Formation of Earth- like planets -...
Transcript of Formation of Earth- like planets -...
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How do terrestrial planets like the
Earth form?
Where conditions are required to form
Earth-like planets?
What is the diversity of terrestrial
planets that can form?
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The (new) Solar System planets
Constraints: planetary masses, orbits,
compositions, spacing, isotopic ratios,
asteroid and comet populations
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Planets form in disks
around stars
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The Solar Nebula
More
volatile
“Primitive”
asteroids have
higher water
content farther
from the Sun
Raymond, Quinn & Lunine 2004;
based on Abe et al 2000
Log W
ate
r C
on
ten
t
Orbital Distance (AU)
Disk temperatureDisk temperature
profile imprintedprofile imprinted
on primitiveon primitive
bodiesbodies
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Sequence of Events in Solar System
Formation
1. Collapse of Sun and SolarNebula
2. Formation of giant planets
• Continued growth ofterrestrial bodies
3. Dispersal of gas in disk (106-7
years)
4. Final assembly of terrestrialplanets (30-50 Myr)
5. Continued dynamicalevolution of planetary system,impacts from asteroids andcomets
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Stages of Terrestrial Planet
Formation
Reviews: Lissauer 1993, Chambers 2004
1.1. Grains condense in Solar NebulaGrains condense in Solar Nebulaand settle to the disk and settle to the disk midplanemidplane(~10(~104-54-5 yrs) yrs)
2.2. ~1km ~1km ““planetesimalsplanetesimals”” form (~10 form (~1055 yrs) yrs)
3.3. Runaway and Oligarchic Growth:Runaway and Oligarchic Growth:Formation of ~Moon-Mars sizedFormation of ~Moon-Mars sized““Planetary EmbryosPlanetary Embryos”” (~10 (~105-75-7 yrs) yrs)
4.4. Late-stage Accretion of terrestrialLate-stage Accretion of terrestrialplanets from embryos (~10planets from embryos (~107-87-8 yrs) yrs)
(Giant planets form in <1-10 (Giant planets form in <1-10 MyrMyr, so, sothey affect stages 3 and 4)they affect stages 3 and 4)
Kokubo & Ida 2002E
ccen
tric
ity
Semimajor Axis
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Where did Earth get its water?
• Earth is in the “habitable zone”, where water is
liquid (hotter than 273 K = 0˚ C = 32˚ F)
• To incorporate water into Earth need icy impacts.
Water freezes at 170 K (= -100˚ C = -150˚ F)
Some of EarthSome of Earth’’s building blocks came from pasts building blocks came from past
the the ““snow linesnow line””: Earth did not form entirely from: Earth did not form entirely from
local material local material (Morbidelli et al 2000)(Morbidelli et al 2000)
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Raymond, Quinn & Lunine 2006
Snapshots in time of a high-res simulation: 1885
initial particles, Jup at 5.5 AU (eJ=0)E
ccen
tric
ity
Semimajor Axis
ab c
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Raymond, Quinn & Lunine 2006
Ecc
entr
icit
y
Semimajor Axis
Evolution of a high-res simulation: 1885
initial particles, Jup at 5.5 AU (eJ=0)
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Diversity in planetary systems like our own
Raymond,
Quinn &
Lunine 2004
Semimajor Axis (AU)
Ecc
entr
icit
y (1)
(2)
(3) (4)
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Diversity in planetary
systems like our own
(1) aJUP = 4 AU
Images from NASA
(4) Solar System
(2) MJUP = 10 MEARTH
(3) MJUP = 1/3
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Differences in Planetary Systems come
from Two Sources
1.1. Stochastic variation in the accretionStochastic variation in the accretion
process because of the small number ofprocess because of the small number of
embryos in late stagesembryos in late stages
2.2. Systematic variations among systemsSystematic variations among systems
•• Number, masses, orbits of giant planetsNumber, masses, orbits of giant planets•• Higher Higher eeJUPJUP fewer, drier terrestrial planets fewer, drier terrestrial planets
•• Higher MHigher MJUPJUP fewer, more massive terrestrial planets fewer, more massive terrestrial planets
•• Disk mass (related to stellar Disk mass (related to stellar metallicitymetallicity), disk), disk
surface density profilesurface density profile
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Eccentric giant planets form dry terrestrial planetsE
ccen
tric
ity
Semimajor Axis
eJ=0 eJ=0.1 eJ=0.2
Raymond,
Quinn &
Lunine 2004
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Could terrestrial planets exist in the known
systems of extra-solar (giant) planets?
Hot Jupiters
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Giant Planet Migration
HotHot Jupiter Jupiter
Hot Jupiters
migrated to their
current locations
because of
interactions with
the protoplanetary
disk. How does
this affect
terrestrial planet
formation?
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Raymond, Mandell &
Sigurdsson 2006
Ecc
entr
icit
y,
sin
(In
clin
ati
on
)
Log Semimajor Axis
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Raymond, Mandell &
Sigurdsson 2006
Ecc
entr
icit
y,
sin
(In
clin
ati
on
)
Log Semimajor Axis
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Credit: Nahks Tr’Enhl
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Credit: Nahks Tr’Enhl
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Can the giant planets we see tell us
something about the Earth-like
planets we can’t see?
YES.
• Giant planets form faster than terrestrial
planets
• Final stage of terrestrial planet growth is
strongly affected by gravitational influence
of giant planets
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About 1/3 of known exoplanet systems
could have formed a habitable planet
Raymond, Mandell &
Sigudsson 2006
Giant planets
outside Earth-
like planets
Giant planets interior to
Earth-like planetsGiant p
lanet too close to
HZ --
no habita
ble planets
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Diversity of habitable planetary
systems
Solar System
Computer
simulation 1
Computer
simulation 2
Computer
simulation 3
Habitable
Zone
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What might the surfaces of these
planets look like?
EarthSmall, dry
planet
Water world
Lissauer
1999
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Conclusions
Diversity of terrestrial planets, in terms of mass,
orbits, composition
Earth-like planets can form in hot Jupiter systems
but should be “water worlds”
Growth of terrestrial planets is affected by giant
planets! Can begin to predict the nature &
habitability of extrasolar terrestrial planets
Useful for upcoming missions (Kepler,
Terrestrial Planet Finder)
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How many planets are out there?
The Hubble Space
Telescope stared at
a dark patch of sky for
15 days straight
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100s of billions stars in our galaxy100s of billions stars in our galaxy
100s of billions of galaxies in the100s of billions of galaxies in the
UniverseUniverse
Probably quintillions of planetsProbably quintillions of planets
(1,000,000,000,000,000,000)(1,000,000,000,000,000,000)
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Additional Additional InformationInformation
• http://lasp.colorado.edu/~raymond
Credit: Nahks Tr’Enhl (nahks.com)
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Additional Slides
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Collaborators• Tom Quinn (Washington)
• Jonathan Lunine (Arizona)
• Avi Mandell (Penn State)
• Rory Barnes (Arizona)
• John Scalo (Texas)
• Steinn Sigurdsson (Penn St.)
• Vikki Meadows (Caltech)
• John Chambers (CIW)
• Nader Haghighipour (Hawaii)
• Nate Kaib (Washington)
• Dimitri Veras (Colorado)
Funding: Thanks to
NASA Astrobiology
Institute (thru the
Virtual Planetary
Laboratory, based
at Caltech)
Credit: Nahks Tr’Enhl
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Water content vs orbital radius
Less water
inside 2 AU
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Model for Solar System Formation
SuccessesSuccesses
•• Can roughly reproduceCan roughly reproducemasses and orbits of terrestrialmasses and orbits of terrestrialplanets with 20-1000 startingplanets with 20-1000 startingparticles particles ((Agnor Agnor et al 1999; Chambers 2001; Oet al 1999; Chambers 2001; O’’BrienBrien
et al 2006)et al 2006)
•• Asteroidal Asteroidal source explainssource explainsisotopic ratio of Earth waterisotopic ratio of Earth water((Morbidelli Morbidelli et al 2000)et al 2000)
ShortcomingsShortcomings
•• Mars is too small (unexplainedMars is too small (unexplained–– Wetherill Wetherill 19911991))
•• Mercury is too small and tooMercury is too small and tooiron-rich (giant impact? iron-rich (giant impact? Benz et alBenz et al
1988, 1988, Wetherill Wetherill 19881988))
•• Not included: Not included: collisionalcollisionalfragmentation fragmentation ((Asphaug Asphaug et al 2006),et al 2006),
water depletion from impactswater depletion from impactsand hydrodynamic escape and hydrodynamic escape (Matsui(Matsui
& Abe 1986, & Abe 1986, Canup Canup & & Pierazzo Pierazzo 2006, 2006, Genda Genda & Abe 2005)& Abe 2005)
Agnor et al 1999M
ass
(M
Eart
h)
Semimajor Axis (AU)
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Snapshots
of a sim
with giant
planet
migration
Raymond, Mandell &
Sigurdsson 2006
A “hot Earth” Ecc
entr
icit
y,
sin
(In
clin
ati
on
)
Log Semimajor Axis
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When are we going to find terrestrial
planets around other stars?
•• Ground-based radial velocities can find 3-5 MGround-based radial velocities can find 3-5 MEarthEarthplanets in HZ of K stars (Marcy group)planets in HZ of K stars (Marcy group)
•• COROT (ESA): 2006-7COROT (ESA): 2006-7–– can detect 2-3 Mcan detect 2-3 MEarthEarth planets in HZ planets in HZ
•• Kepler Kepler (NASA): 2008(NASA): 2008–– can detect Earth at 1 AUcan detect Earth at 1 AU
–– will survey 100,000 stars, expect ~50 will survey 100,000 stars, expect ~50 terrterr. planets. planets
•• SIM (NASA): 2011 (delayedSIM (NASA): 2011 (delayed……))–– 1 1 micro-arcsec astrometric micro-arcsec astrometric precision in deep modeprecision in deep mode
–– Hopes to find ~20 EarthsHopes to find ~20 Earths
•• Terrestrial Planet Finder, Darwin: 10-15 yrs (we hope)Terrestrial Planet Finder, Darwin: 10-15 yrs (we hope)–– spectra of terrestrial planets?spectra of terrestrial planets?
•• Web CashWeb Cash’’s s occulter/starshade occulter/starshade (timeline uncertain)(timeline uncertain)