tidal dissipation in binaries - cornell universityastro.cornell.edu/~dong/talks/tide-harvard.pdf ·...
TRANSCRIPT
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Tidal Dissipation in Binaries
March 14, 2013, Harvard ITC Colloquium
Dong Lai Cornell University
From Merging White Dwarfs to Exoplanetary Systems
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Tidal Dissipation in Binaries I. Merging White Dwarf Binaries II. Kepler Heartbeat Stars (KOI-54)
III. Exoplanetary Systems (a) Hot Jupiters (b) Host Stars
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Equilibrium Tide
M, R M’
Torque ∼ G
�M �
a3
�2
R5 k2
Q
k2 = Love Number
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Equilibrium Tide
M, R M’
Weak friction theory: ∆tlag ∼ (ω2dyntvisc)−1 = const
Torque ∼ G
�M �
a3
�2
R5 k2
Q
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Equilibrium Tide
M, R M’
Problems: -- Parameterized theory -- The physics of tidal dissipation is more complex: Excitation/damping of internal waves/modes (Dynamical Tides) -- For some applications, the parameterization is misleading
Torque ∼ G
�M �
a3
�2
R5 k2
Q
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Compact White Dwarf Binaries
-- May lead to various outcomes: R CrB stars, AM CVn, SN Ia, AIC-->NS, transients, etc
-- Gravitational waves (eLISA-NGO)
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12 min orbital period double WD eclipsing binary
Brown et al. 2011
-- Will merge in 0.9 Myr -- Large GW strain ==> eLISA -- Orbital decay measured from eclipse timing (Hermes et al. 2012)
Primary & secondary eclipses Ellipsoidal (tidal) distortion Doppler boosting
SDSS J0651+2844
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Dynamical Tides in Compact WD Binaries
Issues: -- Spin-orbit synchronization? -- Tidal dissipation and heating? -- Effect on orbital decay rate? (e.g. eLISA-NGO)
with Jim Fuller (Ph.D. 2013)
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White Dwarf Propagation Diagram
CO WD
He-core WD
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Resonant Tidal Excitation of G-modes As the orbit decays, resonance occurs when
Calculation: mode amplitude evolution + orbital evolution
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Resonant Tidal Excitation of G-modes As the orbit decays, resonance occurs when
Calculation: mode amplitude evolution + orbital evolution
Result: Surface displacement is ~ R ==> Dissipation==> No standing wave
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“Continuous” Excitation of Gravity Waves
Waves are excited in the interior/envelope, propagate outwards and dissipate near surface
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“Continuous” Excitation of Gravity Waves
Waves are excited in the interior/envelope, propagate outwards and dissipate near surface
Fuller & DL 2012
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k2
Q AA AA
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Quasi cavity
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Spin-Orbit Synchronization
1 hour
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Tidal Heating Rate
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Consequences of Tidal Heating Depend on where the heat is deposited …
If deposited in shallow layer: thermal time short ==> change Teff If deposited in deeper layer: (common: critical layer…) thermal time longer than orbital ==> Nuclear flash
Explain SDSS J0651+2844
“Tidal Nova” *
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Summary: Tides in White Dwarf Binaries
-- Dynamical tides: Continuous excitation of gravity waves, outgoing, nonlinear breaking/critical layer… -- Spin synchronized prior to merger (but not completely) -- Tidal heating important… Tidal novae
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“Heartbeat Stars” Tidally Excited Oscillations in Eccentric Binaries
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KOI-54a,b Binary A-type stars: 2.32, 2.38 Msun P=42 days, e=0.834, face-on (5.5 deg) --> At periastron:
Welsh et al 2012
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Welsh et al 2012
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Most of the observed flux variations are explained by m=0 modes (more visible for near face-on orientation)
Variations at 90,91 harmonics require very close resonances
Tidally Forced Oscillations: Flux Variations
m=2
m=0
Fuller & DL 2012
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Why N=90,91 ?
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The probability of seeing high-amplitude modes
Consider mode near resonance
• By chance likely for N=20-80 ( )
• If mode dominates tidal energy transfer
unlikely for N=90,91
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Resonance Locking
• Tidal excitation of modes ==> Orbitdal decay, spinup of star, change mode frequency
• At resonance,
• Mode can stay in resonance if or
==>
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Resonance Locking (continued)
Including intrinsic stellar spin-down torque: ===> ===> Mode can lock into resonance if
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Resonance Locking: Numerical Examples
Coupled evolution of orbit, spin and mode amplitudes…
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Resonance Locking in Both Stars
• Locking in one star:
• Similar modes are locked simultaneously in both stars
• Explain the observed N=90,91 harmonics
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Non-Linear Mode Coupling
• 9 oscillations detected at non-integer multiples of orbital frequencies • Could be produced by nonlinear coupling to daughter modes • In KOI-54,
• Other non-integer modes likely due to nonlinear coupling in which one of the daughter modes is
invisible
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Summary: Lessons from KOI-54 (Heartbeat Stars)
• Direct detection of tidally excited oscillations in eccentric binary ==> Dynamical tides at work • Resonance locking
• First direct evidence of nonlinear mode coupling
• More such systems …
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Tides in Exoplanetary Systems
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Slide from Josh Winn
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1 10 100
100
0
-100
Orbital Period [Days]
Spin
-Orb
it M
isal
ignm
ent [
Deg
rees
]
exoplanets.org | 3/10/2013
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S*-Lp misalignment in Exoplanetary Systems The Importance of few-body interactions 1. Kozai + Tide migration by a distant companion star/planet (e.g., Wu & Murray 03; Fabrycky & Tremaine 07; Naoz et al.12) 2. Planet-planet Interactions -- Strong scatterings (e.g., Rasio & Ford 96; Chatterjee et al. 08; Juric & Tremaine 08)
-- Secular interactions (“Internal Kozai”, chaos) + Tide (e.g Nagasawa et al. 08; Wu & Lithwick 11; Naoz et al.11)
Misaligned protostar - protoplanetary disk ? (e.g. Solar system) (Bate et al.2010; DL, Foucart & Lin 2011; Batygin 2012)
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Kozai Migration with Tide
m
M’
M
i Kozai (1962), Lidov (1962):
When the orbit of planet oscillates in e and I
Tidal dissipation in planet: Circluarize the orbit at small radius
(planet)
Importance of higher-order effect (Naoz et al.2011; Katz et al.2011)
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Kozai Migration with Tide
Wu & Murray 2003
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Naoz et al. 2011
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High-e Migration requires tidal dissipation in giant planets
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Tidal Q of Solar System Planets Measured/constrained by orbital evolution of their satellites (Goldreich & Soter 1966,……)
Jupiter: 6× 104 � Q � 2× 106
Q � 4× 104 (Lainey et al. 2009)
Saturn: 2× 104 � Q � 105
Q = (1− 2)× 103 (Lainey et al. 2012)
Ptide = 6.5 hr
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Theory of Tidal Q of Giant Planets
-- Viscous (turbulent) dissipation of equilibrium tide in convective envelope Q>1013
-- Gravity waves in outer radiative layer Q>1010
-- Inertial waves (Ogilvie & Lin 2004,07; Ogilvie 2009,13; Goodman & Lackner 2009)
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Inertial Waves in Rotating Fluid
Dispersion relation (in rotating frame) Can be excited if tidal forcing frequency satisfies
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Q = 105
Ogilvie & Lin 2004
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Tidal Dissipation in High-e Migration: Phenomenological Approach
Using measured Q for Jupiter (single freq), extrapolate to high-e (many frequencies) using weak friction theory: (many papers…)
∆tlag = constwith
Hot Jupiters need to be >10 times more dissipative than our Jupiter (e.g., Socrates et al 2013)
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Tidal Dissipation in Solid Core of Giant Planets with Natalia Shabaltas
Rocky/icy core: highly uncertain … Can be important if Rcore � 0.1Rp
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Shabaltas & DL 2013
k2
Q
Tidal response of Jupiter with visco-elastic core
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0.02 0.05 0.10 0.20 0.50
0.5
1.0
5.0
10.0
50.0
100.0
1!e
a" !a" weak
Orbital decay of proto hot Jupiters (visco-elastic core vs weak friction)
Shabaltas & DL 2013
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Hot Jupiter Radius Anomaly
Leconte et al. 2010
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Tidal Dissipation in Planet Host Stars:
Misalignment Damping and Survival of Hot Jupiters
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Correlation: Misalignment -- Stellar Temperature/Mass Winn et al. 2010; Schlaufman 2010
Winn et al.2010
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Albrecht, Winn, et al 2012
Correlation: Misalignment -- Stellar Temperature/Mass
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Correlation: Misalignment -- Stellar Age Triaud 2011
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Reasonable Hypothesis:
Many hot Jupiters are formed in misaligned orbits Tidal damping of misalignment (especially for cooler stars)
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Problem with Equilibrium Tide (with the parameterization…)
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Possible Solution: Different Tidal Q’s for Orbital Decay and Alignment ?
(see DL 2012)
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Tidal Forcing Frequency=? For aligned system For misaligned system
7 physically distinct components
==> Effective tidal evolution equations with 7 different Q’s
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Inertial Waves in Rotating Fluid
Dispersion relation (in rotating frame) Can only be excited if tidal forcing frequency satisfies
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Stellar Tides in Hot Jupiter Systems
For aligned system: ==> Cannot excite inertial waves
For misaligned system:
The m’=0, m=1 component has
This component leads to alignment, but not orbital decay
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Summary: Tides in Hot Jupiter Systems
Tidal dissipation in giant planets: -- Required for high-e migration -- Inertial wave excitation? -- Dissipation in solid core? Tidal dissipation in host stars: -- Spin-orbit misalignment may be damped faster than orbital decay -- Different Q’s for different processes (equilibrium tide parameterization misleading)
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Thanks !