Theory of planet formation C. Mordasini
|
|
- Milton Clarke
- 5 years ago
- Views:
Transcription
1 Theory of planet formation C. Mordasini Kiel, Y. Alibert, W. Benz, K. Dittkrist, H. Klahr Max Planck Institute for Astronomy, Germany University of Berne, Switzerland Observatoire de Besancon, France
2 Content star formation dust & gas dynamics disk evolution collisional growth 1. Constraints on planet formation 2. Dust > Planetesimals 3. Planetesimals > Protoplanets 4. Protoplanets > Terrestrial Planets 5. Protoplanets> Giant planets 6. Planetary population synthesis planetary system
3 1. Observational constraints on planet formation
4 Centuries of solar system studies... remote observations laboratory analysis theoretical modelling in-situ measurements sample returns Benchmark for formation models: detailed constraints
5 Protoplanetary disks Decades of nearby star formation region studies various stages of star formation sizes, masses, radial structure chemical analysis of disks lifetime of disks Initial & boundary conditions
6 Example: The evolution of disks Hernandez et al NGC 2024 Trapezium IC 348 disks disappear in about 5-7 Myr NGC 2362! formation timescale for giant gaseous planets
7 15 years of exoplanet studies planets orbit a large fraction of stars (30% ++ for low mass planets) the planet population is extremely diverse! heavy elements play a role in the formation of at least the giant planets End products
8 The surprise... giant planets cannot form 455 planets... Jupiter Saturn Exoplanets have been found exactly where one did not expect to find them... Neptune Venus Earth Mars Uranus points towards a serious gap in our understanding of planet formation derived from the solar system alone!
9 Planet Formation: stages in presence of gas dust 10 7 years giant planets planetesimals protoplanets giant collisions terrestrial planets migration 10 8 years in absence of gas
10 2. Growth from dust to planetesimals
11 Classical coagulation - solids and gas do not orbit the star at the same speed! gas drag causes dust to drift towards the star! gas drag & turbulence determines the relative collision velocities maximum relative velocities? surface effects!m mm m km x 1000 x 1000 x 1000 strength regime Barrier for classical coagulation gravity regime -Drift barrier (drift timescale only 100 yr for 1 m body at 1 AU) -Fragmentation barrier (typical relative velocities for 1 m bodies lead to destructive collisions)
12 Classical coagulation fdg=1% fdg=3% fdg=1%, vf=10m/s fdg=3%, vf=30m/s Time No fragmentation Brauer et al With fragmentation
13 Alternative: The Goldreich & Ward Instability Dust settles into the midplane into a thin sheet: for sufficiently high dust concentration, could become instable to a self-gravity. (Goldreich & Ward 1973) The turbulent speed of grains must however be low to reach the necessary concentration. Vertical shear between (kepler.) dust disk and (subkepler.) gas above causes KH instabilities: stir up dust: no collapse possible. Conclusion: Turbulence prevents self gravitational formation. from Klahr al. 2008
14 Gravoturbulent planetesimal formation Dust is trapped locally in transient gas vortices in a turbulent disk and eventually becomes gravitationally bound. max(n) Johansen et al Klahr & Johansen t/(2&"!1 0 ) max(n)/n 0 max(! p /! g ) " K # f = M Hill /M Ceres!!!> t Turbulence aided growth might proceed from pebbles directly to intermediate-sized ( km) objects. Sedimentation Self!gravity 10 0!10.0! t/t orb
15 Planetesimals: Evidence for born big? Morbidelli et al The observed size frequency distribution SFD in the asteroid belt cannot be reproduced with planetesimals that grow (and fragment) starting at a small size (left). but with initial sizes between 100 and 1000 km (right).
16 3. From planetesimals to protoplanets
17 Collisional growth Gravity is now the dominant force. Still difficult to study because: - Initial conditions poorly known - how do the first planetesimals form? - large number of planetesimals to follow (no direct N body) - 10 MEarth > 10 8 rocky bodies with R=30 km - long evolution time years are equivalent to 10 7 dynamical times... - highly non-linear with complex feed-back mechanisms - growing bodies play an increasing role in the dynamics - non-trivial physics - shock waves, multi-phase fluid, fracturing, etc. Tackle with different approaches, each with + and - points.
18 Semi-analytical rate equations Rate equations: simplest possible approach. One big body & many small background planetesimals (surface density) Alibert et al ( 3 m isolation (4πr2 Σ) 2 (3M ) 1 2 Gravitational focussing! vrel key parameter. Without radial excursion, growth goes up until the isolation mass is reached: the protoplanet has accreted all planetesimals in its gravitational reach (in the feeding zone, width ca 5 Hill sphere radii) ( a ) ( 3 Σ 1AU 10gcm 2 Safronov 1969 ) 3/2 M.
19 Growth as a function of semimajor axis Mordasini et al xMMSN (!=7 g/cm 2 ) 5xMMSN Growth is faster at small distances ig. 7. Snapshots of the embryo mass (solid line) as a function of semimajor axis at four moments in time for two different solid surface densities. he dashed line is the isolation mass. The dotted line is M But stops at smaller masses. emb,0 = 0.6 M. The initial solid surface density at 1 AU is 7 g/cm 2 (left panel) and 5 g/cm 2 (right panel). It should be kept in mind that this kind of calculationno is neededgiant to generate the planet start time t start in whensitu. the embryo is put into he formation model. The real evolution of the solid core for M > 0.6 M is in general much more complex than plotted here. In this figure, we ave continued the calculations up to the isolation mass to allow comparison with other models. Quick and massive: Beyond the iceline 2.7 AU) Higher!: Protoplanets more that the massive resulting sub-population & quicker: of observablegp syntheticcores planets he results are quite similar, even if core growth proceeds at arge orbital distances somewhat faster in our model. Compared reasonably well reproduces the observed population (Paper II).
20 Monte carlo method Monte Carlo (probabilistic), particle-in-a-box (statistical); discrete (masses); adaptive (superparticles) Stirring increase of random velocities (e, i) Gas drag damping Collisions Dynamical friction energy equipartition Annulus at 1 AU 7 km initial size Dot size: total mass in size bin Color: relative random velocity v/vh (vh=" RH) Ormel et al subm.
21 Example: runaway and olig. growth -early phase: runaway growth. low random velocities fast growth big bodies decouple -later phase: oligarchic growth. big bodies heat smaller higher random velocities slower growth big bodies grow in lockstep -finally: isolation mass oligarchs separated by a few RH Ormel et al subm.
22 4. Formation of terrestrial planets
23 Terrestrial planet formation Once damping influence of the gas disk gone, eccentricity grows, and growth from Miso (oligarchs) w MEarth to final masses by giant impacts starts. Evolution until long time stable configuration is reached. Constraints (for the solar system): 1. the orbits, in particular the small eccentricities (Earth: 0.03) 2. the masse, in particular Mars small mass 3. the formation time of Earth from isotope dating ( Myr) 4. the bulk structure of the asteroid belt (no big bodies) 5. Earth relatively large water content (mass fraction 10-3 ) 6. influence from Jupiter & Saturn Method: N body simulation.
24 Solar system MEarth Excitation at MMRs Diffusion Substantial radial mixing S.N. Raymond et al. / Icarus 203 (2009) Raymond et al oligarchs + small pl. dotsize prop. M1/3 4 terrestrial planets with masses between MEarth M, Tform, ecc. and water content ok, but Mars to massive, and 3 addit. bodies Giant planets? When where? Fig. 3. Snapshots in time from a simulation with Jupiter and Saturn in 3:2 mean motion resonance (JSRES). The size of each body is proportional to its scale on the x axis). The color of each body corresponds to its water content by mass, from red (dry) to blue (5% water). Jupiter is shown as the large shown. Low eccentricity, water rich But mars too large Addit. bodies
25 Giant impacts - Impact of bodies of similar size - shaping planetary systems - formation of the Moon, composition of the Earth - blasting Mercury s mantle - making exoplanets visible... Red, yellow: mantel Dark & light blue: iron
26 5. Formation of giant planets
27 Direct collapse model Q = c s κ/πgσ 1.7 #cool!#orb GJ 758B Klahr et al. in prep Thalmann et al M: 34 MJ (10-39 MJ) Teff: K a:~55 AU e:~0.69 Allowed region Min. from Toomre criterion for grav. instability Impossible at small separations Max. from cooling criterion (#cool!#orb) Numerically demanding...
28 Core accretion model Perri & Cameron 1974, Mizuno et al. 1978, Mizuno 1980, Bodenheimer & Pollack 1986, Pollack et al. 1996, Lissauer et al Follow the growth in solids and gas of an initially small solid core (ices, rocks) surrounded by a gaseous envelope (H2 & He) in the protoplanetary disk. envelope growth: 1D structure equations (similar to stellar structure) core growth: collisional accretion of background planetesimals velocity dispersion of planetesimal is key parameter (runaway, oligarchic, orderly) 1) dr3 dm = 3 4πρ mass conservation 2) dp dm = G(m + M core) 4πr 4 hydrostatic equilibrium 3) dl dm = du dt + P dρ ρ 2 dt + ɛ acc energy conservation dt 4) dp = ad or rad energy transfer heating by infalling planetesimals
29 Accretion of gas: comparison planets are not 1D recently, 3D self-gravitating radiation hydrodynamical models of gas accretion with a realistic core size (Ayliffe & Bate 2009, Paardekooper & Mellema 2008) Ayliffe & Bate 2009 Ayliffe & Bate 2009 (3D) Papaloizou & Nelson 2005 (1D) 1D, 15 Mearth 3D, 10 Mearth 1D, 5 Mearth Consistent accretion rates in 1D and 3D
30 Jupiter in-situ formation Main model assumptions (as Pollack et al. 1996): in situ formation (no migration) standard opacities Phase I: Rapid build up of a core. Until isolation mass: Emptying planetesimal feeding zone Phase II: Slow accretion of gas and planetesimals Phase III: Runaway gas accretion at Mcore> Mcrit Mass Mass [MEarth] Total Core Envelope Phase I Phase II Phase III Disk gone Total Gas Solids 0 1e+06 2e+06 3e+06 4e+06 5e+06 6e+06 7e+06 8e+06 9e+06 Time [yr] Time [Yr] 9 Myr Radius [RJup] [Jupiter Luminosities] Luminosity [LJupiter] 100 Radius [Jupiter Radii] Total Core Capture Capture Runaway solids accretion Total Time [Yr] Runaway gas accretion e+06 1e+07 1e+08 1e+09 1e+10 Time [yr] Core e+06 1e+07 1e+08 1e+09 1e+10 Time [yr] Rapid, but not dynamic collapse Time [Yr] Slow contraction Slow cooling 10 Gyr 10 Gyr
31 Luminosities (a) Two peaks: Planetesimal accretion Fi of m ac in al ru lo tim is Lissauer et al L L=10 Sun Gas runaway accretion L= LSun T= yrs!"#$%&$'%&'()*'+%,-%&./#/*,' 0123"%4/5&6 Constrains dm/dt (b) Klahr & Kley 2006 Hot blob around the planet Size: few RH: AU (1 MJ,5 AU) Temp K Detectable in the mid-ir Might also cast shadows Fig. 13. Model DR: temperature in the midplane of the protoplanetary disk after 121 orbits. Brightness corresponds to the logarithm of tem- Wolf 2008 Fig. 8. The planet s luminosity as a function of time is shown for all of the runs which resulted in planets of mass equal to that of Jupiter. Diamonds denote bifurcaformation. We conclude that at least for the time when Jupiter is accreting its mass there can be no formation of a satellite!"#$ tion times. (a) The companion to Figs. 4 and 5, shows data from five pre-bifurcation system. runs as thick solid lines and post-bifurcation results from selected cases in high %&&'(#)"*$ viscosity disks as narrow lines. (b) The companion to Figs. 6 and 7, shows the post4. Conclusions +(,)"*$$$$$$$$$$$$ bifurcation luminosity of nine runs that produce planets of mass 1M J. Note in all We have performed full 3D radiation hydrodynamical simucases the steep increase in luminosity as the rate of gas accretion accelerates after lations of embedded protoplanets in disks, and compare the -'".*/$#0($ results in detail to the standard isothermal approach. crossover; this is a real physical consequence of the core nucleated accretion model Mean torques and migration rates are not strongly af12-*(# fected by the treatment of the thermodynamics in the case of of giant planet formation. The value at which luminosity peaks depends upon the Jupiter mass planets. This might change for lower mass planplanetary mass at which disk hydrodynamics begins to limit the rate of mass acets, which are more embedded in the disk. The fluctuations of 23""'78/.#4*' the torques on the other hand are much stronger, in particucretion, and thus on the viscosity and surface density of the disk in the vicinity of lar in higher resolution cases. Similar effects have been ob9/%$)(&*77' the planet. Those simulations in which accretion of gas is tapered off exhibit a corserved in high resolution nested grid simulations (D Angelo et al. 2002, 2003b) and also MHD simulations of planet-disk :/5.%;* "3$-$4$ responding taper in luminosity; the curve for run 3lRH J is probably most realistic, interactions (Papaloizou & Nelson 2003; Nelson & Papaloizou 2003; Winters et al. 2003). In some cases the torques even4-.')$/)56$7)#0$ as this run has!"#$%& the most plausible treatment of the tail off in gas accretion. (For in!"'#$%& change their sign for a short period. terpretation of the references to color in this figure legend, the reader is referred to -*$(89(//(/$ We find that planets are most likely to form a circumplane- H. Klahr and W. Kley: 3D-radiation hydro simulations of disk-planet interactions. I $m si p d p w n to ru o fo to d in th h ev p re p ex al
32 Extending the models Similar timescales of various processes:! migration "! formation #! disk evolution & extend model to include in a self consistent way (Alibert, Mordasini, Benz 2004) 1) type I and type II planetary migration (Lin & Papaloizou 86; Ward 97; Tanaka et al. 02). Isothermal Type I reduced by constant factor f1 (free parameter). Currently working on eliminating f1 (Dittkrist et al. in prep). 2) disk evolution (1+1 D) %-disk with photoevaporation (Papaloizou & Terquem 1999), now also with irradiation from the host star (Fouchet et al. submitted). Simplifications (most important) One embryo per disk, no systems (including Nbody also work in progress) Formation only until the gas disk disappears: No mass growth/loss after disk dispersal (Terrestrial planets, Ice giants, evaporating planets) No eccentricity, planets on circular orbits No particular stopping mechanism, amin=0.1 AU
33 Models meet observations Jupiter slow type I fast type I species measured computed Alibert et al. 2005b Saturn species measured computed
34 Migration and planetesimal disk ~100km accretion ejection Kalas et al Iceline Migration path Inner edge of FZ Outer edge of FZ Log(Planetesimal surface density) Paardekooper Mellema 2004 Planet shapes the planetesimal disk: effect on the dust
35 Migration and gas disk Disk accretion rate (Msun/yr) Start of runaway gas accreation Planet migration path Accretion onto the planet strongly influences the evolution of the gas disk itself
36 Gap formation 3 4 H + 50 R H qr 1 Crida et al Gap opening & gap width constrains disk and planetary properties (mp, scale height H, viscosity) Kley & Dirksen 2006 Gap formation crucial for -accretion rate -migration rate (type I vs II) Wolf & Klahr 2008 Σ t = M_jup 2 M_jup 3 M_jup 4 M_jup 5 M_jup r Large scale signs of planetdisk interaction also visible outside the gap (density waves of a Jupiter mass planet) in scattered light (VIS, near IR).
37 Gaps and accretion rates Lubow et al Kley & Dirksen 2006 Accretion Rate Transition See also Papaloizou et al Gap reduces accretion rate > 1 MJ Veras & Armitage 2004 ( Mp ) ( 1/ e M p ) 1.5M J +0.04, M J Sufficiently massive Planet Mass planets [M star ] (>3-5 MJ): sudden transition of Mass accretion rate onto planet the disk state from circular to increases strongly again. eccentric. More massive planets Limits to 6-10 MJ Detectable?
38 Gaps and migration rates Migration rates change by 1-2 orders of magnitude from type I to type II Type I: Planets seem to migrate so fast that within the disk s lifetime they fall into the star disk lifetimes (Ward 1997) simple linear theory for isothermal disks cannot be the final word!
39 Migration: Beyond linear models... 1) Turbulence in disk (Nelson & Papaloizou 2003) 2) Opacity transition regions (Menou & Goodman 2004) 3) Radiation effects (Paardekooper & Mellema 2008; Kley & Crida 2008, Kley, Bitsch & Klahr 2009, Paardekooper et al. 2009) 4) Dead zones (Ida & Lin 2008; Terquem 2008) Need observational guidance and tests Disk structure matters a lot!
40 6. Planetary population synthesis
41 Principle Extended core accretion model Formation model tested in the Solar System (Alibert, Mordasini, Benz 2004) Initial Conditions: Probability distributions & parameters Disk gas mass Disk dust mass Disk lifetime Mordasini et al. 2009a Mordasini et al. 2009b From observations red line shows the total number of known extrasolar planetary compan Observed population No match: improve, change parameters Draw and compute synthetic planet population Apply observational detection bias Comparison: Observable sub-population - Distribution of semi-major axis - Distribution of masses - Fraction of hot/cold Jupiters - Metallicity effect Match Cross check Couple to other detection methods Predictions (going back to the full synthetic population) Model solution found!
42 Initial conditions Some can be constrained by observations, some from theoretical arguments and some are just educated guesses. Four Monte Carlo variables with probability distributions Dust-to-gas ratio (solid surface density). Derived from observed (stellar) metallicities. Initial gas surface density. Derived from observed protoplanetary (dust) disk masses. Photoevaporation rate. Derived from observed lifetime distribution of protplanetary disks. Initial semimajor axis of the small planetary seed put into the disk. Uniform in log(a). Parameters (fixed for one synthetic population) Type I migration rate reduction factor f1 Disk viscosity parameter % (0.007) Planetesimal size (R=100 km) Initial solid surface distribution (! r -3/2 ) Stellar mass
43 : Planetary formation tracks Mstar=1 M" Nominal model f1=0.001 Time Mass Starting mass Mordasini, Alibert, Benz, 2009 Mordasini, Alibert, Benz, Naef 2009 Semi-major axis
44 Synthetic Population Nominal Model: alpha= 7x10-3, f1=0.001, M=1 M" Text Mordasini et al. 2009a The variation of the initial conditions within the observed limits (protoplanetary disk properties) produces synthetic planets of a very large diversity. Planets that reached inner boarder of computational disk A number of clusters can be identified. Iceline clump Planetary desert Failed cores Fig. 14. Final mass M versus final distance a of all N synt synthetic planets of the planetary population orbiting G type stars using the parameters and distributions described in 3 (α = , f I = 0.001). The feeding limit at a touch is plotted as dashed line. Planets migrating into
45 Planetary Initial Mass Function PIMF Mordasini et al. 2009b Peak at low masses Neptunian Bump Minimum: Planetary desert Flat Giant s Plateau Superjupiter Tail MStar=1 MSun Nominal Model Type Mass (MEarth) % (Super)-Earth < 7 58 Neptunian Intermediate Jovian Super-Jupiter > Model incompleteness Complex structure, dominated by low mass planets Consistent w. non-detection of Jupiters around 90-95% stars. Maxima at masses similar to Solar System planets. Model predicts that planets with M < 30 MEarth account for over 75% of all planets
46 PIMF: Dependence on disk properties Metallicity Disk Low mass mass Disk lifetime planets Udry, Mayor, Benz et al Observation Weak metallicity effect for Neptunes Fe/H mainly just scales PIMF for giant planets: Fe/H: threshold, but final mass not given by Fe/H higher number of giants but not more massive [Fe/H] dist. of Hot Neptunes: flat! [Fe/H] dist. of all known planets Disk mass changes the MF P<20 Disk d lifetime changes both. shape for giant planets. Long living disks: giants High disk mass: giant more numerous and Metal poor systems produce more small bodies planets Minimum of higher metallicity mass, effect but for Super-Earths higher & mass Neptunes less of lower mass. -Correlation with MD
47 Mass distribution Blue lines: Observational comparison sample for radial velocity Black lines: Detectable synthetic sub-population Number of Planets Planet Mass Distribution dn/dm! M Planets Keck, Lick, AAT Marcy et al Mass: KS 96% M sin i (M JUP ) The mass distribution is very well reproduced.
48 Towards the underlying mass distribution Observation Udry & Santos 2007 All instruments HARPS (1 m/s) Observational bias Synthetic 10 m/s (KS) 1m/s 0.1 m/s Full Population? Hints of the Neptunian bump and the minimum at 30 M!? If confirmed, very strong sign of c. a. Dryness of the planetary desert
49 Tasks Dust growth Break (?) the meter barrier (bouncing & fragmentation) Planetesimal formation Solved by local collapse models? (fragmentation?) Formation of giant planet cores Timescale issue Migration Realistic type I migration, incl. outward migration Planets at large distances Core accretion +... vs. direct collapse model Statistics will tell Formation of multiple planetary systems Keeping the detailled physics describing one embryo Statistics of system architectures
50 Conclusions The discovery of a whole population of exoplanets is providing important clues toward a better understanding of planet formation. -constrain formation models in a statistical sense -use the full wealth of observational data -...but don t forget the solar system. A comprehensive picture of planet formation is still beyond present capabilities: - pieces are available but don t fit well together yet... Field still observationally driven but theory beginning to be able -to make quantitative statements -to interpretate the detections -to make testable predictions Observation will remain the necessary guideline for theoretical progress. Observe directly formation (gaps, luminosity,..)!
Sta%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 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 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 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 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 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 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 informationHow do we model each process of planet formation? How do results depend on the model parameters?
How do we model each process of planet formation? How do results depend on the model parameters? Planetary Population Synthesis: The Predictive Power of Planet Formation Theory, Ringberg, Nov 29, 2010
More 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 informationObservational constraints from the Solar System and from Extrasolar Planets
Lecture 1 Part II Observational constraints from the Solar System and from Extrasolar Planets Lecture Universität Heidelberg WS 11/12 Dr. Christoph Mordasini mordasini@mpia.de Mentor Prof. T. Henning Lecture
More informationC. Mordasini & G. Bryden. Sagan Summer School 2015
Hands-on Session I C. Mordasini & G. Bryden Sagan Summer School 2015 Population synthesis Monday Tuesday Wednesday Thursday Thursday GlobalPFE model Minimum physical processes to consider GlobalPFE: Toy
More informationarxiv: v1 [astro-ph] 30 Oct 2007
**FULL TITLE** ASP Conference Series, Vol. **VOLUME**, **YEAR OF PUBLICATION** **NAMES OF EDITORS** Giant Planet Formation by Core Accretion arxiv:0710.5667v1 [astro-ph] 30 Oct 2007 Christoph Mordasini,
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 informationAccretion of Planets. Bill Hartmann. Star & Planet Formation Minicourse, U of T Astronomy Dept. Lecture 5 - Ed Thommes
Accretion of Planets Bill Hartmann Star & Planet Formation Minicourse, U of T Astronomy Dept. Lecture 5 - Ed Thommes Overview Start with planetesimals: km-size bodies, interactions are gravitational (formation
More 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 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 informationTime: a new dimension of constraints for planet formation and evolution theory
S. Jin, P. Mollière Max Planck Institut for Astronomy, Heidelberg, Germany Y. Alibert & W. Benz University of Bern, Switzerland Christoph Mordasini PLATO meeting Taormina 3.12.2014 Time: a new dimension
More informationMigration. Phil Armitage (University of Colorado) 4Migration regimes 4Time scale for massive planet formation 4Observational signatures
Phil Armitage (University of Colorado) Migration 4Migration regimes 4Time scale for massive planet formation 4Observational signatures Ken Rice (UC Riverside) Dimitri Veras (Colorado) + Mario Livio, Steve
More informationPlanet Formation. lecture by Roy van Boekel (MPIA) suggested reading: LECTURE NOTES ON THE FORMATION AND EARLY EVOLUTION OF PLANETARY SYSTEMS
Planet Formation lecture by Roy van Boekel (MPIA) suggested reading: LECTURE NOTES ON THE FORMATION AND EARLY EVOLUTION OF PLANETARY SYSTEMS by Philip J. Armitage http://arxiv.org/abs/astro-ph/0701485
More informationLecture 20: Planet formation II. Clues from Exoplanets
Lecture 20: Planet formation II. Clues from Exoplanets 1 Outline Definition of a planet Properties of exoplanets Formation models for exoplanets gravitational instability model core accretion scenario
More informationPlanet formation and (orbital) Evolution
W. Kley Planet formation and (orbital) Evolution Wilhelm Kley Institut für Astronomie & Astrophysik & Kepler Center for Astro and Particle Physics Tübingen 31. July, 2013 W. Kley Plato 2.0, ESTEC: 31.
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 informationPlanet Formation. XIII Ciclo de Cursos Especiais
Planet Formation Outline 1. Observations of planetary systems 2. Protoplanetary disks 3. Formation of planetesimals (km-scale bodies) 4. Formation of terrestrial and giant planets 5. Evolution and stability
More 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 informationDisc-Planet Interactions during Planet Formation
Disc-Planet Interactions during Planet Formation Richard Nelson Queen Mary, University of London Collaborators: Paul Cresswell (QMUL), Martin Ilgner (QMUL), Sebastien Fromang (DAMTP), John Papaloizou (DAMTP),
More informationPlanet disk interaction
Planet disk interaction Wilhelm Kley Institut für Astronomie & Astrophysik & Kepler Center for Astro and Particle Physics Tübingen March 2015 4. Planet-Disk: Organisation Lecture overview: 4.1 Introduction
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 informationGlobal models of planetary system formation. Richard Nelson Queen Mary, University of London
Global models of planetary system formation Richard Nelson Queen Mary, University of London Hot Jupiters Cold Jupiters Super-Earths/ Neptunes 2 Sumi et al (2016) Occurence rates 30-50% of FGK stars host
More informationThe theory of planet formation
The theory of planet formation Willy Benz University of Bern An incomplete and biased review Collaborators: Y. Alibert, T. Schröter, L. Fouchet, University of Bern C. Mordasini, K.M. Dittkrist, MPIA Observations
More informationHeavy meteal rules. Vardan Adibekyan Institute of Astrophysics and Space Sciences. The star-planet connection. 1 June 2015 NAOJ, Tokyo
The star-planet connection Institute of Astrophysics and Space Sciences 1 June 2015 NAOJ, Tokyo 1 Introduction to exoplanets Diversity of exoplanets Planet formation theories 2 Planet formation and metallicity
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 informationSolar System evolution and the diversity of planetary systems
Solar System evolution and the diversity of planetary systems Alessandro Morbidelli (OCA, Nice) Work in collaboration with: R. Brasser, A. Crida, R. Gomes, H. Levison, F. Masset, D. O brien, S. Raymond,
More 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 informationAccretion of Uranus and Neptune
Accretion of Uranus and Neptune by collisions among planetary embryos Jakubík M., Morbidelli A., Neslušan L., Brasser R. Astronomical Institute SAS, Tatranska Lomnica Observatoire de la Côte d Azur, Nice,
More 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 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 informationF. Marzari, Dept. Physics, Padova Univ. Planetary migration
F. Marzari, Dept. Physics, Padova Univ. Planetary migration Standard model of planet formation based on Solar system exploration Small semimajor axes Large eccentricities The standard model Protostar +Disk
More informationOverview of Planetesimal Accretion
Overview of Planetesimal Accretion German-Japanese Workshop Jena, 01.10.2010 Chris W. Ormel Max-Planck-Institute for Astronomy, Heidelberg, Germany with Kees Dullemond, Hubert Klahr, Marco Spaans MPIA
More informationPLANETARY MIGRATION A. CRIDA
PLANETARY MIGRATION A. CRIDA (the migration of Jupiter carrying its satellites. Alegory.) 1 INTRODUCTION A planet orbiting in a protoplanetary disk launches a one-armed, spiral wake. Ωp star planet Orange
More informationExtrasolar planet population synthesis
Astronomy & Astrophysics manuscript no. aamontecarloivarxiv c ESO 2018 August 24, 2018 Extrasolar planet population synthesis IV. Correlations with disk metallicity, mass and lifetime C. Mordasini 1, Y.
More informationPLANETARY MIGRATION A. CRIDA
PLANETARY MIGRATION A. CRIDA (the migration of Jupiter carrying its satellites. Alegory.) 1 INTRODUCTION A planet orbiting in a protoplanetary disk launches a one-armed, spiral wake. p star planet Orange
More informationTerrestrial planet formation: planetesimal mixing KEVIN WALSH (SWRI)
Terrestrial planet formation: planetesimal mixing KEVIN WALSH (SWRI) Questions How are terrestrial planets put together? Where do they get their material? Questions How are terrestrial planets put together?
More informationarxiv: v1 [astro-ph.ep] 18 Jul 2013
Astronomy & Astrophysics manuscript no. ms c ESO 23 July 9, 23 arxiv:37.4864v [astro-ph.ep] 8 Jul 23 Theoretical models of planetary system formation: mass vs semi-major axis Y. Alibert,2, F. Carron, A.
More informationPLANETARY MIGRATION. Review presented at the Protostars & Planets VI conference in Heidelberg, september 2013 (updated).
PLANETARY MIGRATION Review presented at the Protostars & Planets VI conference in Heidelberg, september 2013 (updated). Reference : Baruteau et al. (2014) (arxiv:1312.4293) see also : https://www.youtube.com/watch?v=_hmw4lh7ioo
More informationAstronomy. Astrophysics. Extrasolar planet population synthesis. IV. Correlations with disk metallicity, mass, and lifetime
DOI: 10.1051/0004-6361/201117350 c ESO 2012 Astronomy & Astrophysics Extrasolar planet population synthesis IV. Correlations with disk metallicity, mass, and lifetime C. Mordasini 1, Y. Alibert 2,3,W.Benz
More informationDynamically Unstable Planetary Systems Emerging Out of Gas Disks
EXTREME SOLAR SYSTEMS ASP Conference Series, Vol. 398, 2008 D. Fischer, F. A. Rasio, S. E. Thorsett, and A. Wolszczan Dynamically Unstable Planetary Systems Emerging Out of Gas Disks Soko Matsumura, Edward
More 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 informationPlanetesimal Accretion
Planetesimal Accretion Chris W. Ormel Max-Planck-Institute for Astronomy, Heidelberg and Kees Dullemond, Marco Spaans MPIA + U. of Heidelberg U. of Groningen Chris Ormel: planetesimal accretion Bern 26.05.2010
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 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 informationarxiv: v1 [astro-ph.ep] 16 Apr 2009
Astronomy & Astrophysics manuscript no. CMpopulationsynth2accepted c ESO 2009 April 16, 2009 Extrasolar planet population synthesis II: Statistical comparison with observation Christoph Mordasini 1,2,
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 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 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 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 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 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 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 informationGiant Planet Formation: episodic impacts vs. gradual core growth
Giant Planet Formation: episodic impacts vs. gradual core growth C. Broeg 1, W. Benz 1, A. Reufer 1 1 University of Berne, Institute for Space and Planetary Sciences Ringberg Castle Workshop: Planetary
More informationSIMULTANEOUS FORMATION OF GIANT PLANETS
SIMULTANEOUS FORMATION OF GIANT PLANETS ANDREA FORTIER O. GUILERA, O.G. BENVENUTO, A. BRUNINI RINGBERG, 30 NOVEMBER 2010 PHYSIKALISCHES INSTITUT, UNIVERSITY OF BERN, SWITZERLAND FCAGLP, UNIVERSIDAD DE
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 informationMinimum Radii of Super-Earths: Constraints from Giant Impacts
Minimum Radii of Super-Earths: Constraints from Giant Impacts Robert A. Marcus 1,a, Dimitar Sasselov 1, Lars Hernquist 1, Sarah T. Stewart 2 1 Astronomy Department, Harvard University, Cambridge, MA 02138
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 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 informationData from: The Extrasolar Planet Encyclopaedia.
Data from: The Extrasolar Planet Encyclopaedia http://exoplanet.eu/ 2009->10 Status of Exoplanet Searches Direct Detection: 5->9 planets detected Sensitive to large planets in large orbits around faint
More informationSuper-Earths as Failed Cores in Orbital Migration Traps
Super-Earths as Failed Cores in Orbital Migration Traps Yasuhiro Hasegawa (Jet Propulsion Laboratory, California Institute of Technology) Hasegawa 2016, ApJ, 832, 83 Copyright 2017. All rights reserved.
More 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 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 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 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 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 informationTHE ORIGIN OF HEAVY ELEMENT CONTENT TREND IN GIANT PLANETS VIA CORE ACCRETION
Draft version July 17, 2018 Preprint typeset using L A TEX style emulateapj v. 12/16/11 THE ORIGIN OF HEAVY ELEMENT CONTENT TREND IN GIANT PLANETS VIA CORE ACCRETION Yasuhiro Hasegawa 1, Geoffrey Bryden
More informationplanet migration driven by a planetesimal disk Solar System & extra solar planets: evidence for/against planet migration?
2 planet migration driven by a gas disk: type I & type II planet migration driven by a planetesimal disk Solar System & extra solar planets: evidence for/against planet migration? 3 Type I migration: follow
More informationDynamical water delivery: how Earth and rocky exoplanets get wet
Dynamical water delivery: how Earth and rocky exoplanets get wet Sean Raymond Laboratoire d Astrophysique de Bordeaux with Andre Izidoro and Alessandro Morbidelli Is Earth dry or wet? Surface water = 1
More informationarxiv: v1 [astro-ph.ep] 17 May 2017
Astronomy & Astrophysics manuscript no. ms c ESO 2017 May 18, 2017 The maximum mass of planetary embryos formed in core-accretion models Y. Alibert 1 arxiv:1705.06008v1 [astro-ph.ep] 17 May 2017 Physikalisches
More informationFormation, Orbital and Internal Evolutions of Young Planetary Systems
Accepted for publication in Space Science Reviews Formation, Orbital and Internal Evolutions of Young Planetary Systems Clément Baruteau Xuening Bai Christoph Mordasini Paul Mollière arxiv:1604.07558v1
More informationForming terrestrial planets & impacts
Lecture 11 Forming terrestrial planets & impacts Lecture Universität Heidelberg WS 11/12 Dr. C. Mordasini Based partially on script of Prof. W. Benz Mentor Prof. T. Henning Lecture 11 overview 1. Terrestrial
More informationFormation of Planets around M & L dwarfs
Formation of Planets around & L dwarfs D.N.C. Lin University of California with S. Ida, H. Li, S.L.Li, E. Thommes, I. Dobbs-Dixon, S.T. Lee,P. Garaud,. Nagasawa AAS Washington Jan 11th, 006 17 slides Disk
More informationImportance of the study of extrasolar planets. Exoplanets Introduction. Importance of the study of extrasolar planets
Importance of the study of extrasolar planets Exoplanets Introduction Planets and Astrobiology (2017-2018) G. Vladilo Technological and scientific spin-offs Exoplanet observations are driving huge technological
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 informationOrigin of high orbital eccentricity and inclination of asteroids
Earth Planets Space, 53, 85 9, 2 Origin of high orbital eccentricity and inclination of asteroids Makiko Nagasawa, Shigeru Ida, and Hidekazu Tanaka Department of Earth and Planetary Sciences, Tokyo Institute
More informationarxiv: v2 [astro-ph.ep] 7 Aug 2015
Astronomy& Astrophysics manuscript no. Planetgrowth c ESO 205 August, 205 The growth of planets by pebble accretion in evolving protoplanetary discs Bertram Bitsch, Michiel Lambrechts, and Anders Johansen
More informationLecture Outlines. Chapter 15. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 15 Astronomy Today 8th Edition Chaisson/McMillan Chapter 15 Exoplanets Units of Chapter 15 15.1 Modeling Planet Formation 15.2 Solar System Regularities and Irregularities 15.3
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 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 informationPLANET-DISC INTERACTIONS and EARLY EVOLUTION of PLANETARY SYSTEMS
PLANET-DISC INTERACTIONS and EARLY EVOLUTION of PLANETARY SYSTEMS C. Baruteau, A. Crida, B. Bitsch, J. Guilet, W. Kley, F. Masset, R. Nelson, S-J. Paardekooper, J. Papaloizou INTRODUCTION Planets form
More 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 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 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 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 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 informationMinimum Mass Solar Nebulae, Nice model, & Planetary Migration.
Minimum Mass Solar Nebulae, Nice model, & Planetary Migration. Aurélien CRIDA 1) MMSN : definition, recipe Minimum Mass Solar Nebula Little reminder : It is not a nebula, but a protoplanetary disc. Solar
More informationOn the relation between stars and their planets
On the relation between stars and their planets Nuno C. Santos Centro de Astrofísica, Universidade do Porto Instituto de Astrofísica e Ciências do Espaço Why we stellar parameters are important in exoplanets
More informationInstitute for. Advanced Study. Multi-planetary systems. Hanno of Toronto, Scarborough, March 2013
Institute for Advanced Study Multi-planetary systems Hanno Rein @University of Toronto, Scarborough, March 2013 Projects that I will not talk about today Symplectic integrators Viscous overstability Parallel
More informationComponents of Galaxies Stars What Properties of Stars are Important for Understanding Galaxies?
Components of Galaxies Stars What Properties of Stars are Important for Understanding Galaxies? Temperature Determines the λ range over which the radiation is emitted Chemical Composition metallicities
More information3D-radiation hydro simulations of disk-planet interactions. I. Numerical algorithm and test cases ABSTRACT
A&A 445, 747 758 (2006) DOI: 10.1051/0004-6361:20053238 c ESO 2005 Astronomy & Astrophysics 3D-radiation hydro simulations of disk-planet interactions I. Numerical algorithm and test cases H. Klahr 1,2
More informationTesting Theories of Planet Formation & Dynamical Evolution of Planetary Systems using Orbital Properties of Exoplanets
Testing Theories of Planet Formation & Dynamical Evolution of Planetary Systems using Orbital Properties of Exoplanets Eric B. Ford Harvard-Smithsonian Center for Astrophysics (Starting at UF in August
More informationAnders Johansen (Max-Planck-Institut für Astronomie) From Stars to Planets Gainesville, April 2007
in in (Max-Planck-Institut für Astronomie) From Stars to Planets Gainesville, April 2007 Collaborators: Hubert Klahr, Thomas Henning, Andrew Youdin, Jeff Oishi, Mordecai-Mark Mac Low in 1. Problems with
More informationKepler Planets back to the origin
Kepler Planets back to the origin Acknowledgements to the Kepler Team Yanqin Wu (Toronto) + Yoram Lithwick, James Owen, Ji-Wei Xie, Nikhil Mahajan, Bonan Pu, Ari Silburt Kepler planets: an Unexpected population
More informationarxiv:astro-ph/ v1 30 Oct 2006
Planet Formation with Migration J. E. Chambers 1 ABSTRACT arxiv:astro-ph/0610905v1 30 Oct 2006 In the core-accretion model, gas-giant planets form solid cores which then accrete gaseous envelopes. Tidal
More information