e. chiang uc berkeleyw.astro.berkeley.edu/~echiang/talks/talk_argonne.pdf · 2012. 8. 13. ·...
TRANSCRIPT
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keywords:Kuiper beltdebris disks
imaging of extrasolar planetsorbit-orbit resonance
Planetary Dynamics at the Outer Limits
E. ChiangUC Berkeley
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Sample Blinking
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Sample Blinking
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KBOs = test particles
M ~ 0.1 M⊕
3 AU-3 π (100 km)2 1 km s-1
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conjunction
Neptune-Pluto Orbit-Orbit Resonance
“resonant width” Δ a resb
2.9:2
3:2 3:2
3.1:2
2.9:2
3:2
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Resonant KBOs (~26%)
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Orbital Migration by Planetesimal Ejection
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Resonance Sweeping
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Plutino (3:2) Snapshot
Wave pattern rotates rigidly with Neptune
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2:1 = Planetary Speedometer
tmigrate = 106 yrtmigrate ≡ a/(da/dt) ≥ 107 yr
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Big KBOs are excited
The Kuiper Belt: The Global View
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678130 AU67880 AU
678
70 AU
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planetary wire(secular approximation)
closed non-crossing orbits
Eccentric planet begetseccentric ring
Equilibrium belt orbitsare eccentric
and aligned withthe planet’s orbit
Fomalhaut
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planetary wire(secular approximation)
closed non-crossing orbits
Dissipative relaxation of parent bodies
onto non-crossing (forced eccentric)
orbits
Relaxation occurs during:
• Present-day collisional cascade
• Prior coagulation
Wyatt et al. 99Kalas et al. 05
eforced(a) =b(2)3/2(aplanet/a)
b(1)3/2(aplanet/a)
eplanet
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J SU
N
Lecar et al. 2001
Surface brightnessfrom Kalas et al. 05
Constraining ap and Mp
using the sharp inner belt edge
Inner belt edge =Outer edge of planet’s
“chaotic zone”
Chaotic zone width ~ (Mplanet/Mstar)2/7 aplanet
chaotic zone
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m:m
−1
m+
1:m
∆s
x
Planetary chaotic zone
= Region where first-orderresonances overlap
∆x
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conjunction #1
#2
#3
#1
Regular
Chaotic
Wisdom 1980Duncan et al. 1989
Quillen 2006#2
#3
Cha
otic
zon
e Chaotic zone
. . .
Randomwalk
in aand e
Orbit crossingand ejection
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J SU
N
Lecar et al. 2001
Surface brightnessfrom Kalas et al. 05
Constraining ap and Mp
using the sharp inner belt edge
Inner belt edge =Outer edge of planet’s
“chaotic zone”
Chaotic zone width ~ (Mplanet/Mstar)2/7 aplanet
chaotic zone
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not thermal emission from planetary atmosphere
40 RJ reflective dust disk?
Variable Hα emission?
not confirmed: only 2 epochs
Candidate planet (0.5 Jupiter mass)
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HR 8799A-type star 30-60 Myr oldwith 4 Super-Jupiters
Orbital resonances afford stabilityd:c = 2:1 resonance
Other possibilities included:c:b = 4:2:1e:d:c = 4:2:1
dynamical masses < 20 Jupitermasses each
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log(
L/L
!)
log(age/yr)
6-7MJ
7-10MJ
Cloudy spectra unlikebrown dwarfs
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Gemini Planet Imager (GPI)2012
Pan-STARRS (once a week, mag 24)
and LSST (once every few days, mag 24.5)
PS1
LSST site
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Deriving the chaotic zone width
Resonance overlap
m:m
−1
m+
1:m
∆s
x
∆s
a
∼
(
x
a
)2
Resonance spacing
then chaos
if ∆x > ∆s
i.e., if x <
(
Mp
M∗
)2/7
a
∆x
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Deriving the chaotic zone widthI. The kick at conjunction
ap
Mp
x
Ωp
= ap + x
a
2x
∆x
∆e ∼
∆v
v∼
1
v
GMp
x2∆t
∼
Mp
M∗
(
a
x
)2
x ! a
Kick in eccentricity
Kick in semimajor axis
Use Jacobi constant: CJ ≈ −GM∗
2(a + x)− Ωp
√
M∗(a + x)(1 − e2)
⇒x∆x
a2∼ (∆e)2 ⇒
∆x
a∼
(
Mp
M∗
)2(
a
x
)5
∆e
∆x
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eplanet = 0.12
ωplanet = ωbelt (nested ellipses)
aplanet = 115 AU
e.g., if
then
Mplanet = 0.5MJ
Mbelt > Mparent bodies ∼ 3M⊕
Enough material forgas giant core
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Asymmetric capture:Migration-shifted potentials
Φ
“V”
π
Direct
Indirect
∆Φ ∼
t2librate
torbitaltmigrate
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Results
If Mplanet ↑ then aplanet ↓
Planet position too farfrom dust belt
→ Mplanet < 3 MJ
Planet also evacuatesKirkwood-type gaps
Chiang et al. 2008Kalas et al. 2008
10
100
10000.3 MJ 6:5
11:95:4
9:74:3
10
100
Num
ber
of st
able
par
ent b
odie
s (in
0.1
AU
bin
s)
1 MJ
4:3 7:5
10
100
3 MJ
3:2
90 100 110 120 130 140 1501
10
100
Time-averaged semimajor axis (AU)
10 MJ
5:37:4
∴
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Results
Surface brightnessprofiles broaden too much
If Mplanet ↑ then edust ↑
→ Mplanet < 3 MJ
100 120 140 160 180 200Semimajor axis a (AU)
0.0
0.2
0.4
0.6
0.8
1.0
Rel
ativ
e
K05 model0.1 MJ, apl=120 AU0.3 MJ, apl=115.5 AU1 MJ, apl=109 AU3 MJ, apl=101.5 AU10 MJ, apl=94 AU
∴
Mbelt > Mparent bodies ∼ 3M⊕
Enough material for gas giant core
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eplanet = 0.12
ωplanet = ωbelt (nested ellipses)
aplanet = 115 AU
e.g., if
then
Mplanet = 0.5MJ
• The Kuiper belt comprises tens of thousands of icy, rocky objects having sizes greater than 100 km
• Many KBOs occupy highly eccentric and inclined orbits that imply a violent past
• Pluto and other Resonant KBOs share special gravitational relationships with Neptune
• Extrasolar debris disks are nascent Kuiper belts
• Belts are gravitationally sculpted by planets
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Fomalhaut b: Planet-Debris Disk Interaction
Step 1: Screen parent bodies for gravitational stability
tage ∼ 108 yr
t = 0Myrt = 100Myr
chaoticwidth
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Step 2: Replace parent bodies with dust grains
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Step 3: Integrate dust grains with radiative force for collisional lifetime
tcollision ∼ torb/τ ∼ 0.1 Myr
∆t = tcollision = 0.1 Myr
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Classical
Excited
1000 100 10 1
20 25 30 35-4
-2
0
2
4
6
mR
Nominal Diameter at 42 AU (km)
log
N(<
mR)
(de
g-2 )
Measured Extrapolated
Parent bodies collide once in system age
Most visible grains are just largeenough to avoid stellar blow-out
Collisional Cascade
Distribution of sizes ofKuiper belt objects
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Results
If Mplanet ↑ then aplanet ↓
Planet position too farfrom dust belt
→ Mplanet < 3 MJ
Planet also evacuatesKirkwood-type gaps
Chiang et al. 2008Kalas et al. 2008
10
100
10000.3 MJ 6:5
11:95:4
9:74:3
10
100
Num
ber
of st
able
par
ent b
odie
s (in
0.1
AU
bin
s)
1 MJ
4:3 7:5
10
100
3 MJ
3:2
90 100 110 120 130 140 1501
10
100
Time-averaged semimajor axis (AU)
10 MJ
5:37:4
∴
Mbelt > Mparent bodies ∼ 3M⊕
Enough material for gas giant core
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M∗ = 1M"
M∗ = 10M"
M∗ = 102M"
M∗ = 103M"
Measuring Debris Disk Masses
N
ssblow
∼ 0.2µm
svisible ssubmm stop
dN/ds ∝ s−q
850 µm flux consistent w/
q = 7/2(Dohnanyi)
[from tcollision(stop) ∼ tage]
stop ∼ 10 cm
∼ 100 µm
MSED(stop) ∼ 0.01M⊕
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Packed planetary systems
Packedformation
Instabilityand ejection
occurs whenplanets outweigh
parent disk
Stabilityrestored
Regularizationby dynamical
friction
Signature recorded in Kuiper belt
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Numerical simulations of packed planetary systems
Solar system-like outcomes emerge from chaos
Dynamical friction:Small bodies slow
big bodies
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Stirringof KBOs
byRogue
Ice Giants
ObservedSimulated
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Short-Period Comets
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Raising Sedna’s Periby Stellar Encounters
Typical opencluster
Before After
Fernandez & Brunini 00
Praesepe cluster M44
· n∗ ∼ 4 stars/pc3 (R1/2 ∼ 2 pc)
· t ∼ 200 Myr
· 〈v2
∗〉1/2 ∼ 1 km/s
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Discovery ofKuiper Belt Object
(KBO) #3
1992 QB1: “Smiley”
David Jewitt (U Hawaii)Jane Luu (UC Berkeley)
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Size depends on observed brightness and intrinsic reflectivity (albedo)
IxionQuaoar
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Planetary Protection Mechanism:Orbit-Orbit Resonance
Neptune makes 3 orbits
for every
2 orbits of Pluto
“Dance of the Plutinos”
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The Orbit of Sedna
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Resonant KBOs
5:1 4:1 3:1 5:2 7:3 2:1 9:5 7:40
6
12Number
5:3 8:5 3:2 10:7 7:5 11:8 4:30
40
80
Number
13:10 9:7 14:11 5:4 11:9 6:5 1:1036
Number
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2003 UB313 (mapp = 19)Diameter = 2397±100 km
vs.
PlutoDiameter = 2274 km
Palomar 48-inch / M. Brown, C. Trujillo, & D. Rabinowitz (Caltech, Yale)
Hubble Space Telescope
2003 UB313
“Xena”Bigger than Pluto
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“Santa”
“Easter Bunny”
I.A.U. definition
(a) orbits the Sun(b) hydrostatic (round) shape(c) not a satellite(d) not cleared its
neighborhood
“Dwarf Planets”
Nix
Hydra
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• The Kuiper belt comprises tens of thousands of icy, rocky objects having sizes greater than 100 km
• The Kuiper belt is the source of short-period comets
• Pluto and other Resonant KBOs share special gravitational relationships with Neptune
• Many KBOs, especially large ones, occupy highly eccentric and inclined orbits that imply a violent past
• Other star systems have their own Kuiper belts
What we know:
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1 “Large” Neptune Trojan in 60 °~10-30 Large Neptune Trojans
vs. ~1 Large Jovian Trojan
(“Large” ≡ 130-230 km diameterassuming 12-4% visual albedo)
⇒
First discovered Neptune Trojan (1:1)
Neptune
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based on Mike Brown’s survey limits:1 Earth mass at less than 200 AU1 Neptune at less than 500 AU
1 Jupiter (in reflected light) at less than 1000 AU
based on Hipparcos and Tycho-2cannot be a self-luminous main-sequence star above
the hydrogen burning limit
infrared detection of a Jupiter or brown dwarfcould be interesting
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daughter dust particle
birth ring
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Theoretical Snapshots of Resonant KBOs
•
•
Chiang & Jordan 2002
⇐ Plutinos 3:2
Twotinos 2:1 ⇒
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Observational Facts and Theoretical Deductions
1. Pluto is the largest known member of a swarm of billions of outer solar system bodies that supply
new comets.2. Pluto and the Plutinos are locked in an orbital
resonance established by Neptune.3. The orbits of many Kuiper Belt Objects are dynamically
excited.4. Pluto is not alone in having an
orbital companion.
Pluto Charon 1999 TC 36