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Course: GEL 132, Fall 2010
School: Caltech
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Caltech - GEL - 133
Characteristics of planetary candidates observed by Kepler, II: Analysisof the first four months of dataWilliam J. Borucki0,1, David G. Koch1, Gibor Basri2, Natalie Batalha3, Timothy M. Brown5,Stephen T. Bryson1, Douglas Caldwell6, Jrgen Christensen-Da
Caltech - GEL - 133
Etc. etc. etc.NPlutinos3:22:1Nrosne ceptusingscattered KBOsclassical KBOsNSJUNPPlutoUranusNeptuneSaturnJupiterAsteroid beltMarsEarthVenusMercuryPlutoEarthSaturnJupiterAsteroid beltVenusMercuryMarsUranusNeptune?Kuiper
Caltech - GEL - 133
Ge 133 Planetary Formation & EvolutionFinal ExaminationOut: 02 December 2011Due: 09 December 20111 pmThis exam has a 4-hour limit and must be completed within a single block of time.It is totally closed book, notes, friends, neighbors, internet, dog
Caltech - GEL - 133
1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T1996ApJ.460.832T
Caltech - GEL - 133
The Demographics of Extrasolar Planets Beyond theSnow Line with Ground-based Microlensing SurveysarXiv:0903.0880v1 [astro-ph.EP] 4 Mar 2009White Paper for the Astro2010 PSF Science Frontier PanelB. Scott GaudiThe Ohio State Universitygaudi@astronomy
Caltech - GEL - 133
LETTERdoi:10.1038/nature10201A low mass for Mars from Jupiters earlygas-driven migrationKevin J. Walsh1,2, Alessandro Morbidelli1, Sean N. Raymond3,4, David P. OBrien5 & Avi M. Mandell6we present a simple scenario that reflects one plausible history
Caltech - GEL - 133
c ESO 2011Astronomy & Astrophysics manuscript no. HARPSstatSeptember 13, 2011The HARPS search for southern extra-solar planetsXXXIV. Occurrence, mass distribution and orbital properties of super-Earths andNeptune-mass planetsM. Mayor1 , M. Marmier1
Caltech - GEL - 133
Draft version August 20, 2009APreprint typeset using L TEX style emulateapj v. 10/09/06INTERNATIONAL YEAR OF ASTRONOMY INVITED REVIEW ON EXOPLANETSJohn Asher Johnson1arXiv:0903.3059v1 [astro-ph.EP] 17 Mar 2009Draft version August 20, 2009ABSTRACTJ
Caltech - GEL - 133
Lecture 1 What can the solar system tell us about theformation & evolution of planetary systems?Lets consider:1. The sun.2. The major planets.3. Small bodies, including the Kuiper Beltand laboratory samples.What is the composition of the sun? Are o
Caltech - GEL - 133
Lecture 1 What can the solar system tell us about theformation & evolution of planetary systems?Lets consider:1. The sun.2. The major planets.3. Small bodies, including the Kuiper Beltand laboratory samples.What is the composition of the sun? Are o
Caltech - GEL - 133
Extrasolar planet detection:Methods and limitsGe/Ay133How do you find a planet? Look for it? Hard (as well see)!Only planet imagedis very young andfar from its star.Are such objectscommon or rare?Duquennoy & Mayor (1991) - BinariesWhere should
Caltech - GEL - 133
Extrasolar planet detection:Methods and limitsGe/Ay133How do you find a planet? Look for it? Hard (as well see)!Only planets imagedare very young andfar from their stars.Are such objectscommon or rare?Duquennoy & Mayor (1991) - BinariesWhere sh
Caltech - GEL - 133
Extrasolar planet detection:Methods and limitsGe/Ay133How do you find a planet? Look for it? Hard (as well see)!Only planets imagedare very young andfar from their stars.Are such objectscommon or rare?Duquennoy & Mayor (1991) - BinariesWhere sh
Caltech - GEL - 133
What have radial velocity surveys toldus about (exo)-planetary science?Ge/Ay133Discovery space forindirect methods:Radial velocityAstrometry(r=distance to the star)Mayor, M. & Queloz, D. 1995, Nature, 378, 355Udry, S. et al. 2002, A&A, 390, 26Jo
Caltech - GEL - 133
Extrasolar planet detection: Methods and limitsGe/Ay133Spectral Energy Distributions(or, Blinded by the light!.)How do you find a planet? Look for it? Hard (as weve seen)!Only planets imaged are very young and far from their stars. Are such objects
Caltech - GEL - 133
What have radial velocity surveys toldus about (exo)-planetary science?Ge/Ay133Discovery space forindirect methods:Radial velocityAstrometry(r=distance to the star)Mayor, M. & Queloz, D. 1995, Nature, 378, 355Udry, S. et al. 2002, A&A, 390, 26Jo
Caltech - GEL - 133
What have radial velocity surveys told us about (exo)-planetary science?Ge/Ay133Discovery space for indirect methods:Radial velocityAstrometry(r=distance to the star)Mayor, M. & Queloz, D. 1995, Nature, 378, 355Udry, S. et al. 2002, A&A, 390, 26Jo
Caltech - GEL - 133
What can transit observations tell us about (exo)-planetary science?Ge/Ay133Sometimes the absence of signal is interesting:Gilliland, R.L. et al. 2000, ApJ, 545, L47No transits in 47 Tuc, `expectation'=30-40 (34,000 stars)Transits, approach #1:Sato,
Caltech - GEL - 133
What (exo)-planetary science can bedone with microlensing?Ge/Ay133Other routes to Earth-like planets? = 4GM/bc2bMicrolensing example:Microlensing example:Best geometry uses stars at a few kpc (the lens)against the Galactic Bulge (light source).5
Caltech - GEL - 133
What (exo)-planetary science can bedone with microlensing?Ge/Ay133Other routes to Earth-like planets? = 4GM/bc2bMicrolensing example:Microlensing example:Best geometry uses stars at a few kpc (the lens)against the Galactic Bulge (light source).5
Caltech - GEL - 133
SED studies of disk lifetimes &Long wavelength studies of disksGe/Ay133Characterizinglargedisksamples?SEDModels:HH30G.J. vanZadelhoff2002Chiang &Goldreich1997IRdisk surface within several 0.1 several tens of AU(sub)mmdisk surface at large ra
Caltech - GEL - 133
SED studies of disk lifetimes &Long wavelength studies of disksGe/Ay133Characterizinglargedisksamples?SEDModels:HH30G.J. vanZadelhoff2002Chiang &Goldreich1997IRdisk surface within several 0.1 several tens of AU(sub)mmdisk surface at large ra
Caltech - GEL - 133
SED studies of disk lifetimes & Long wavelength studies of disksGe/Ay133Characterizinglargedisksamples?SEDModels:HH30G.J. van Zadelhoff 2002Chiang & Goldreich 1997IR disk surface within several 0.1 several tens of AU (sub)mm disk surface at large ra
Caltech - GEL - 133
Disk Structure and Evolution(the so-called model of disk viscosity)Ge/Ay 133Recapitulationofpassivediskstructureequations.I.Equation for hydrostatic equilibrium using only stellar gravity.For an ideal gaswhere c is the sound speed (c2 = RT).Solving
Caltech - GEL - 133
Disk Structure and Evolution(the so-called model of disk viscosity)Ge/Ay 133Recapitulationofpassivediskstructureequations.I.Equation for hydrostatic equilibrium using only stellar gravity.For an ideal gaswhere c is the sound speed (c2 = RT).Solving
Caltech - GEL - 133
How do small dust grains growin protoplanetary disks?Ge/Ay133Howdowegofromawellmixedgas/dustgraindisk:Toamatureplanetarysystem?Forsolids,itishelpfultodistinguishamongstseveralregimes:mcmkmmoon/Mars(oligarchs)110MEarthStep#1:Growthfrom~0.1mto~1cmsca
Caltech - GEL - 133
How do small dust grains grow in protoplanetary disks?Ge/Ay133Howdowegofromawellmixedgas/dustgraindisk:Toamatureplanetarysystem?Forsolids,itishelpfultodistinguishamongstseveralregimes: mcmkmmoon/Mars(oligarchs)110MEarthStep#1:Growthfrom~0.1 mto~1cmsc
Caltech - GEL - 133
How do small dust grains growin protoplanetary disks?Ge/Ay133Howdowegofromawellmixedgas/dustgraindisk:Toamatureplanetarysystem?Forsolids,itishelpfultodistinguishamongstseveralregimes:mcmkmmoon/Mars(oligarchs)110MEarthStep#1:Growthfrom~0.1mto~1cmsca
Caltech - GEL - 133
How do planetesimals grow toform ~terrestrial mass cores?Ge/Ay133Fornow,letsignorethegas.Thismeanswecanjustworryaboutgravity.Forthepairwiseinteractionoftwobodies,wehave:r=a1br=a2Forcollisionsthataregrazing,thevelocityatimpactcanbeshowntobePluggi
Caltech - GEL - 133
How do planetesimals grow to form ~terrestrial mass cores?Ge/Ay133Fornow,letsignorethegas.Thismeanswecanjustworryaboutgravity.Forthe pairwiseinteractionoftwobodies,wehave: r=a1 br=a2 Forcollisionsthataregrazing,the velocityatimpactcanbeshowntobe Pluggi
Caltech - GEL - 133
How do planetesimals grow toform ~terrestrial mass cores?Ge/Ay133Fornow,letsignorethegas.Thismeanswecanjustworryaboutgravity.Forthepairwiseinteractionoftwobodies,wehave:r=a1br=a2Forcollisionsthataregrazing,thevelocityatimpactcanbeshowntobePluggi
Caltech - GEL - 133
Jovian planet formation. Core-accretion or gravitational instability?Ge/Ay133PropertiesoftheJovianPlanetsintheSolarSystemP 2 forH2HeI/MR2=0.4forauniformsphere I/MR2=0.26forP 2Theradiusmass relationshipandM.o.I. areusedtoinferthe presenceofprimordial
Caltech - GEL - 133
Jovian planet formation. Core-accretionor gravitational instability?Ge/Ay133PropertiesoftheJovianPlanetsintheSolarSystemP2forH2HeI/MR2=0.4forauniformsphereI/MR2=0.26forP2TheradiusmassrelationshipandM.o.I.areusedtoinferthepresenceofprimordialco
Caltech - GEL - 133
Jovian planet formation. Core-accretionor gravitational instability?Ge/Ay133PropertiesoftheJovianPlanetsintheSolarSystemP2forH2HeI/MR2=0.4forauniformsphereI/MR2=0.26forP2TheradiusmassrelationshipandM.o.I.areusedtoinferthepresenceofprimordialco
Caltech - GEL - 133
What effects do 1-10 MEarth cores & Jovian planets have on the surrounding disk? Or, Migration & GapsGe/Ay133Disks can be unstable globally:Toomres criterion Q c/( G) < 1 ( axisymmetric perturbations) = epicyclic frequencyDisks can be unstable globall
Caltech - GEL - 133
What effects do 1-10 MEarth coreshave on the surrounding disk?Today = GapsWednesday = Migration (included here)Ge/Ay133Disks can be unstable globally:Toomres criterionQ c/(G) < 1( axisymmetric perturbations) = epicyclic frequencyDisks can be uns
Caltech - GEL - 133
What effects do 1-10 MEarth coreshave on the surrounding disk?Today = GapsWednesday = Migration (included here)Ge/Ay133Disks can be unstable globally:Toomres criterionQ c/(G) < 1( axisymmetric perturbations) = epicyclic frequencyDisks can be uns
Caltech - GEL - 133
What can the Kuiper belt tell usabout the early solar system?Part I (Part II next lecture)Ge/Ay133Kuipers Hypothesis (1950) Pluto should not be alone!1999 KR 16First (non-Pluto)trans-Neptunianobject found in1992 (Jewitt &Luu), now manymany hund
Caltech - GEL - 133
Can we study extrasolar Kuiper Belts? Pic, A5V starGe/Ay133AU Mic, M1Ve starImpossible to see any exo-KBOs themselves, butHow do we find debris disks?Spitzer Data (FEPS team)Model has 0.1 Mmoon of30 m size dust grainsin a disk from 3060 AUBars a
Caltech - GEL - 133
Can we study extrasolar Kuiper Belts? Pic, A5V starGe/Ay133AU Mic, M1Ve starImpossible to see any exo-KBOs themselves, butHow do we find debris disks?Spitzer Data (FEPS team)Model has 0.1 Mmoon of30 m size dust grainsin a disk from 3060 AUBars a
Caltech - GEL - 133
Can we study extrasolar Kuiper/Asteroid Belts? Pic, A5V starAU Mic, M1Ve starGe/Ay133Impossible to see any exo-KBOs themselves, butNear Earth dust source?How do we find debris disks?Spitzer Data (FEPS team) Model has 0.1 Mmoon of 30 m size dust gra
Caltech - GEL - 133
What can the asteroid belt tell us about the early S.S.?433 Eros? PhobosGe/Ay133These types are not strongly separated, radially.Comets are icy bodies that sublimate and becomeactive when close to the Sun. They are believed tooriginate in two cold
Caltech - GEL - 133
In what sort of region did our own solar system form?Ge/Ay133Inrelativeisolation(Taurus,Bokglobules,)?In what sort of environment did our own solar system form?Oraspartofarichcluster(morelikely)?Oneimportantsetofclues: Shortlivednuclidesinmeteorites
Caltech - GEL - 133
When and how did the cores of terrestrial planets form?Ge/Ay133Two end member hypotheses for core formation:Estimated core sizesof the terrestrial planets.Two end member hypotheses for core formation:Q: Why is heterogeneousaccretion unlikely?A: In
Caltech - GEL - 133
When and how did the cores of terrestrial planets form?Ge/Ay133Two end member hypotheses for core formation:Estimated core sizesof the terrestrial planets.Two end member hypotheses for core formation:Q: Why is heterogeneousaccretion unlikely?A: In
Caltech - GEL - 133
Planetary DynamicsGe/Ay133Orbital elements (3-D),& time evolution:What ARE Lyapounov exponents and times?Regular Chaotic Suppose that twoorbits are separated inphase space by d, andthat d followsd = d0 e- (t-t0)G is the Lyapounovexponent, and
Caltech - GEL - 133
Planetary DynamicsGe/Ay133Orbital elements (3-D),& time evolution:What ARE Lyapounov exponents and times?Regular Chaotic Suppose that twoorbits are separated inphase space by d, andthat d followsd = d0 e- (t-t0)G is the Lyapounovexponent, and
Caltech - GEL - 133
January 4, 2009APreprint typeset using L TEX style emulateapj v. 03/07/07MODELS OF JUPITERS GROWTH INCORPORATING THERMAL AND HYDRODYNAMIC CONSTRAINTSJack J. Lissauer, Olenka Hubickyj1 , Gennaro DAngelo2NASA Ames Research Center, Space Science and Ast
Caltech - GEL - 133
Formation of Jupiter and Conditions for Accretion of the GalileanSatellitesarXiv:0809.1418v3 [astro-ph] 16 Jan 2009P. R. Estrada, and I. MosqueiraSETI InstituteJ. J. Lissauer, G. DAngelo, and D. P. CruikshankNASA Ames Research CenterAbstractWe pre
Caltech - GEL - 133
Caltech - GEL - 133
arXiv:0811.0441v1 [astro-ph] 4 Nov 2008Introduction to Gravitational MicrolensingShude MaoJodrell Bank Centre for Astrophysics, University of Manchester, Manchester M13 9PL, UKE-mail: shude.mao@manchester.ac.ukThe basic concepts of gravitational micr
Caltech - GEL - 133
Problem Set #1Ge/Ay 133Due Thursday, 6 October 20111. Consider a planet of mass Mp that orbits a star of mass M at orbital distance a, or,more precisely, the star and the planet go around their common center of mass. For astar some R parsecs distant,
Caltech - GEL - 133
Due October 13th , 2011Ge/Ay133 Problem Set #21Angular Momenta(a) Verify eq. (1.1) (page 3) in Armitage, and use it to estimate the total angular momentum of the spinningsun, and how much angular momentum the sun would have if it were spinning on the
Caltech - GEL - 133
Ge 133 - Problem Set # 3, due Oct. 27thA) The goal of this problem is to understand Spectral Energy Distributions (SEDs), the spectra emitted bya star plus a disk. Using some simple assumptions, youll generate your own model SED. For this problem,assum
Caltech - GEL - 133
Problem set 4Ge/Ay 133Due 03 November 20111Gaps and migration(a) Large planets open gaps in disks and then become tied to the evolution of the disk. Thus,if the disk is evolving on the viscous timescale, the planet will also migrate on the viscoust
Caltech - GEL - 133
Problem set 5Ge/Ay 133Due November 10More MMSNScattering of planetesimals in the outer solar system caused the orbits of Saturn,Uranus, and Neptune to expand. Using adiabatic theory, one can show thatthe eccentricies of the KBOs grow as they are pus
Caltech - GEL - 133
Ge/Ay133 Problem Set #6Revenge of the (Geo)ChemistsDue November 17th(1) This problem is to help you think about the thermal history of bodies that are assembledin the early solar system. Information of this sort is important when thinking about the co
Caltech - GEL - 133
Ay/Ge 133 Problem Set #8Due December 1st , 2011(1) The Jeans formula governing atmospheric escape due to thermal evaporation is: = ni < v > .The ux of escaping particles where ni is the number density of the species of interest and < v >is given byG
Caltech - MS - 115a
Caltech - MS - 115a
Diffusional ProcessesPdH2cH+CO+CO2HxhydrogenseparationmembraneABt=0CACBt>0CACBinterdiffusion couple