-sized bodies Oligarchic ~few Myr Growth 1-3 Myr Myr Core Envelope Formation Accretion Giant Planet Formation Giant Impacts including Moon Formation and Late Patina Myr time Once gas has dissipated, km-sized bodies agglomerate into oligarchs that stir small bodies Infrared observations of dust can help constrain disk properties during the period of oligarchic growth to determine average properties and magnitude of variation 24
25 Oligarchic Growth Simulations Coagulation N-body simulations (Kenyon & Bromley 2004, 2005, 2008) Gas dissipates on a timescale ~10 Myr Parent bodies with sizes 1m- 1km at AU in the disk Pluto-sized (1000 km) objects grow via collisions until gas dissipates They stir leftover planetesimals, which generates debris 25
26 MIPS 24 m Excess Evolution Our MIPS 24 m observations of F0-F5 stars are broadly consistent with the Kenyon & Bromley (2008) models, but do not indicate a peak in the upper envelope of 24 m excess at Myr The Carpenter et al. (2009) observation of US show that models must be updated to include dust within 30 AU around the latetype stars Chen et al
27 A Hypervelocity Collision Around HD Silica (Tektite and Obsidian) and possible SiO gas detected Fine dust mass kg; gas mass kg, if gas is fluorescent If gas is dense then it must be transient High spectral resolution observations are needed to confirm SiO, measure gas properties and infer excitation mechanism Lisse et al
28 The Main Asteroid Belt as a Function of Time Grogan et al Simulations of the Main Asteroid Belt suggest that individual collisions between parent asteroids may have been detectable to outside observers Are debris disks observed today bright because they have undergone a recent collision? 28
29 The Period of Late Heavy Bombardment in Our Solar System The moon and terrestrial planets were resurfaced during a short period ( Myr) of intense impact cratering 3.85 Ga called the Late Heavy Bombardment (LHB) Apollo collected lunar impact melts suggest that the planetary impactors had a composition similar to asteroids Size distribution of main belt asteroids is virtually identical to that inferred for lunar highlands Formation and subsequent migration of giant planets may have caused orbital instabilities of asteroids as gravitational resonances swept through the asteroid belt, scattering asteroids into the terrestrial planets. Strom et al. (2005) 29
30 Is Crv Experiencing a Period of Late Heavy Bombardment? Wyatt et al Lisse et al The SED shows warm (~300 K) and cool components (~30 K) The mid-infrared spectrum of the warm component is well modeled using primitive materials such as amorphous silicates and carbon, metal sufides, and water ice 30
31 Outline Dust Debris in our Solar System The Discovery of Dust Debris Around Other Stars The Connection Planet-Dust Connection Unsolved Problems in Planetary System Formation and Evolution JWST and the Future of Debris Disk Observations 31
32 JWST MIRI 6.5 m primary mirror Direct imaging: m Coronagraphic Imaging: 4QPM 10.65, 12.3, 15.5 m Lyot 23 m Low Resolution Spectrograph (R~100): 5-10 (14) m Medium Resolution Spectrograph (R~3000): 5-27 m 32
33 Mid-Infrared Imaging of the Vega Disk Su et al Spitzer MIPS 24 and 70 m imaging has revealed a large extended disk at distances > 85 away from the central star The dust geometry and the low apparent vsini of the star suggests that the star-disk system is face-on Mid-infrared imaging is sensitive to smallest grains that are either gravitationally unbound or on eccentric orbits 33
34 Millimeter Imaging of the Vega Disk Wilner et al IRAM Plateau de Bure inteferometric observations at 1.3 mm detected dust in two lobes around Vega, at distances 9.5 and 8.0 from the central star The observations can be explain using large dust grains that are trapped into principal mean motion resonances of a 3 M Jup planet 34
35 High Resolution Multi-wavelength Imaging Wyatt 2006 Sub-blow out sized dust grains will be subject to radiation pressure (infrared imaging) Largest grains may be trapped in resonances (submm/mm imaging) Intermediate-sized grains may be at similar distances as larger grains but not physically trapped in resonances (far-infrared imaging) 35
36 Processed Grains in the Outer Solar System Infrared spectroscopy of comets and analysis of comet dust grains from STARDUST suggest that comets possess crystalline silicates How does material processed at high temperatures near the sun mix in a proto-planetary disk become incorporated into cold bodies such as comets? 36
37 Spatially Resolved Spectroscopy Gradients in grain size as a function of position in debris disks may suggest the presence of planetesimal belts (e.g. Okamoto et al Pic) Gradients in grain composition as a function of position may allow use to test theories for the origin of atomic gas Okamoto et al
38 Conclusions Our Solar System possesses second generation dust generated by sublimation of comets and collisions between asteroids and KBOs There are exoplanetary systems that possess similar dust In these systems, collisions between asteroids and comets is believed to generate dust Whenever disks are observed at high angular resolution, structures, suggesting the presence of planets are discovered Observations of these systems can help us place constraints on terrestrial planet formation and solar system evolution JWST is expected to make important contributions to our understanding of debris disks 38
Debris Disks and the Evolution of Planetary Systems. Christine Chen September 1, 2009
Debris Disks and the Evolution of Planetary Systems Christine Chen September 1, 2009 Why Study Circumstellar Disks? How common is the architecture of our solar system (terrestrial planets, asteroid belt,
More informationThe Fomalhaut Debris Disk
The Fomalhaut Debris Disk IRAS 12 micron http://ssc.spitzer.caltech.edu/documents/compendium/foma lhaut/ Fomalhaut is a bright A3 V star 7.7 pc away IRAS discovered an IR excess indicating a circumstellar
More informationDebris Disks from Spitzer to Herschel and Beyond. G. H. Rieke, K. Y. L. Su, et al. Steward Observatory The University of Arizona
Debris Disks from Spitzer to Herschel and Beyond G. H. Rieke, K. Y. L. Su, et al. Steward Observatory The University of Arizona Our neighborhood debris disk There was a huge amount of collisional activity
More informationDebris disk structure arising from planetary perturbations
Debris disk structure arising from planetary perturbations Mark Wyatt Institute of Astronomy, Cambridge Debris disk structure arising from planetary perturbations Disk dynamical theory and the observables
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 informationKate Su (University of Arizona)
Debris Disks with Spitzer and beyond Kate Su (University of Arizona) Collaborators: G. Rieke, K. Misselt, P. Smith J. Sierchio, P. Espinoza (U of A), K. Stapelfeldt, F. Morales, G. Bryden (Caltech/JPL),
More informationMid-IR and Far-IR Spectroscopic Measurements & Variability. Kate Su (University of Arizona)
Mid-IR and Far-IR Spectroscopic Measurements & Variability Kate Su (University of Arizona) Five Zones of Debris Dust edge-on view of the Fomalhaut planetary system distance, r 1500 K very hot dust 500
More informationPlacing Our Solar System in Context: [A 12 step program to learn to accept disk evolution]
Placing Our Solar System in Context: [A 12 step program to learn to accept disk evolution] Michael R. Meyer Steward Observatory, The University of Arizona Dana Backman, SOFIA/SETI Institute Alycia Weinberger,
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 information2018 TIARA Summer School Origins of the Solar System. Observations and Modelling of Debris Disks. J.P. Marshall (ASIAA) Wednesday 18 th July 2018
2018 TIARA Summer School Origins of the Solar System Observations and Modelling of Debris Disks J.P. Marshall (ASIAA) Wednesday 18 th July 2018 [Hogerheijde 1998] Debris disks Tenuous belts of icy and
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 informationPlanetary 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
More informationThe architecture of planetary systems revealed by debris disk imaging
The architecture of planetary systems revealed by debris disk imaging Paul Kalas University of California at Berkeley Collaborators: James Graham, Mark Clampin, Brenda Matthews, Mike Fitzgerald, Geoff
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 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 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 informationFormation and Evolution of Planetary Systems
Formation and Evolution of Planetary Systems Meyer, Hillenbrand et al., Formation and Evolution of Planetary Systems (FEPS): First Results from a Spitzer Legacy Science Program ApJ S 154: 422 427 (2004).
More informationPlanetary 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
More informationTransneptunian objects. Minor bodies in the outer Solar System. Transneptunian objects
Transneptunian objects Minor bodies in the outer Solar System Planets and Astrobiology (2016-2017) G. Vladilo Around 1980 it was proposed that the hypothetical disk of small bodies beyond Neptune (called
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 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 informationOrigins of Stars and Planets in the VLT Era
Origins of Stars and Planets in the VLT Era Michael R. Meyer Institute for Astronomy, ETH-Zurich From Circumstellar Disks to Planets 5 November 2009, ESO/MPE Garching Planet Formation = Saving the Solids
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 informationExozodiacal discs with infrared interferometry
Exozodiacal discs with infrared interferometry First results and perspectives * (post-doc at LAOG, Grenoble) and E. Di Folco (Obs. Geneva), J.C. Augereau (LAOG), V. Coudé du Foresto (Obs. Paris), A. Mérand
More information9. Formation of the Solar System
9. Formation of the Solar System The evolution of the world may be compared to a display of fireworks that has just ended: some few red wisps, ashes, and smoke. Standing on a cool cinder, we see the slow
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 informationCircumstellar disks The MIDI view. Sebastian Wolf Kiel University, Germany
Circumstellar disks The MIDI view Sebastian Wolf Kiel University, Germany MPIA MIDI SG concluding meeting May 5, 2014 Overview Circumstellar disks: Potential of IR long-baseline interferometry MIDI: Exemplary
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 informationPlacing Our Solar System in Context with the Spitzer Space Telescope
Placing Our Solar System in Context with the Spitzer Space Telescope Michael R. Meyer Steward Observatory, The University of Arizona D. Backman (NASA-Ames, D.P.I.), S.V.W. Beckwith (STScI), J. Bouwman
More informationA White Paper for the Astro2010 Decadal Survey Submitted to the Planetary and Star Formation Panel
Debris Disks: Signposts to planetary systems Prospects for the next decade A White Paper for the Astro2010 Decadal Survey Submitted to the Planetary and Star Formation Panel Wayne Holland, UK ATC, Royal
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 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 informationAstronomy 405 Solar System and ISM
Astronomy 405 Solar System and ISM Lecture 14 Comets February 15, 2013 Dynamics of Comet Tails Gas (ion) tails - interact with the solar wind - point away from the Sun. Dust tails - pushed by radiation
More informationSolar System. A collection of planets, asteroids, etc that are gravitationally bound to the Sun
Introduction Inventory of the Solar System Major Characteristics Distances & Timescales Spectroscopy Abundances, Rocks & Minerals Half-Life Some Definitions and Key Equations Solar System A collection
More informationObservations of exozodiacal disks. Jean-Charles Augereau LAOG, Grenoble, France. ISSI team: Exozodiacal dust diks and Darwin. Cambridge, August 2009
+ Olivier Absil Emmanuel Di Folco Hervé Beust Rémy Reche Alexander Krivov Philippe Thébault Torsten Loehne Vincent Coudé du Foresto Bertrand Menesson Pierre Kervella ISSI team: Exozodiacal dust diks and
More informationSpitzer Space Telescope Imaging of Spatially- Resolved Debris Disks. Karl Stapelfeldt Jet Propulsion Laboratory MSC d2p: Mar
Spitzer Space Telescope Imaging of Spatially- Resolved Debris Disks Karl Stapelfeldt Jet Propulsion Laboratory MSC d2p: Mar 9 2005 1 In collaboration with Jet Propulsion Laboratory: Michael Werner, Chas
More informationDETAILED MODEL OF THE EXOZODIACAL DISK OF FOMALHAUT AND ITS ORIGIN
EXOZODI project http://ipag.osug.fr/~augereau/site/ ANR_EXOZODI.html IAU Symposium 299 EXPLORING THE FORMATION AND EVOLUTION OF PLANETARY SYSTEMS Victoria, Canada 2013, June 6 DETAILED MODEL OF THE EXOZODIACAL
More informationarxiv: v1 [astro-ph] 8 Jul 2008
Dynamics of small bodies in planetary systems Mark C. Wyatt arxiv:0807.1272v1 [astro-ph] 8 Jul 2008 Institute of Astronomy, University of Cambridge, Cambridge CB3 0HA, UK wyatt@ast.cam.ac.uk The number
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 informationCurrently, the largest optical telescope mirrors have a diameter of A) 1 m. B) 2 m. C) 5 m. D) 10 m. E) 100 m.
If a material is highly opaque, then it reflects most light. absorbs most light. transmits most light. scatters most light. emits most light. When light reflects off an object, what is the relation between
More informationBeta Pictoris : Disk, comets, planet
Beta Pictoris : Disk, comets, planet Hervé Beust Institut de Planétologie et d Astrophysique de Grenoble (IPAG) 1 Outline of the talk 1. The star 2. The dust disk Clues for the presence of planets 3. The
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 informationVagabonds of the Solar System
Vagabonds of the Solar System Guiding Questions 1. How and why were the asteroids first discovered? 2. Why didn t the asteroids coalesce to form a single planet? 3. What do asteroids look like? 4. How
More information12/3/14. Guiding Questions. Vagabonds of the Solar System. A search for a planet between Mars and Jupiter led to the discovery of asteroids
Guiding Questions Vagabonds of the Solar System 1. How and why were the asteroids first discovered? 2. Why didn t the asteroids coalesce to form a single planet? 3. What do asteroids look like? 4. How
More informationOur Planetary System & the Formation of the Solar System
Our Planetary System & the Formation of the Solar System Chapters 7 & 8 Comparative Planetology We learn about the planets by comparing them and assessing their similarities and differences Similarities
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 informationDebris Disks: A Brief Observational History Thomas Oberst April 19, 2006 A671
Debris Disks: A Brief Observational History Thomas Oberst A671 Debris Disk; Artist s rendition (T. Pyle (SSC), JPL-Caltech, & NASA http://www.spitz er.caltech.edu/m edia/happenings /20051214/) Debris Disks
More informationExtrasolar Planets: Molecules and Disks
Extrasolar Planets: Molecules and Disks The basic question: Is our solar system typical of what we should affect around other stars (inhabited or not), or is it an unusual freak? One approach is to look
More informationBrooks Observatory telescope observing this week
Brooks Observatory telescope observing this week Mon. - Thurs., 7:30 9:15 PM MW, 7:30 8:45 PM TR See the class web page for weather updates. This evening s session is cancelled. Present your blue ticket
More informationWFIRST Preparatory Science (WPS) Project: The Circumstellar Environments of Exoplanet Host Stars (NNH14ZDA001N-WPS; PI: Christine Chen)
Permission to use these WFIRST CGI simulated data products and information within this document is granted under the condition that credit is given to: Charles Poteet (STScI), Christine Chen (STScI), Maxime
More informationIRS SPECTRA OF SOLAR-TYPE STARS: A SEARCH FOR ASTEROID BELT ANALOGS
IRS SPECTRA OF SOLAR-TYPE STARS: A SEARCH FOR ASTEROID BELT ANALOGS Debris disks Around Stars In our Solar System, dust is generated by collisions between larger bodies in the asteroid and Kuiper belts,
More informationSearching for Other Worlds
Searching for Other Worlds Lecture 32 1 In-Class Question What is the Greenhouse effect? a) Optical light from the Sun is reflected into space while infrared light passes through the atmosphere and heats
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 informationThe Coriolis effect. Why does the cloud spin? The Solar Nebula. Origin of the Solar System. Gravitational Collapse
Origin of the Solar System Our theory must explain the data 1. Large bodies in the Solar System have orderly motions. 2. There are two types of planets. small, rocky terrestrial planets large, hydrogen-rich
More informationThe Ecology of Stars
The Ecology of Stars We have been considering stars as individuals; what they are doing and what will happen to them Now we want to look at their surroundings And their births 1 Interstellar Matter Space
More informationAsteroids February 23
Asteroids February 23 Test 2 Mon, Feb 28 Covers 6 questions from Test 1. Added to score of Test 1 Telescopes Solar system Format similar to Test 1 Missouri Club Fri 9:00 1415 Fri, last 10 minutes of class
More information1 Solar System Debris and Formation
1 Solar System Debris and Formation Chapters 14 and 15 of your textbook Exercises: Do all Review and Discussion and all Conceptual Self-Test 1.1 Solar System Debris Asteroids small rocky bodies Most under
More informationCIRCUMSTELLAR DISKS AND OUTER PLANET FORMATION
CIRCUMSTELLAR DISKS AND OUTER PLANET FORMATION A. LECAVELIER DES ETANGS Institut d Astrophysique de Paris 98 Bld Arago, F-75014 Paris, France Abstract. The dust disk around β Pictoris must be produced
More informationPLANETARY FORMATION THEORY EXPLORING EXOPLANETS
PLANETARY FORMATION THEORY EXPLORING EXOPLANETS This is what we call planets around OTHER stars! PLANETARY FORMATION THEORY EXPLORING EXOPLANETS This is only as of June 2012. We ve found at least double
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 informationOrigin 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)
More informationThe History of the Solar System. From cloud to Sun, planets, and smaller bodies
The History of the Solar System From cloud to Sun, planets, and smaller bodies The Birth of a Star Twenty years ago, we knew of only one star with planets the Sun and our understanding of the birth of
More informationWhy are Saturn s rings confined to a thin plane? 1. Tidal forces 2. Newton s 1st law 3. Conservation of energy 4. Conservation of angular momentum
Announcements Astro 101, 12/2/08 Formation of the Solar System (text unit 33) Last OWL homework: late this week or early next week Final exam: Monday, Dec. 15, 10:30 AM, Hasbrouck 20 Saturn Moons Rings
More informationChapter 19 The Origin of the Solar System
Chapter 19 The Origin of the Solar System Early Hypotheses catastrophic hypotheses, e.g., passing star hypothesis: Star passing closely to the the sun tore material out of the sun, from which planets could
More informationExoplanets Direct imaging. Direct method of exoplanet detection. Direct imaging: observational challenges
Black body flux (in units 10-26 W m -2 Hz -1 ) of some Solar System bodies as seen from 10 pc. A putative hot Jupiter is also shown. The planets have two peaks in their spectra. The short-wavelength peak
More informationA Tale of Star and Planet Formation. Lynne Hillenbrand Caltech
A Tale of Star and Planet Formation Lynne Hillenbrand Caltech Vermeer s The Astronomer (1688) Mauna Kea (last week) photos by: Sarah Anderson and Bill Bates Context: Our Sun The Sun is a completely average
More informationWhich 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
More informationAstronomy 210 Midterm #2
Astronomy 210 Midterm #2 This Class (Lecture 27): Birth of the Solar System II Next Class: Exam!!!! 2 nd Hour Exam on Friday!!! Review Session on Thursday 12-1:30 in room 236 Solar Observing starts on
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 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 informationDebris dust tell us much about planetesimals and planets and sheds light to formation and evolution of planetary systems. KALAS et al.
Debris dust tell us much about planetesimals and planets and sheds light to formation and evolution of planetary systems KALAS et al. 2008 THE STAR Spectral type: F8 Distance : 17.4 pc Age : ~ 2 Gyr A
More informationRadioactive Dating. U238>Pb206. Halflife: Oldest earth rocks. Meteors and Moon rocks. 4.5 billion years billion years
U238>Pb206 Halflife: 4.5 billion years Oldest earth rocks 3.96 billion years Meteors and Moon rocks 4.6 billion years This is the time they solidified The solar system is older than this. Radioactive Dating
More informationGiant Planet Formation
Giant Planet Formation Overview Observations: Meteorites to Extrasolar Planets Our Solar System Dynamics Meteorites Geology Planetary composition & structure Other Stars Circumstellar disks Extrasolar
More informationScience Olympiad Astronomy C Division Event National Exam
Science Olympiad Astronomy C Division Event National Exam University of Nebraska-Lincoln May 15-16, 2015 Team Number: Team Name: Instructions: 1) Please turn in all materials at the end of the event. 2)
More informationSignatures of Planets in Spatially Unresolved Debris Disks
Signatures of Planets in Spatially Unresolved Debris Disks Amaya Moro-Martín 1,2, Sebastian Wolf 2,3 & Renu Malhotra 4 amaya@as.arizona.edu, swolf@astro.caltech.edu, renu@lpl.arizona.edu ABSTRACT Main
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 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 informationAstronomy 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
More information23.1 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
More informationPrentice Hall EARTH SCIENCE
Prentice Hall EARTH SCIENCE Tarbuck Lutgens Chapter 23 Touring Our Solar System 23.1 The Solar System The Planets: An Overview The terrestrial planets are planets that are small and rocky Mercury, Venus,
More informationExoplanets Direct imaging. Direct method of exoplanet detection. Direct imaging: observational challenges
Black body flux (in units 10-26 W m -2 Hz -1 ) of some Solar System bodies as seen from 10 pc. A putative hot Jupiter is also shown. The planets have two peaks in their spectra. The short-wavelength peak
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 informationHNRS 227 Fall 2006 Chapter 13. What is Pluto? What is a Planet? There are two broad categories of planets: Terrestrial and Jovian
Key Points of Chapter 13 HNRS 227 Fall 2006 Chapter 13 The Solar System presented by Prof. Geller 24 October 2006 Planets Mercury, Venus, Earth, Mars, Jupiter, Saturn, Uranus, Neptune Dwarf Planets Pluto,
More informationAST 101 INTRODUCTION TO ASTRONOMY SPRING MIDTERM EXAM 2 TEST VERSION 1 ANSWERS
AST 101 INTRODUCTION TO ASTRONOMY SPRING 2008 - MIDTERM EXAM 2 TEST VERSION 1 ANSWERS Multiple Choice. In the blanks provided before each question write the letter for the phrase that best answers the
More informationNature 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
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 informationToday. Solar System Formation. a few more bits and pieces. Homework due
Today Solar System Formation a few more bits and pieces Homework due Pluto Charon 3000 km Asteroids small irregular rocky bodies Comets icy bodies Formation of the Solar System How did these things come
More informationLinking 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
More informationAstronomy 1001/1005 Midterm (200 points) Name:
Astronomy 1001/1005 Midterm (00 points) Name: Instructions: Mark your answers on this test AND your bubble sheet You will NOT get your bubble sheet back One page of notes and calculators are allowed Use
More informationThe Earth-Moon system. Origin of the Moon. Mark Wyatt
Origin of the Moon Mark Wyatt The Earth-Moon system The Moon orbits the Earth at a moon = 385,000 km with an eccentricity of 0.05, inclination to ecliptic of 5 o The Earth orbits the Sun at a earth = 150,000,000
More informationOther worlds. Innumerable suns exist;
Innumerable suns exist; Other worlds innumerable earths revolve around these suns in a manner similar to the way the seven planets revolve around our Sun. Living beings inhabit these worlds. Giordano Bruno
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 informationAstronomy Wed. Oct. 6
Astronomy 301 - Wed. Oct. 6 Guest lectures, Monday and today: Prof. Harriet Dinerstein Monday: The outer planets & their moons Today: asteroids, comets, & the Kuiper Belt; formation of the Solar System
More informationSetting the Stage for Planet Formation: Grain Growth in Circumstellar Disks
Setting the Stage for Planet Formation: Grain Growth in Circumstellar Disks Leonardo Testi (European Southern Observatory) Disk Evolution From Grains to Pebbles Do we understand what we observe? Wish List
More informationPrentice Hall EARTH SCIENCE
Prentice Hall EARTH SCIENCE Tarbuck Lutgens 23.1 The Solar System The Planets: An Overview The terrestrial planets are planets that are small and rocky Mercury, Venus, Earth, and Mars. The Jovian planets
More informationAstronomy 1140 Quiz 4 Review
Astronomy 1140 Quiz 4 Review Anil Pradhan November 16, 2017 I Jupiter 1. How do Jupiter s mass, size, day and year compare to Earth s? Mass: 318 Earth masses (or about 1/1000th the mass of the Sun). Radius:
More informationWed. Aug. 30, 2017 Reading:
Wed. Aug. 30, 2017 Reading: Reading for Fri.: Wood Ch. 1 (solar system overview) Reading for Wed. Wed. Wood Ch. 6 & 8 (Asteroids & Meteorites, Solar Nebula) Reading for Fri. Sept. 8. Rozel et al. (link
More informationYoung Solar-like Systems
Young Solar-like Systems FIG.2. Panels(a),(b),and(c)show 2.9,1.3,and 0.87 mm ALMA continuum images of other panels, as well as an inset with an enlarged view of the inner 300 mas centered on the (f) show
More informationOn the direct imaging of Exoplanets. Sebastian Perez Stellar Coffee - December 2008
On the direct imaging of Exoplanets Sebastian Perez Stellar Coffee - December 2008 Outline Exoplanets overview Direct Imaging: - Observing strategy - Angular differential imaging HR8799 Fomalhaut beta
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