Montana State University Dana Longcope
Transcript of Montana State University Dana Longcope
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Q: Why do the Sun and planets have magnetic fields?
Dana Longcope
Montana State University
w/ liberal “borrowing” from Bagenal, Stanley, Christensen, Schrijver, Charbonneau, …
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Q: Why do the Sun and planets have magnetic fields?
A: They all have dynamos
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•Plasma (stars)•Liquid iron (terrestrial planets)•Metallic hydrogen (gas giants)•Ionized water (ice giants)
•Complex turbulent flows•Rotation: breaks mirror-symmetry not required, but needed for large- scale, organized fields
From Stanley 2013
•Figure of merit: Magnetic Reynold’s # Rm = velocity × size × conductivity
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A Toy w/ all ingredients
motionalEMF
backEMF
Growth:
generation dissipation
Growth:
conducting fluid
multi-partconductor
complex motions
differentialmotion of parts
lack of mirror symmetry
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Fluid dynamics
Faraday’s+ Ohm’s laws
If B is weak: kinematic equations
Linear equation for B(x,t) – solve w/ known v(x,t)
Reality: Conducting fluid – MHD
Traditional (neutral) fluid – solve first
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Dynamo action in MHD
If M has a positive eigenvalue λ > 0 B can grow exponentially: DYNAMO ACTION
Growth:
• B 🡪 -B : same e-vector 🡪 same λ• Reverse velocity AND reflect in mirror 🡪 λ 🡪 λ• Do one and not the other 🡪 λ 🡪 -λ
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Q: What kind of flow has λ > 0? • Turbulent flows have pos. Lyapunov exponent: λ > 0
• tend to stretch balls into strands• tend to amplify fields
• Conditions for turbulence:• driving: e.g. Rayleigh-Taylor instability• viscosity fights driving – must be small
• Rotation can organize turbulence: align stretching direction 🡪 azimuthal (toroidal) – known as Ω-effect – must be significant w.r.t. fluid motion
η [m2/s] υ [m2/s] L [m] v [m/s] Ω [rad/s] Rm Re Ro
Sun (CZ) 1 10-2 108 1 10-6 108 1010 10-2
Earth (core) 1 10-5 106 10-4 10-4 102 107 10-6
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•Plasma (stars)•Liquid iron (terrestrial planets)•Metallic hydrogen (gas giants)•Ionized water (ice giants)
•Complex turbulent flows•Rotation: breaks mirror-symmetry not required, but needed for large- scale, organized fields
From Stanley 2013
•Figure of merit: Magnetic Reynold’s # Rm = velocity × size × conductivity
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How it works in the Sun
• Entire Star: H/He plasma• Convection Zone (CZ)
• Outer 200,000 km• Turbulence: Re = 1010
• Thermally driven• Good conductor Rm = 108
• Rotation effective Ro = 10-2
• Corona – conductive but tenuous:
J smaller (~0?)
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Evidence of the dynamo
Magnetic field where there are sunspots
Field outside sunspots and elsewhere too
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Evidence of the dynamo
Field is fibril
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Evidence of the dynamo
+
+
+(-)
(-)
(-)
Field orientation: mostly toroidal (E-W)
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Mu
noz
-Jar
amill
o le
ctu
re (
2015
)
NB: Bpol
& Btor
out of phase like Q & I in LC circuit (oscillator)
An oscillator at work:
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Solar dynamo as an oscillator
Mu
noz
-Jar
amill
o le
ctu
re (
2015
)
???
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Half of the oscillation…
Mu
noz
-Jar
amill
o le
ctu
re (
2015
)
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Activity 44: Estimate the time it takes for the solar equator to execute one more full rotation than the poles in the same time.
P = 25 d @ equator: f = 1/25 = 0.040 d-1
P = 35 d @ poles: f = 1/35 = 0.029 d-1
Δf = 0.011 d-1 🡪 1/Δf = 87 d
Check:N
eq = 87/25 = 3.5 rotations of equator
Npole
= 87/35 = 2.5 rotations of equator
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Activity 47: If we take the Sun’s polar field – averaging at cycle minimum at about 5 Gauss – how long would it take to wind that field into a strength of some 105 G? Hint: remember the field line stretch-and-fold from Fig. 4.6, look at the illustration in Fig. 4.9, and consider ’compound interest’. [i.e. exponentials]
Fig. 4.6
Fig. 4.9
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Activity 47: p. 86: If we take the Sun’s polar field – averaging at cycle minimum at about 5 Gauss – how long would it take to wind that field into a strength of some 105 G? Hint: remember the field line stretch-and-fold from Fig. 4.6, look at the illustration in Fig. 4.9, and consider ’compound interest’. [i.e. exponententials]
1 stretch+fold requires 87 days (one rotation of pole w.r.t. equator)`compound interest’: Field strength doubles every 87 days
🡪 e-folding time = 87/ln(2) = 125 days
B = 5 G × exp( t/125 ) = 105 G
t = 125 d × ln( 105/5 ) = 1,240 days = 3.4 years
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The other half … mean field theory(see lecture by Prof. Bhattacharjee)
Mu
noz
-Jar
amill
o le
ctu
re (
2015
)
α effect
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Mu
noz
-Jar
amill
o le
ctu
re (
2015
)
The other half…Babcock-Leighton model
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Synoptic plot: unwrapped view built up over time
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Tilted active regions contribute to magnetic dipole moment – in sense to reverse it
remnant of last cycle
avg-ed over φ
Btor B
pol
dipole component
sin
(lat
)
Hale’s Law: toroidal field from diff. rotation
Joy’s Law: tilt of bipole 🡪 poloidal field
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old cycle
tilted active regions
newcycle
sun-spot #
dipole moment
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Activity 51: Question: with this value of D [=250 km2/s], what is the characteristic time scale for flux to disperse over the solar surface (hint: Eq. 3.20)? [H]ow important is the meridional advection from equator to pole (with a characteristic velocity of 10 m/s) in transporting the field within the duration of a solar cycle?
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Activity 51: Question: with this value of D [=250 km2/s], what is the characteristic time scale for flux to disperse over the solar surface (hint: Eq. 3.20)? [H]ow important is the meridional advection from equator to pole (with a characteristic velocity of 10 m/s) in transporting the field within the duration of a solar cycle?
Lt ~ R
⊙ = 7 × 105 km
τd
~ Lt2/D = 2 × 109 s = 65 y
vs. R⊙
/v = (7 × 105 km)/(10-2 km/s) = 7 × 107 s = 2.3 y
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Cliver et. al 2013
Long(er)-term variation on the solar dynamo:
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Stan
ley
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Convection zones
7000 6000 5000 40008000
R⨀
2 R⨀
F0 F5 G0 G5 K0 K5
R*
CZ radius
Fullyradiative
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Other stars
Activity on main sequence: types F 🡪 M
B-V > 0.4
Evidence ofmagnetic activity
(From Linsky 1985)
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Activity 50: Relate the Rossby number in Eq. (4.2) to the dynamo number CΩ and the magnetic Reynolds number R
m in Eq. (4.20):
NR = R
m2/ CΩ.
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The Dynamo NumberDynamo is linear instability for D > D
crit
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Activity vs. Rossby Number
(from Noyes et al. 1984)
young stars
old stars
Increasing D
Stars spin down over time:
~ m
agn
etic
fie
ld
(Skumanich law)
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Wright et al. 2011
Sun
Increasing D
824 stars=
L X/Lb
ol
= Prot
/τc
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From Cameron & Schussler 2017:• The solar dynamo is operating near D ≃ D
crit• Only single normal mode is unstable• Long term variation from fluctuations
Sun
Increasing D
Dcrit
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γ
π 2π 3π 4π 5π
D > DcritD < D
crit
D ≫ Dcrit
kd
γ > 0
one unstable mode
vv
v
many unstable modes
Generic to many PDEs:Rayleigh-Taylor: Ra > Ra
crit🡪 Kelvin-Helmholtz
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Cam
ero
n &
Sc
hu
ssle
r 20
17
σ = 0: no random forcing
σ > 0: random forcing
linear instability random forcing(Wiener process)
years
one normal mode:non-linear saturation
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How the dynamo works for Earth
Turbulent conducting fluid: DYNAMO
Non-conducting mantle
Complex flows – complex field
simplifies w/ increasing r
Ch
rist
ense
n
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Dominated by low l
More even distribution over l
Ch
rist
ense
n
Simplifies w/ radius
@ surface
@ core-mantle boundary
dipole
e-1.26 l
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Observation: what Br looks like today
@ core-mantle boundary: lower boundary of potential region
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Simplifies w/ increasing r
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Evolution of field@ surface for 100 years
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Evolution of field@ core-mantle boundary for 100 years
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Use evolution to infer fluid velocity
Subsonic flow,Ignore stratification
Ignore diffusion
v ~ 3 X 10-4 m/s Δx = 1,000 km in 100 years
known
Ch
rist
ense
n
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Longer-term evolution
normal reversed
Like toy dynamo, Earth works in 2 modes. Flips between them seemingly at random
Ch
rist
ense
n
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Model geodynamo
• Glatzmaier & Roberts 1995
• Numerical solution of MHD
• Toroidal structure inside convecting core
http
://w
ww
.es.
ucs
c.ed
u/~
glat
z/ge
od
ynam
o.h
tml
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Activity 57: Summarize the contrast between the dynamo of a terrestrial planet with that of stars as discussed in this Chapter 4: consider, among others, flow speed, rotation period, stratification, differential rotation, and meridional advection.
η [m2/s] υ [m2/s] L [m] v [m/s] Ω [rad/s] Rm Re Ro
Sun (CZ) 1 10-2 108 1 10-6 108 1010 10-2
Earth (core) 1 10-5 106 10-4 10-4 102 107 10-6
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Dynamo comparison: Sun vs. Earth
Rm = 108
Rm = 102
Ro = 10-2
Ro = 10-6
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Ro = 10-6 D ~ 1012 ≫ Dcrit
Ro = 10-2 D ~ 104 ≳ Dcrit
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Other planets
Ch
rist
ense
n
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Other planetsChristensen
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What that means
Christensen
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Stan
ley
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Stan
ley
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Level of saturation
B saturates(exp growth ends)
when driving power – thermal conduction q
0 –
balances Ohmic dissipation
Rc = 0.4 R
Rc = 0.6 R
from Christensen
dimensionless factors
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Summary
• Magnetic fields – all from dynamos– Conducting fluid
– Complex motions w/ enough umph
• Create complex fields
• Fields evolve in time – reverse occasionally
• Differences from different parameters:
Rm, Re, Ro