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GEOMAGNETISM: a dynamo at the centre of the Earth

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... G. Masters, D Price & M.J. Gillan 'Can the Earth's dynamo run on heat alone? ... Round up 1000 MW/K. And find the heat flux ... E = 262 MW/K Dynamo fails ... – PowerPoint PPT presentation

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Title: GEOMAGNETISM: a dynamo at the centre of the Earth


1
GEOMAGNETISM a dynamo at the centre of the Earth
  • Lecture 1 How the dynamo is powered
  • Lecture 2 How the dynamo works
  • Lecture 3 Interpreting the observations
  • Lecture 4 Thermal core-mantle interactions

2
Lecture 1How the dynamo is powered
  • Gubbins, D., D. Alfe, G. Masters, D Price M.J.
    Gillan Can the Earths dynamo run on heat
    alone?
  • Gross thermodynamics of 2-component core
    convection
  • - both under review for Geophysical Journal
    International

3
ENERGY LOST THROUGH ELECTRICAL RESISTANCE
  • Magnetic field decays in 15,000 years
  • Energy loss is 1011 - 1012 W

4
THE MODEL
  • Core cooling drives convection
  • Perhaps some radioactive heating
  • Inner core freezes -gt more latent heat
  • and releases light material that drives
    convection through
  • Release of gravitational energy

5
Mantle
K40
O
inner core
H
latent heat
Fe
S
Si
6
THE BASIC STATE
  • Pressure is nearly hydrostatic
  • Convective velocity gtgt diffusion
  • means core is well mixed
  • including entropy
  • Temperature is adiabatic

7
GRUNEISSENS PARAMETER
Thermodynamic definition
Hydrostatic pressure
Seismic parameter
8
Temperature in the core is found by integrating
up from the inner core boundary, where T is the
known melting temperature
Time evolution of the (logarithm) of temperature
is then the same everywhere
9
INNER CORE FREEZING
10
THE FIRST TWIST...
  • Conservation of energy does not equate the energy
    required with the heat lost by the magnetic
    field, in fact it does not involve the magnetic
    field at all!

11
ENERGY FLOW CHART
dynamo
conduction convection
electrical heating
buoyancy
expansion
12
ENTROPY BALANCE
  • Dissipation gives entropy gains
  • thermal conduction
  • electrical conduction
  • Offset by entropy losses if TingtTout

13
BACKUS IDEAL DYNAMO
Efficiency
  • Can be greater than unity.
  • This is because the output of the heat engine,
    the electrical heating, is used again in powering
    the convection.
  • A Carnot engine driving a disk dynamo achieves
    the ideal bound

14
THE SECOND TWIST...
  • Cooling and contraction releases a significant
    amount of Earths gravitational energy
  • Freezing also releases gravitational energy
  • Is this available to the dynamo? Some think so
  • But only about 5 is available

15
GRAVITATIONAL ENERGY
  • Is calculated from the work done in assembling
    all the mass from infinity
  • The gravitational force is conservative, so we
    can do this however we like
  • Assemble the mass of the Earth slowly,
    maintaining hydrostatic pressure
  • Then all of the gravitational energy goes into
    compaction, except for.
  • a small amount caused by pressure heating

16
PRESSURE HEATING
Drop temperature for change in volume
From the Maxwell relation
Heat released
Divide by specific heat released
17
PRESSURE EFFECT ON FREEZING
The change in volume on freezing also releases
gravitational energy The change in volume on
freezing is related to the latent heat (L)
through the Clausius-Clapeyron equation
Again the only part of this gravitational energy
that is available to drive convection is a small
amount of pressure heating
18
The increase in melting temperature caused by the
higher causes the inner core to grow a little
more The latent heat released is identically
equal to the gravitational energy change, because
of the Clausius-Clapeyron equation
19
SUMMARY - HEAT ONLY
Entropy balance choose LHS and find cooling rate
and radioactive heating h
Energy balance find heat flux from cooling rate
and radioactive heating h
20
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21
ADIABATIC GRADIENTS
22
HEAT BUDGET
Earths heat budget Crustal radioactivity 9 TW
mostly lower crust mantle radioactivity
25 TW chondritic composition core
radioactivity 0 TW iron meteorites,
chemistry cooling 10 TW includes
core, mantle TOTAL 44 TW Surface heat
flux Cooling rate 36 K/Gyr From core 3 TW
23
RESULTS FOR THERMAL CONVECTION
MODEL dTc/dt dri/dt ICage QL QS Q K/Gyr
km/Gyr Ma TW TW TW GAMP02 214
1414 288 10.2 10.9 21.6 LPL97 234
1550 263 8.4 14.2 23.0 NOIC 565
0.0 28.8 28.8
Comparison between 3 models of Gubbins et al
2002 LaBrosse et al 1997 (modified) and a model
with no inner core (L0)
24
COMPOSITIONAL CONVECTION
  • Light material released at the inner core
    boundary on freezing rises to stir the core
  • Energy source is Earths gravitational energy
  • This changes as light material rises, heavy iron
    sinks
  • Compositional convection stirs the core directly,
    there is no thermal efficiency factor

25
Mantle
K40
O
inner core
H
latent heat
Fe
S
Si
26
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27
THE STORY SO FAR...
  • Thermal convection cannot drive the dynamo
    because too much heat is needed
  • This means we have no means of generating a
    magnetic field before the inner core formed, the
    inner core must be as old as the magnetic field
  • Compositional convection can help drive the
    dynamo
  • The solid inner core can include 8 S or Si to
    explain the density. When this mixture freezes,
    it all freezes.
  • A liquid Fe8S8 O can explain the density of
    the liquid outer core
  • When Fe8O mixture freezes, the O is left in the
    liquid
  • This provides the source of buoyancy for
    compositional convection

28
NEXT...
  • We see if compositional plus thermal convection
    can drive the dynamo
  • We estimate the cooling rates and radioactive
    heating needed by balancing the entropy
  • Then we use the cooling rate and radioactive
    heating to calculate the heat flux across the
    core-mantle boundary and the inner core age.

29
CORE COMPOSITION OF PRICE, ALFE GILLAN (2001)
30
DENSITY REDUCTIONS FROM PURE IRON AT ICB PRESSURE
AND TEMPERATURE
r Dr Solid iron 13.16 8
S/Si 12.76 3.0 0.40 Melting 12.52 1.8 0.24 8
O 12.17 2.8 0.37
Ideal solutions theory predicts densities well,
but not diffusion constants or free energies
31
DISSIPATION ENTROPY
  • Thermal conduction 200-500 MW/K
  • Ohmic heating 50-500 MW/K
  • Molecular diffusion 1 MW/K
  • Round up 1000 MW/K

32
FINAL EQUATIONS
Find the cooling rate and radioactive heating
from the entropy balance
And find the heat flux from cooling rate and
radioactive heating
33
THE MODELS
  • E 1000 MW/K rounding up
  • E 546 MW/K, heat conducted down by compositional
    convection
  • E 262 MW/K Dynamo fails
  • Repeat with enough radioactive heating to make
    the inner core last 3.5 Gyr

34
RESULTS FOR COMPOSITIONAL CONVECTION
35
CONCLUSIONS
  • Compositional convection only doubles the
    efficiency of the dynamo
  • With present estimates and no radioactivity in
    the core, the age of the inner core is less than
    1Ga
  • The simplest way to alter this result is to
    increase the seismological estimate of the
    density jump at the inner core boundary
  • At present it seems impossible to drive the
    dynamo without an inner core
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