A Framework for Atmospheric Escape from Low-Mass Planets. Ruth Murray-Clay Harvard-Smithsonian Center for Astrophysics
|
|
- Jacob Welch
- 5 years ago
- Views:
Transcription
1 A Framework for Atmospheric Escape from Low-Mass Planets Ruth Murray-Clay Harvard-Smithsonian Center for Astrophysics 1
2 hot Jupiter Mercury 0.39 AU Earth 1 AU ~0.05 AU ~ 10 R * Star Sun: LUV ~ 10-6 Lbol x10 3 during T Tauri phase planets occupy a large phase space M p,r p,a,l,l UV,,e,Ṁ w,b p initial atmosphere 2
3 Low mass gas giants and the atmospheres of solid planets can be significantly depleted Fraction of Mass Lost Over 10 Gyr planet is 0.05AU from a solar mass star ice giants gas giants Neptune 0.02 HD b super Earth Planet Mass (M J ) 3
4 Atmospheric escape is crucial to characterization of planetary atmospheres Charbonneau et al
5 Atmospheric escape is crucial to Super-Earths or mini-neptunes? characterization of planetary atmospheres Charbonneau et al
6 Atmospheric escape is crucial to characterization of planetary atmospheres Super-Earths or vs. mini-neptunes? mini-neptunes: primordial atmosphere vs. ongoing outgassing and loss Charbonneau et al
7 Two classes of escape mechanisms: Each can be thermal or non-thermal kinetic loss to space of individual atoms hydrodynamic bulk outflow of a collisional fluid exobase 5
8 Two classes of escape mechanisms: Each can be thermal or non-thermal kinetic loss to space of individual atoms hydrodynamic bulk outflow of a collisional fluid exobase Jeans escape non-thermal processes, often mediated by B-fields limits of thermal escape hydrodynamic escape Roche lobe overflow ram pressure stripping 5
9 UV photons heat the upper atmosphere by photoionization Before: After: UV photon e - collisions distribute energy from ejected electron H p + solar system planets have thermospheres heated this way 6
10 Three fates for deposited energy 1. radiated away in place 2. conducted lower in the atmosphere then radiated away 3. drives an outflow, which can be energy limited : several possible structures Difficulty: temperature and escape rate are coupled 7
11 No local energy loss Earth 10 5 Parker wind T conduction Jeans dm/dt 8
12 What generates a Parker wind? > 0: bad! fluid, isothermal hydrostatic 9
13 What generates a Parker wind? > 0: bad! fluid, isothermal accelerates the gas outward v energy for PdV work in outward flow comes from this assumption 9
14 Parker winds flow through a critical point T : sonic point: cs ~ vesc x r s = GM p /(2c 2 s) De Laval Nozzle Ṁ =4πr 2 ρv rs exponential dropoff Von Braun with the Saturn V rocket 10
15 Drop isothermal assumption still assume fluid (collisional) heating from photoionization sets lower boundary condition only photoionization heating and pdv work deposited primarily at ~ 1 : n 0 1 σh P ~ nanobars, altitude set by lower atmosphere 11
16 Jeans escape If FUV low many scale heights to sonic point; no longer collisional & model isn t self-consistent (modified) Jeans escape fluid outflow v < cs 12
17 No local energy loss Earth 10 5 Parker wind T conduction Jeans dm/dt 13
18 Conduction low UV flux regime T r Watson et al
19 No local energy loss Earth 10 5 Parker wind T conduction Jeans dm/dt 15
20 No local energy loss Earth: CO Parker wind T 10 5 Jeans conduction dm/dt 16
21 No local energy loss hot Jupiter 10 5 Parker wind T 10 4 conduction Jeans dm/dt 17
22 Radiative cooling T ~ 10^4 K EUV Ly α ~ 1 X-ray H3 + T ~ 10^3 K can kill flow altogether if too high 18
23 Mass-Loss rates remain roughly energy limited at late times for hydrogen-dominated super-earths Lyα cooling :;66!,<66*1;=0*/2367!"!$!"!#!"!!!"!"!" 9 > ">9 :*!*+ ()?@*#"9%&8A B-C01!D;1=E > ">' :*!*+ ()!" 8!" #!" $!" %!" &!" ' Energy-limited ()*+,-.*/ #
24 Three fates for deposited energy 1. conducted lower in the atmosphere then radiated away Earth and Venus 2. radiated away in place hot Jupiters orbiting T Tauri stars (in place radiation + outflow) 3. drives an outflow, which can be energy limited : several possible structures hot Jupiters; early Earth and Venus (inflated by conduction) 20
25 Summary Given UV fluxes typical of hot Jupiters orbiting Sun-like stars, atmospheric escape is ~ hydrodynamic and energy limited with r ~ Rp for observed exoplanets if they have hydrogen-dominated atmospheres, but... this need not be so for smaller planets, lower UV fluxes, higher UV fluxes, much higher X-ray fluxes, and different chemistries. Considerations: Coupling between upper and lower regions of outflow, radiative cooling, conduction, high energy spectrum, outer boundary conditions 21
Thermal Atmospheric Escape: From Jupiters to Earths
Thermal Atmospheric Escape: From Jupiters to Earths Ruth Murray-Clay University of California, Santa Barbara Image Credit: Mark Garlick Super-Earths vs. Mini Neptunes primordial hydrogen envelope accreted
More informationClose-in Planets: From Hot Jupiters to Super-Mercuries. E. Chiang (UC Berkeley)
Close-in Planets: From Hot Jupiters to Super-Mercuries E. Chiang (UC Berkeley) From exo-jupiters to exo-mars n number of planets per star 2 n R α P β (say) ln R ln P Youdin 11 Planet Counts per Star 10
More informationEvaporation of planetary atmospheres
Evaporation of planetary atmospheres Alain Lecavelier des Etangs Institut d Astrophysique de Paris Une planète s évapore Evaporation of planetary atmospheres V. Bourrier (IAP) R. Ferlet (IAP) G. Hébrard
More informationAn MHD Model for Hot Jupiter Upper Atmospheres: Mass/Angular Momentum Loss & Transits
An MHD Model for Hot Jupiter Upper Atmospheres: Mass/Angular Momentum Loss & Transits George B. Trammell University of Virginia Collaborators: Phil Arras, Zhi-Yun Li Introduction hot Jupiters M ~ MJup;
More informationPlanetary Temperatures
Planetary Temperatures How does Sunlight heat a planet with no atmosphere? This is similar to our dust grain heating problem First pass: Consider a planet of radius a at a distance R from a star of luminosity
More informationPlanetary Atmospheres
Planetary Atmospheres Structure Composition Clouds Meteorology Photochemistry Atmospheric Escape EAS 4803/8803 - CP 22:1 Where do planetary atmospheres come from? Three primary sources Primordial (solar
More informationAtmospheric escape. Volatile species on the terrestrial planets
Atmospheric escape MAVEN s Ultraviolet Views of Hydrogen s Escape from Mars Atomic hydrogen scattering sunlight in the upper atmosphere of Mars, as seen by the Imaging Ultraviolet Spectrograph on NASA's
More informationTRANSONIC HYDRODYNAMIC ESCAPE OF HYDROGEN FROM EXTRASOLAR PLANETARY ATMOSPHERES
The Astrophysical Journal, 621:1049 1060, 2005 March 10 # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. TRANSONIC HYDRODYNAMIC ESCAPE OF HYDROGEN FROM EXTRASOLAR PLANETARY
More informationPlanetary evaporation by UV and X-ray radiation: basic hydrodynamics
Mon. Not. R. Astron. Soc. 425, 2931 2947 (2012) doi:10.1111/j.1365-2966.2012.21481.x Planetary evaporation by UV and X-ray radiation: basic hydrodynamics James E. Owen 1 and Alan P. Jackson 2 1 Canadian
More informationPlanetary Atmospheres
Planetary Atmospheres Structure Composition Clouds Meteorology Photochemistry Atmospheric Escape EAS 4803/8803 - CP 11:1 Structure Generalized Hydrostatic Equilibrium P( z) = P( 0)e z # ( ) " dr / H r
More informationPlanetary Upper Atmospheres Under Strong XUV radiation
Planetary Upper Atmospheres Under Strong XUV radiation Feng Tian Laboratory for Atmosphere and Space Physics University of Colorado at Boulder March 4 th, 2010 Outline Early Solar XUV radiation was strong.
More informationHelmut Lammer Austrian Academy of Sciences, Space Research Institute Schmiedlstr. 6, A-8042 Graz, Austria (
The search of habitable Earth-like exoplanets Helmut Lammer Austrian Academy of Sciences, Space Research Institute Schmiedlstr. 6, A-8042 Graz, Austria (email: helmut.lammer@oeaw.ac.at) Graz in Space 2008
More informationPlanetary Atmospheres
Planetary Atmospheres Structure Composition Clouds Meteorology Photochemistry Atmospheric Escape EAS 4803/8803 - CP 17:1 Structure Generalized Hydrostatic Equilibrium P( z) = P( 0)e z # ( ) " dr / H r
More informationThe Sun s Influence on Planetary Atmospheres
The Sun s Influence on Planetary Atmospheres Frank Eparvier eparvier@colorado.edu University of Colorado, Laboratory for Atmospheric & Space Physics Who am I? Dr. Frank Eparvier Research Scientist @ LASP
More informationThe Earth s Hydrosphere. The volatile component of rocky planets (hydrospheres and atmospheres) Earth water reservoirs Rollins (2007)
The Earth s Hydrosphere Oceans The volatile component of rocky planets (hydrospheres and atmospheres) Planets and Astrobiology (2016-2017) G. Vladilo The Earth is the only planet of the Solar System with
More informationYes, inner planets tend to be and outer planets tend to be.
1. Planet Density Make some general comments about inner and outer planets density Inner Planets Density Outer Planets Density Is there a pattern or a trend in planet density? Yes, inner planets tend to
More informationObservational Astronomy - Lecture 6 Solar System I - The Planets
Observational Astronomy - Lecture 6 Solar System I - The Planets Craig Lage New York University - Department of Physics craig.lage@nyu.edu March 23, 2014 1 / 39 The Sun and the Earth The Sun is 23,000
More informationEarth s Atmosphere About 10 km thick
10.1 Atmospheric Basics Our goals for learning: What is an atmosphere? How does the greenhouse effect warm a planet? Why do atmospheric properties vary with altitude? Earth s Atmosphere About 10 km thick
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 informationLecture 44: The Future of Life in the Solar System
Lecture 44 The Future of Life in the Solar System Astronomy 141 Autumn 2009 This lecture is about the future of life in the Solar System. The Sun today is a steadily shining, middle-aged Main Sequence
More informationGeneral Comments about the Atmospheres of Terrestrial Planets
General Comments about the Atmospheres of Terrestrial Planets Mercury Very little atmosphere Contents: vaporized micrometeorites, solar wind Sky is black Venus Very thick (10% density of water), dense
More informationOutline. Planetary Atmospheres. General Comments about the Atmospheres of Terrestrial Planets. General Comments, continued
Outline Planetary Atmospheres Chapter 10 General comments about terrestrial planet atmospheres Atmospheric structure & the generic atmosphere Greenhouse effect Magnetosphere & the aurora Weather & climate
More informationExercise: A Toy Model for Dust-driven Winds
Astrofysikalisk dynamik, VT 00 Exercise: A Toy Model for Dust-driven Winds Susanne Höfner Department of Physics and Astronomy, Uppsala University Cool luminous giants stars, in particular pulsating AGB
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 informationLecture 5: Hydrogen Escape, Part 1
41st Saas-Fee Course From Planets to Life 3-9 April 2011 Lecture 5: Hydrogen Escape, Part 1 Prebiotic O 2 levels/ Kinetic theory of gases/ Jeans escape/ Nonthermal escape J. F. Kasting Why do we care about
More informationChallenges in Exoplanet Research for the UV
Challenges in UV Astronomy Garching 7 Oct 2013 Collaborators Catherine Huitson Exeter, UK / U of Colorado Alain Lecavelier des Etangs IAP, France Alfred Vidal-Madjar IAP, France V. Bourrier IAP, France
More informationAstro 162 Planetary Astrophysics Solution to Problem Set 3
Astro 162 Planetary Astrophysics Solution to Problem Set 3 Problem 1. Disk Heaven Consider once again the minimum-mass solar nebula, a circumstellar disk of gas and dust of solar composition orbiting the
More informationLecture 24: Saturn. The Solar System. Saturn s Rings. First we focus on solar distance, average density, and mass: (where we have used Earth units)
Lecture 24: Saturn The Solar System First we focus on solar distance, average density, and mass: Planet Distance Density Mass Mercury 0.4 1.0 0.06 Venus 0.7 0.9 0.8 Earth 1.0 1.0 1.0 Mars 1.5 0.7 0.1 (asteroid)
More informationThe Earth s Hydrosphere. The volatile component of rocky planets (hydrospheres and atmospheres) Earth water reservoirs Rollins (2007)
The Earth s Hydrosphere Oceans The volatile component of rocky planets (hydrospheres and atmospheres) Planets and Astrobiology (2017-2018) G. Vladilo The Earth is the only planet of the Solar System with
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 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 informationExample: model a star using a two layer model: Radiation starts from the inner layer as blackbody radiation at temperature T in. T out.
Next, consider an optically thick source: Already shown that in the interior, radiation will be described by the Planck function. Radiation escaping from the source will be modified because the temperature
More informationRadiation from planets
Chapter 4 Radiation from planets We consider first basic, mostly photometric radiation parameters for solar system planets which can be easily compared with existing or future observations of extra-solar
More informationStar-planet interaction and planetary characterization methods
Star-planet interaction and planetary characterization methods K. G. Kislyakova (1), H. Lammer (1), M. Holmström (2), C.P. Johnstone (3) P. Odert (4), N.V. Erkaev (5,6) (1) Space Research Institute (IWF),
More informationTransmission spectra of exoplanet atmospheres
Transmission spectra of exoplanet atmospheres David Ehrenreich Grenoble Institute of Planetology and Astrophysics (IPAG) Alain Lecavelier des Etangs (IAP) David K. Sing (U Exeter) J.-M. Désert (Harvard)
More informationDetermining the mass loss limit for close-in exoplanets: what can we learn from transit observations? ABSTRACT
A&A 506, 399 410 (2009) DOI: 10.1051/0004-6361/200911922 c ESO 2009 The CoRoT space mission: early results Astronomy & Astrophysics Special feature Determining the mass loss limit for close-in exoplanets:
More informationOur Sun. & the Planets. Sun and Planets.notebook. October 18, Our Sun (a quick review) Hydrogen is the main fuel source
Sun and Planets.notebook October 18, 2016 Our Sun Our Sun (a quick review) Average size main sequence star Hydrogen is the main fuel source In about 5 billion years it will become a & the Planets red giant
More informationSpace Science: Atmospheres Part- 7b. Venus, Earth and Mars Where is the H 2 O on Venus? Planetary Escape Isotope Fractionation Hydrodynamic Escape
Space Science: Atmospheres Part- 7b Venus, Earth and Mars Where is the H 2 O on Venus? Planetary Escape Isotope Fractionation Hydrodynamic Escape Result of Simple Model Mars The Ice Planet Water primarily
More informationSolar System Physics I
Department of Physics and Astronomy Astronomy 1X Session 2006-07 Solar System Physics I Dr Martin Hendry 6 lectures, beginning Autumn 2006 Lectures 4-6: Key Features of the Jovian and Terrestrial Planets
More informationVII. Hydrodynamic theory of stellar winds
VII. Hydrodynamic theory of stellar winds observations winds exist everywhere in the HRD hydrodynamic theory needed to describe stellar atmospheres with winds Unified Model Atmospheres: - based on the
More informationHII regions. Massive (hot) stars produce large numbers of ionizing photons (energy above 13.6 ev) which ionize hydrogen in the vicinity.
HII regions Massive (hot) stars produce large numbers of ionizing photons (energy above 13.6 ev) which ionize hydrogen in the vicinity. Detailed nebular structure depends on density distribution of surrounding
More informationThermosphere Part-3. EUV absorption Thermal Conductivity Mesopause Thermospheric Structure Temperature Structure on other planets
Thermosphere Part-3 EUV absorption Thermal Conductivity Mesopause Thermospheric Structure Temperature Structure on other planets Thermosphere Absorbs EUV Absorption: Solar Spectrum 0.2 0.6 1.0 1.4 1.8
More information9.2 - Our Solar System
9.2 - Our Solar System Scientists describe our solar system as the Sun and all the planets and other celestial objects, such as moons, comets, and asteroids, that are held by the Sun s gravity and orbit
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 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 informationCharacterizing the Atmospheres of Extrasolar Planets. Julianne I. Moses (Space Science Institute)
Characterizing the Atmospheres of Extrasolar Planets Julianne I. Moses (Space Science Institute) Intern Brown Bag, 18 June 2014 1795 Confirmed Exoplanets as of 16 June 2014 hot Jupiters Jupiter Super Earths
More informationToday. Events. Terrestrial Planet Atmospheres (continued) Homework DUE. Review next time? Exam next week
Today Terrestrial Planet Atmospheres (continued) Events Homework DUE Review next time? Exam next week Planetary Temperature A planet's surface temperature is determined by the balance between energy from
More informationThe Physics of Exoplanets
The Physics of Exoplanets Heike Rauer Institut für Planetenforschung, DLR, Berlin-Adlershof, Zentrum für Astronomie und Astrophysik, TU Berlin Formation in protoplanetary disk, migration Loss of primary,
More informationThe Sun. The Sun is a star: a shining ball of gas powered by nuclear fusion. Mass of Sun = 2 x g = 330,000 M Earth = 1 M Sun
The Sun The Sun is a star: a shining ball of gas powered by nuclear fusion. Mass of Sun = 2 x 10 33 g = 330,000 M Earth = 1 M Sun Radius of Sun = 7 x 10 5 km = 109 R Earth = 1 R Sun Luminosity of Sun =
More informationIntroduction The Role of Astronomy p. 3 Astronomical Objects of Research p. 4 The Scale of the Universe p. 7 Spherical Astronomy Spherical
Introduction The Role of Astronomy p. 3 Astronomical Objects of Research p. 4 The Scale of the Universe p. 7 Spherical Astronomy Spherical Trigonometry p. 9 The Earth p. 12 The Celestial Sphere p. 14 The
More informationArchitecture and demographics of planetary systems
Architecture and demographics of planetary systems Struve (1952) The demography of the planets that we detect is strongly affected by detection methods psychology of the observer Understanding planet demography
More informationarxiv:astro-ph/ v1 15 Dec 2003
**TITLE** ASP Conference Series, Vol. **VOLUME***, **YEAR OF PUBLICATION** **NAMES OF EDITORS** Osiris (HD209458b), an evaporating planet arxiv:astro-ph/0312382v1 15 Dec 2003 Alfred Vidal-Madjar & Alain
More informationWhat s in Our Solar System?
The Planets What s in Our Solar System? Our Solar System consists of a central star (the Sun), the main eight planets orbiting the sun, the dwarf planets, moons, asteroids, comets, meteors, interplanetary
More informationResearch paper assignment
Research paper assignment Review of research that interests you, more focused than discussions in class Include references and figures Final format should be PDF (try LaTeX!) Concise! < 5000 words Steps:
More informationPlanetary Interiors. Earth s Interior Structure Hydrostatic Equilibrium Heating Constituent Relations Gravitational Fields Isostasy Magnetism
Planetary Interiors Earth s Interior Structure Hydrostatic Equilibrium Heating Constituent Relations Gravitational Fields Isostasy Magnetism Hydrostatic Equilibrium First order for a spherical body: Internal
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 informationIcarus. Hybrid fluid/kinetic modeling of Pluto s escaping atmosphere. Justin Erwin a,, O.J. Tucker b, Robert E. Johnson a,c.
Icarus 226 (2013) 375 384 Contents lists available at SciVerse ScienceDirect Icarus journal homepage: www.elsevier.com/locate/icarus Hybrid fluid/kinetic modeling of Pluto s escaping atmosphere Justin
More informationInner Planets (Part II)
Inner Planets (Part II) Sept. 18, 2002 1) Atmospheres 2) Greenhouse Effect 3) Mercury 4) Venus 5) Mars 6) Moon Announcements Due to technical difficulties, Monday s quiz doesn t count An extra credit problem
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 informationComposition and the Early History of the Earth
Composition and the Early History of the Earth Sujoy Mukhopadhyay CIDER 2006 What we will cover in this lecture Composition of Earth Short lived nuclides and differentiation of the Earth Atmosphere and
More informationAstr 1050 Fri., Feb. 24, 2017
Astr 1050 Fri., Feb. 24, 2017 Chapter 7 & 8: Overview & Formation of the Solar System Reading: Chapters 7 on Solar System Chapter 8: Earth & Terrestrial Planets Reminders: New homework on MA up this afternoon,
More informationAST 105 Intro Astronomy The Solar System
AST 105 Intro Astronomy The Solar System STRUCTURE OF A PLANET S ATMOSPHERE If you remember this. X-rays Ultraviolet Heating & Destruction Heating & Destruction Visible Infrared Transmission and Scattering
More informationStellar Winds: Mechanisms and Dynamics
Astrofysikalisk dynamik, VT 010 Stellar Winds: Mechanisms and Dynamics Lecture Notes Susanne Höfner Department of Physics and Astronomy Uppsala University 1 Most stars have a stellar wind, i.e. and outflow
More informationAdvanced Higher Physics
Wallace Hall Academy Physics Department Advanced Higher Physics Astrophysics Problems Data Common Physical Quantities QUANTITY SYMBOL VALUE Gravitational acceleration g 9.8 m s -2 Radius of Earth R E 6.4
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 informationPractical Numerical Training UKNum
Practical Numerical Training UKNum Conclusions PD. Dr. C. Mordasini Max Planck Institute for Astronomy, Heidelberg Programm: 1) Weiterführende Vorlesungen 2) Fragebogen 3) Eigene Forschung 4) Bachelor/Masterarbeiten
More informationPlanets of the Solar System. What s Initially Available: Solar Nebula - Composition
Planets of the Solar System What s Initially Available: Solar Nebula - Composition Size versus Mass depends on composition - fight between gravity & pressure Differentiation causes the picture to be more
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 informationASTR 200 : Lecture 6 Introduction to the Solar System Pearson Education Inc., publishing as Addison-Wesley
ASTR 200 : Lecture 6 Introduction to the Solar System 1 2004 Pearson Education Inc., publishing as Addison-Wesley Comparative Planetology Studying the similarities among and differences between the planets
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 informationChapter 10 Planetary Atmospheres: Earth and the Other Terrestrial Worlds. What is an atmosphere? Earth s Atmosphere. Atmospheric Pressure
Chapter 10 Planetary Atmospheres: Earth and the Other Terrestrial Worlds 10.1 Atmospheric Basics Our goals for learning What is an atmosphere? How does the greenhouse effect warm a planet? Why do atmospheric
More informationChapter 10 Planetary Atmospheres: Earth and the Other Terrestrial Worlds
Chapter 10 Planetary Atmospheres: Earth and the Other Terrestrial Worlds 10.1 Atmospheric Basics Our goals for learning What is an atmosphere? How does the greenhouse effect warm a planet? Why do atmospheric
More informationPlanetary Atmospheres
Planetary Atmospheres Structure Composition Meteorology Clouds Photochemistry Atmospheric Escape EAS 4803/8803 - CP 20:1 Cloud formation Saturated Vapor Pressure: Maximum amount of water vapor partial
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 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 informationCosmology Vocabulary
Cosmology Vocabulary Vocabulary Words Terrestrial Planets The Sun Gravity Galaxy Lightyear Axis Comets Kuiper Belt Oort Cloud Meteors AU Nebula Solar System Cosmology Universe Coalescence Jovian Planets
More 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 informationThe Earth and Its Atmosphere: 1.Chemical composition and 2. Vertical structure
The Earth and Its Atmosphere: 1.Chemical composition and 2. Vertical structure RECAP Definition of an atmosphere: the gas surrounding a planet/satellite/comet/ Origin of the atmosphere. Three stages: I
More informationThe History of the Earth
The History of the Earth We have talked about how the universe and sun formed, but what about the planets and moons? Review: Origin of the Universe The universe began about 13.7 billion years ago The Big
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 information2.A Material sources of gas and plasma
2.A Material sources of gas and plasma The magnetosphere, extending from the top of the Saturn magnetosphere to beyond the magnetopause is dominated by neutral gas. The main components are atomic hydrogen,
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 Test Review. 3 rd Grade
Astronomy Test Review 3 rd Grade Match the vocabulary word to its definition. Outer Planets The path a planet takes around the sun. Inner Planets Orbit Sun The center of our solar system. Small, rocky
More informationExoplanet Mass, Radius, and the Search for Habitable Worlds
Sara Seager Exoplanet Mass, Radius, and the Search for Habitable Worlds O ur sun is one amongst hundreds of billions of stars in our galaxy. Based on the number of times the planetary dice must have been
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 informationTerrestrial Planetary Atmospheres
Terrestrial For the first time in my life, I saw the horizon as a curved line. It was accentuated by a thin seam of dark blue light our atmosphere. Obviously this was not the ocean of air I had been told
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 informationStar-Planet interaction
Star-Planet interaction Characterization of Exoplanet Atmosphere Magnetosphere Environments Helmut Lammer Space Research Institute, Austrian Academy of Sciences, Graz, Austria Kristina G. Kislyakova: Space
More informationAtmospheres and evaporation of extrasolar planets
Atmospheres and evaporation of extrasolar planets Alain Lecavelier des Etangs Institut d Astrophysique de Paris Une planète s évapore ESLAB ESTEC 29 mai 2007 Absorption spectroscopy during transits Light
More informationAtmosphere expansion and mass loss of close-orbit giant exoplanets heated by stellar XUV:
Atmosphere expansion and mass loss of close-orbit giant exoplanets heated by stellar XUV: II. Effects of planetary magnetic field; Structuring of inner magnetosphere M. L. Khodachenko 1,, I. F. Shaikhislamov,
More informationAnnouncements. - Homework #5 due today - Review on Monday 3:30 4:15pm in RH103 - Test #2 next Tuesday, Oct 11
Announcements - Homework #5 due today - Review on Monday 3:30 4:15pm in RH103 - Test #2 next Tuesday, Oct 11 Review for Test #2 Oct 11 Topics: The Solar System and its Formation The Earth and our Moon
More information( ) a3 (Newton s version of Kepler s 3rd Law) Units: sec, m, kg
Astronomy 18, UCSC Planets and Planetary Systems Generic Mid-Term Exam (A combination of exams from the past several times this class was taught) This exam consists of two parts: Part 1: Multiple Choice
More informationMAGNETISM QUIZ MAGNETISM
MAGNETISM QUIZ MAGNETISM 1. What force steers particles in a supercollider? A. Centrifugal B. Electric C. Magnetic D. Gravity 2. What can we learn from the paths of charged particles after a supercollider
More informationWeek 8: Stellar winds So far, we have been discussing stars as though they have constant masses throughout their lifetimes. On the other hand, toward
Week 8: Stellar winds So far, we have been discussing stars as though they have constant masses throughout their lifetimes. On the other hand, toward the end of the discussion of what happens for post-main
More informationChapter 10 Planetary Atmospheres Earth and the Other Terrestrial Worlds
Chapter 10 Planetary Atmospheres Earth and the Other Terrestrial Worlds What is an atmosphere? 10.1 Atmospheric Basics Our goals for learning:! What is an atmosphere?! How does the greenhouse effect warm
More informationThe Doppler Method, or Radial Velocity Detection of Planets: I. Technique
ASTs309L The Doppler Method, or Radial Velocity Detection of Planets: I. Technique 1. Keplerian Orbits 2. Spectrographs/Doppler shifts 3. Precise Radial Velocity measurements ASTs309L The Doppler Effect:
More informationThe Sun. How are these quantities measured? Properties of the Sun. Chapter 14
The Sun Chapter 14 The Role of the Sun in the Solar System > 99.9% of the mass Its mass is responsible for the orderly orbits of the planets Its heat is responsible for warming the planets It is the source
More informationEarth & Earthlike Planets. David Spergel
Earth & Earthlike Planets David Spergel Course Logistics Life Everywhere and Rare Earths are now in the U-Store Each precept will be divided into two teams (at this week s s precept). Debate topic: Are
More informationLabel next 2 pages in ISN Gas Giants. Make sure the following assignments are turned in:
Do Now: Label next 2 pages in ISN Gas Giants Make sure the following assignments are turned in: A3K Article Analysis Small Group Test Corrections Form (if applicable) Astronomical Bodies in The Solar System
More informationPlanetary Atmospheres. Structure Composition Clouds Photochemistry Meteorology Atmospheric Escape
Planetary Atmospheres Structure Composition Clouds Photochemistry Meteorology Atmospheric Escape Photochemistry We can characterize chemical reactions in the atmosphere in the following way: 1. Photolysis:
More information