EXOPLANET LECTURE PLANET FORMATION. Dr. Judit Szulagyi - ETH Fellow
|
|
- Ralph Harrington
- 5 years ago
- Views:
Transcription
1 EXOPLANET LECTURE PLANET FORMATION Dr. Judit Szulagyi - ETH Fellow (judits@ethz.ch)
2 I. YOUNG STELLAR OBJECTS AND THEIR DISKS (YSOs)
3 Star Formation Young stars born in M Sun Giant Molecular Clouds. Massive clumps form in Giant Molecular Clouds, these clumps fragments into smaller cores, which then collapse and star formation begins
4
5 Spectral Energy Distribution (SED) At each wavelength, we measure the young stellar object brightness: Star is a blackbody If there is dust around it, then there is infrared excess Classification of YSOs
6 Evolutional Sequence of YSOs Envelope Envelope + disk Disk Debris disk (only dust)
7 SED components In class activity
8 In class activity
9
10
11 When do planets form? What do you think? Help: what we need to build planets?
12 Evolutional Sequence of YSOs
13 When do planets form? We need: dust (+gas for giant planets), low enough temperatures Class I and II Observations tell us: already starts within the first million year
14 Observed Planetary Mass Histogram
15 Observed Planetary Mass Histogram Lot of terrestrial planets Lot of Super-Earths/mini-Neptunes Lot of ice giants (like Neptune and Uranus) Few gas giant planets
16 Building Blocks of Planets Sticking, bouncing, fragmenting, mass-transfer, depending on the relative velocities Many problems with how to build planetesimals (very active research field currently)
17 THE TWO REGIMES: Terrestrial and Giant Planet Formation
18 Snowline Terrestrial planets (rocky, no water originally): form within snowline Giant planets (contain water): form outside the snowline
19 Snowline Easier to build larger bodies from icy objects (they stick together easier, like the wet sand on the beach) formation beyond the snowline is quicker These icy aggregates continuously migrate to the inner planetary system due to the interaction with the gas and due to the star s gravity Within the snowline: dust is dry, takes longer time to build planetesimals On the other hand: formation timescale scales with orbital timescale, therefore further away from the star the formation timescale is longer Overall still the outer planetary system is better to build building blocks continuous supply of pebbles to the inner planetary system
20 Timescale Constraints: Gaseous giant planets need gas for their formation; when gas dissipates from the disk, then giant planet formation stops (3-5 Myr) upper limit Rocky planets form mainly by collisions, they only need (dry) dust: they continue forming during the debris disk stage (Class III objects), up to ~20 Myr Probably giant planets form faster than terrestrial ones
21 TERRESTRIAL PLANET FORMATION
22 The circumstellar disk cools more dust condensates out Dust grains aggregate + stick together building up larger objects. These objects collide (and fragment), thus some become more and more massive, climbing up the size leather. These larger bodies then gravitationally attract the smaller ones around them. The region, where the planetesimal's gravity is larger than of the star's is called the Hill-sphere The feeding zone of the planetesimal is a few times of the Hill-sphere.
23 Once it accreted all the available material in the feeding zone, the embryo reaches the so called isolation mass ( M Earth in the inner disk) As the amount of gas is decreasing in the protoplanetary disk (moving toward the debris disk phase /Class III/), the collisions become more frequent among the bodies. This is when giant impacts start. Our Moon existence is a proof of this era Water delivery to Earth
24 GIANT PLANET FORMATION
25 Giant Planet Formation Scenarios Disk Instability Direct gravitational collapse Planets form like stars Probably no solid core Top-down scenario Core Accretion First a solid core forms then it accretes the gaseous envelope Bottom-up formation mechanism
26 DISK INSTABILITY
27 Gravitational Instability Massive circumstellar disk that is gravitationally unstable spiral arms form and then clumps within (((same physical mechanism that builds spiral galaxies and trigger star formation within))) These collapse into proto-planets
28 Pros and Cons + Quick ( years) + Easy to form planets far away from the star (> 30 AU) + We do observe planets even at few hundreds AU away from their star Need gravitationally unstable, massive disk which we rarely observe (probably it is not the most common formation scenario) Need short enough cooling time: clumps only collapse if they are cool Works only far away from the star (most planets we observe are within 10 AU)
29 But: planets do not necessarily form in-situ Migration: interaction with the gas, changing their orbit, usually getting closer to the star Type I: Type II:
30 But: planets do not necessarily form in-situ Planet-planet scattering: dynamical interaction between planets that can throw on planet to wider orbit or to eject from the system Free-floating planets Captured planets
31 CORE ACCRETION
32 Core Accretion Stages Pollack et al D model 3 main stages Solid core Pollack+96
33 Accretion to the planet via disk (in Phase III) Circumplanetary disk acts like a bottle-neck for accretion: slows down by a factor of 40 (Szulagyi+14) 2x10-6 M Jupiter /year: 500,000 years mass doubling time for Jupiter This is where the satellites can form
34 Pros and Cons + Works within 50 AU + Works in low-mass disks (the majority of disks we observe) Slow (couple Myrs), longer than the gaseous disk lifetime Does not work beyond 50 AU
35 Update: Pebble Accretion Accretion of cm-dm sized pebbles can enormously speed up the first (two) phases of the core accretion (in contrast to the classical, km sized planetesimals) Directly form embryos from pebbles The timescale of accretion can be shortened by a factor of at 5 AU, and at 50 AU no more timescale problem Necessities: large amount of dm sized pebbles in the midplane, km sized embryos needed as seeds These embryos can be formed e.g. by the streaming instability
36 Streaming Instability Local dust-overconcentration, that collapses into planetesimals
37 Streaming Instability Anders Johansen
38 MASTER THESIS?
39
40
41
42
43
44 Creating Scattered Light Synthetic Images of Disks with Embedded Planets You! Simulation Observation with SPHERE
Formation 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 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 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 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 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 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 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 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 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 informationChapter 15: The Origin of the Solar System
Chapter 15: The Origin of the Solar System The Solar Nebula Hypothesis Basis of modern theory of planet formation: Planets form at the same time from the same cloud as the star. Planet formation sites
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 informationRegular Features of the Solar System
1 Regular Features of the Solar System All of the planets orbit the Sun in the same plane All planetary orbits are nearly circular All planets orbit the Sun in the same direction Most planets rotate in
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 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 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 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 informationComparative Planetology II: The Origin of Our Solar System. Chapter Eight
Comparative Planetology II: The Origin of Our Solar System Chapter Eight ASTR 111 003 Fall 2007 Lecture 07 Oct. 15, 2007 Introduction To Modern Astronomy I: Solar System Introducing Astronomy (chap. 1-6)
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 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 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 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 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: v1 [astro-ph.ep] 20 Apr 2014
The Formation of Uranus & Neptune: Challenges and Implications For Intermediate-Mass Exoplanets Ravit Helled 1 and Peter Bodenheimer 2 1 Department of Geophysical, Atmospheric, and Planetary Sciences,
More informationMaking a Solar System
Making a Solar System Learning Objectives! What are our Solar System s broad features? Where are asteroids, comets and each type of planet? Where is most of the mass? In what direction do planets orbit
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 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 informationClicker Question: Clicker Question: Clicker Question:
Test results Last day to drop without a grade is Feb 29 Grades posted in cabinet and online F D C B A In which direction would the Earth move if the Sun s gravitational force were suddenly removed from
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 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 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 informationTest 2 Result: Sec 1. To see the scantron & problem set, contact the TA: Mr. He Gao
Test 2 Result: Sec 1 Column Statistics for: Test2 Count: 103 Average: 31.4 Median: 32.0 Maximum: 46.0 Minimum: 10.0 Standard Deviation: 7.94 To see the scantron & problem set, contact the TA: Mr. He Gao
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 informationHW #2. Solar Nebular Theory. Predictions: Young stars have disks. Disks contain gas & dust. Solar System should contain disk remnants
Astronomy 330: Extraterrestrial Life This class (Lecture 9): Next Class: Planet Formation Zachary Brewer Quinn Calvert Exoplanets Itamar Allali Brian Campbell-Deem HW #3 due Sunday night. Music: Another
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 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 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 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 informationStar & Planet Formation 2017 Lecture 10: Particle growth I From dust to planetesimals. Review paper: Blum & Wurm 2008 ARAA
Star & Planet Formation 2017 Lecture 10: Particle growth I From dust to planetesimals Review paper: Blum & Wurm 2008 ARAA Lecture 9: Particle motions in a gaseous disk 1. Planet formation I. From dust
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 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 informationIntroduction to Astronomy. Lecture 7: Observing Stars Star Birth, Stellar Interiors, and Stellar Evolution
Introduction to Astronomy Lecture 7: Observing Stars Star Birth, Stellar Interiors, and Stellar Evolution 1 Stars What are they? Massive gas bodies in space Generates light by fusion Defined by fusion
More informationChapter 8 Lecture. The Cosmic Perspective Seventh Edition. Formation of the Solar System
Chapter 8 Lecture The Cosmic Perspective Seventh Edition Formation of the Solar System Formation of the Solar System 8.1 The Search for Origins Our goals for learning: Develop a theory of solar system
More informationScience Skills Station
Science Skills Station Objective 1. Describe the relationship between the distance from the sun and temperature. 2. Make inferences about how temperature impacted the solar system formation. 3. Explain
More informationAnnouncements. HW #3 is Due on Thursday (September 22) as usual. Chris will be in RH111 on that day.
Announcements The Albuquerque Astronomical Society (TAAS) is hosting a public lecture SATURDAY, SEPTEMBER 17TH - 7:00pm SCIENCE AND MATH LEARNING CENTER, UNM CAMPUS Free and open to the public USA Total
More informationComparative Planetology II: The Origin of Our Solar System. Chapter Eight
Comparative Planetology II: The Origin of Our Solar System Chapter Eight ASTR 111 003 Fall 2007 Lecture 06 Oct. 09, 2007 Introduction To Modern Astronomy I: Solar System Introducing Astronomy (chap. 1-6)
More informationA star is a massive sphere of gases with a core like a thermonuclear reactor. They are the most common celestial bodies in the universe are stars.
A star is a massive sphere of gases with a core like a thermonuclear reactor. They are the most common celestial bodies in the universe are stars. They radiate energy (electromagnetic radiation) from a
More informationAstronomy 230 Section 1 MWF B6 Eng Hall. Outline. Star Formation. The Protostar Stage. Gravity, Spin, & Magnetic Fields
Astronomy 230 Section 1 MWF 1400-1450 106 B6 Eng Hall This Class (Lecture 7): Planet Formation and Next Class: Extrasolar Planets Oral Presentation Decisions! Deadline is Feb 6 th. Outline Star formation
More informationHow migrating geese and falling pens inspire planet formation
How migrating geese and falling pens inspire planet Common Seminar, Department of Astronomy and Theoretical Physics Lund University, November 2010 About me Biträdande universitetslektor (associate senior
More informationWhat does the solar system look like?
What does the solar system look like? The solar system exhibits clear patterns of composition and motion. These patterns are far more important and interesting than numbers, names, and other trivia. Relative
More informationDating the Universe. But first... Lecture 6: Formation of the Solar System. Observational Constraints. How did the Solar System Form?
Dating the Universe Lecture 6: Formation of the Solar System Astro 202 Prof. Jim Bell (jfb8@cornell.edu) Spring 2008 But first... Graded Paper 1 returned today... Paper 2 is due at beginning of class on
More informationSolar System Formation
Solar System Formation Solar System Formation Question: How did our solar system and other planetary systems form? Comparative planetology has helped us understand Compare the differences and similarities
More informationStellar Birth. Stellar Formation. A. Interstellar Clouds. 1b. What is the stuff. Astrophysics: Stellar Evolution. A. Interstellar Clouds (Nebulae)
Astrophysics: Stellar Evolution 1 Stellar Birth Stellar Formation A. Interstellar Clouds (Nebulae) B. Protostellar Clouds 2 C. Protostars Dr. Bill Pezzaglia Updated: 10/02/2006 A. Interstellar Clouds 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 informationChapter 8 Formation of the Solar System
Chapter 8 Formation of the Solar System SUMMARY OF STAGES IN FORMATION OF SOLAR SYSTEM STARTING POINT: A ROTATING SPHERICAL NEBULA with atoms made by Galactic recycling 1-GRAVITATIONAL CONTRACTION AND
More informationTopics for Today s Class
Foundations of Astronomy 13e Seeds Chapter 11 Formation of Stars and Structure of Stars Topics for Today s Class 1. Making Stars from the Interstellar Medium 2. Evidence of Star Formation: The Orion 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 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 informationUranus & Neptune: The Ice Giants. Discovery of Uranus. Bode s Law. Discovery of Neptune
Uranus & Neptune: The Ice Giants Discovery of Uranus Discovery of Uranus & Neptune Properties Density & Composition Internal Heat Source Magnetic fields Rings Uranus Rotational Axis by William Herschel
More informationSta%s%cal Proper%es of Exoplanets
Sta%s%cal Proper%es of Exoplanets Mordasini et al. 2009, A&A, 501, 1139 Next: Popula%on Synthesis 1 Goals of Population Synthesis: incorporate essential planet formation processes, with simplifying approximation
More informationOxford Research Encyclopedia of Planetary Science
Oxford Research Encyclopedia of Planetary Science Planet Formation Morris Podolak Subject: Planet Formation Online Publication Date: Apr 2018 DOI: 10.1093/acrefore/9780190647926.013.108 Summary and Keywords
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 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 informationAccretionary Disk Model
Accretionary Disk Model SOLAR NEBULAR THEORY a large cloud of gas began eventually forming the Sun at its center while the outer, cooler, parts created the planets. SOLAR NEBULA A cloud of gasses and
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 informationJupiter, Saturn, Uranus and Neptune: their formation in few million years
Jupiter, Saturn, Uranus and Neptune: their formation in few million years Omar G. Benvenuto, Andrea Fortier & Adrián Brunini Facultad de Ciencias Astronómicas y Geofísicas Universidad Nacional de La Plata
More informationPractical Numerical Training UKNum
Practical Numerical Training UKNum Conclusions Dr. H. Klahr & Dr. C. Mordasini Max Planck Institute for Astronomy, Heidelberg Programm: 1) Weiterführende Vorlesungen 2) Fragebogen 3) Eigene Forschung 4)
More informationTest 4 Final Review. 5/2/2018 Lecture 25
Test 4 Final Review 5/2/2018 Lecture 25 Apparent daily motion of celestial objects is due to earth s rotation Seasons are created due to the title of the Earth relative to the Sun Phases of the moon due
More informationFormation of the Universe
A. The Universe 1. 2. 3. How did the universe begin? Only one exists or are there more? Composed of space and 100 billion galaxies A galaxy is a grouping of millions or billions of stars kept together
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 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 information! Group project! a)! 65% b)! 70% c)! 75% d)! 80% e)! 85%
This Class (Lecture 6): More Asteroids Next Class: Dino-Killers HW1 due on Sun. Last day to go to the Nat History Building before deadline. Music: The Day Lassie Went to the Moon Camper van Beethoven!
More informationUnit 3 Lesson 2 Gravity and the Solar System. Copyright Houghton Mifflin Harcourt Publishing Company
Florida Benchmarks SC.8.N.1.4 Explain how hypotheses are valuable if they lead to further investigations, even if they turn out not to be supported by the data. SC.8.N.1.5 Analyze the methods used to develop
More informationET: Astronomy 230 Section 1 MWF Astronomy Building. Outline. Presentations. Presentations. HW #2 is due on Friday First Presentations on
This Class (Lecture 8): Planet Formation Next Class: ET: Astronomy 230 Section 1 MWF 1400-1450 134 Astronomy Building Nature of Solar Systems HW #2 is due on Friday First Presentations on 19 th and 23
More informationThe Big Bang Theory (page 854)
Name Class Date Space Homework Packet Homework #1 Hubble s Law (pages 852 853) 1. How can astronomers use the Doppler effect? 2. The shift in the light of a galaxy toward the red wavelengths is called
More informationWhy is it hard to detect planets around other stars?
Extrasolar planets Why is it hard to detect planets around other stars? Planets are small and low in mass Planets are faint The angular separation between planets and their stars is tiny Why is it hard
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 informationLecture 21 Formation of Stars November 15, 2017
Lecture 21 Formation of Stars November 15, 2017 1 2 Birth of Stars Stars originally condense out of a COLD, interstellar cloud composed of H and He + trace elements. cloud breaks into clumps (gravity)
More informationAstronomy 241: Foundations of Astrophysics I. The Solar System
Astronomy 241: Foundations of Astrophysics I. The Solar System Astronomy 241 is the first part of a year-long introduction to astrophysics. It uses basic classical mechanics and thermodynamics to analyze
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 informationGalaxies: enormous collections of gases, dust and stars held together by gravity Our galaxy is called the milky way
Celestial bodies are all of the natural objects in space ex. stars moons, planets, comets etc. Star: celestial body of hot gas that gives off light and heat the closest star to earth is the sun Planet:
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 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 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 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 information9/22/ A Brief Tour of the Solar System. Chapter 6: Formation of the Solar System. What does the solar system look like?
9/22/17 Lecture Outline 6.1 A Brief Tour of the Solar System Chapter 6: Formation of the Solar System What does the solar system look like? Our goals for learning: What does the solar system look like?
More informationTracing the origin of the Solar System. Michel Blanc OAMP, Marseille
Tracing the origin of the Solar System Michel Blanc OAMP, Marseille This talk was prepared with highly appreciated contributions from : Yann Alibert, Antonella Barucci, Willy Benz, Dominique Bockelée-Morvan,Scott
More informationInternal structure and atmospheres of planets
Internal structure and atmospheres of planets SERGEI POPOV 1312.3323 Sizes and masses Radius vs. mass Results of modeling. Old (relaxed) planets. Colors correspond to different fractions of light elements.
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 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 information4 HOW DID THE EARTH FORM?
4 HOW DID THE EARTH FORM? New stars and space debris spinning like pizza dough are a couple of the things that explain the formation of solar systems like ours. In this three-part lecture, David Christian
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 informationsee disks around new stars in Orion nebula where planets are probably being formed 3
Planet Formation contracting cloud forms stars swirling disk of material around forming star (H, He, C, O, heavier elements, molecules, dust ) form planets New born star heats up material, blows away solar
More informationSolar System Formation
Solar System Formation Solar System Formation Question: How did our solar system and other planetary systems form? Comparative planetology has helped us understand Compare the differences and similarities
More information4 HOW OUR SOLAR SYSTEM FORMED 750L
4 HOW OUR SOLAR SYSTEM FORMED 750L HOW OUR SOLAR SYSTEM FORMED A CLOSE LOOK AT THE PLANETS ORBITING OUR SUN By Cynthia Stokes Brown, adapted by Newsela Planets come from the clouds of gas and dust that
More informationAST 248, Lecture 5. James Lattimer. Department of Physics & Astronomy 449 ESS Bldg. Stony Brook University. February 6, 2015
AST 248, Lecture 5 James Lattimer Department of Physics & Astronomy 449 ESS Bldg. Stony Brook University February 6, 2015 The Search for Intelligent Life in the Universe james.lattimer@stonybrook.edu Star
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 informationAstronomy 1 Winter Lecture 11; January
Astronomy 1 Winter 2011 Lecture 11; January 31 2011 Previously on Astro-1 Properties of the Planets: Orbits in the same plane and direction Inner planets are small and made of heavy elements Outer planets
More information13 - EXTRASOLAR PLANETS
NSCI 314 LIFE IN THE COSMOS 13 - EXTRASOLAR PLANETS Dr. Karen Kolehmainen Department of Physics, CSUSB http://physics.csusb.edu/~karen/ EXTRASOLAR PLANETS? DO PLANETS ORBIT AROUND OTHER STARS? WE WOULD
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