tidal influence on orbital dynamics
DESCRIPTION
Tidal Influence on Orbital Dynamics. Dan Fabrycky ([email protected]) 4 Feb, 2010. Collaborators: Scott Tremaine Eric Johnson Jeremy Goodman Josh Winn. Photo: Stefen Seip, apod/ap040611. Orbital Distribution. Inclination to stellar equator?. get misaligned. remain aligned. - PowerPoint PPT PresentationTRANSCRIPT
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Tidal Influence on Orbital Dynamics
Dan Fabrycky
4 Feb, 2010
Collaborators:Scott TremaineEric Johnson Jeremy Goodman Josh Winn
Photo: Stefen Seip, apod/ap040611
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Orbital Distribution
Cumming+08
Hot Jupiters are a Sub-class
remain aligned
get misaligned
Inclination to stellar equator?
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Spin-orbit evolutionLorb
Hot Jupiters are spinning, gaseous bodies with oblate rotational bulges
In the star’s tidal gravitational field:
The spin vector precesses about the orbit normal
A prolate tidal bulge is raised, which tracks the star’s position
Lorb
Dissipating the energy of the tidal bulge:
the spinning planet drags prolate bulge “downstream”
i) Parallelization; || ≈105 yr
ii) Spin synchronization; s=||/2
iii) Eccentricity damping; ≈109 yr
While i, ii, or iii are ongoing, tidal heat is generated in the planet
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• Now suppose the orbital angular momentum (Lorb) precesses due to a stellar rotational bulge or another planet that is non-coplanar
• Then: tidal damping on timescale ||
produces a stable equilibrium obliquity th 0, called a Cassini state.
Cassini States
Lorb
?
I
orbit precession rate
spin precession rate
J
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Moon’s spin
Lunation: Cassini's Laws
1) Protate = Porbit
2) constant
3) , Lorb , and J are coplanar
Lorb
?
I
J
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Settling into Cassini state 2
Lorb
Oblique Pseudo-synch(Levrard et al. 2007)
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Breaking of Cassini state 2
Tidal heating ends
Lorb
[Gyr]
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‘606
Naef+01
Laughlin+09
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Planets in Binaries
On long timescales (secular approx.):
• Semimajor axis a is conserved
• e oscillates dramatically if icrit<i<180- icrit
icrit=cos-1[(3/5)1/2]=39.2
• and both vary as well
i
pericenter
~40 systems known
Orbital inclination relative to stellar equator (a.k.a. stellar obliquity):
• varies for distant planets
• constant for hot Jupiters
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Kozai Cycles
Holman, Touma, Tremaine 1997, on 16 Cyg B
Citations to Kozai 1962, a paper on asteroids
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Kozai Cycles with Tidal FrictionAdding…
• tidal effects:
time-shifted eq’m bulges
• spins:
rotational oblateness
• GR precession
Equations from:
Eggleton & Kiseleva-Eggleton, 2001
HD 80606b:
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Theory of Secular Resonance
frequency g
frequency
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i
HD 80606:
Secular Resonance during Kozai cycles with tidal friction
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Theoretical Predictions
• Disk migration
• Kozai cycles with tidal friction
• Planet-planet scattering with tidal friction
Fabrycky & Tremaine 07
Nagasawa+08
e.g., Cresswell+07
Also, resonant-pumping (Yu & Tremaine 01, Thommes & Lissauer 03)
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Do Tides Realign the Star?
Barker & Ogilvie 2009
Only if the planet is in the run-away process of being tidally consumed.
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Winn et al. 2006 HD189733b
Gaudi & Winn 2006Measuring
stellar obliquity
towards observer
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Spin-orbit observations…
(excluding WASP-3b: =1510°; Kepler-8b: =-275°)
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distributions
Two migration mechanisms? Fabrycky & Winn 2009
1-f
f
= 39 +9-6
= 0.19 +0.18-0.07
E=1.1x10-5E=34
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Topics• Spin states stabilized dynamically• Origin of hot Jupiters• Spin-orbit misalignment• Didn’t touch on:
– Tides and mean-motion resonances• Theory (Terquem & Papaloizou 2007)• 55 Cnc b-c (Novak et al. 2003)• HD 40307 (Lin et al. in prep)
– Tides and apsidal alignment• Mardling 2007, 2010• Batygin et al. 2009ab - particular systems
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Eggleton equations
hin
qin
ein
Dissipative: Non-Dissipative:
…