Geophysics, Lecture Notes- Physics - 16, Study notes of Physics

Overview of head budget and earth, Heat flow and depth of oceans, convection in mantle, thermal structure of core

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2010/2011

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PX266 Geophysics (2010/11)
Lecture 15 Handout Earth’s Magnetic Field and Paleomagnetism
Dr. Gavin Bell
Magnetic declination: angle between magnetic and geographical meridians.
Magnetic inclination: angle Iat which local field dips below horizontal, depending
only on latitude
for a cylindrically symmetric (dipole) field.
tan2tan
I
Where are the geomagnetic poles (GMPs) right now?
NGMP: Canadian Arctic, 82°N 248°E.
SGMP: Antarctic Ocean, 65°S 138°E.
These are not antipodal (i.e. opposite each other)! They also drift (see animation on
course web site). The Earth’s field is quite close to but not precisely a dipole field
there are higher order components which alter the detailed form of the field, including
breaking its N-S and longitudinal symmetry. Actually, symmetry-breaking is required
in the “alpha-omega” theory of the self-exciting geodynamo. The non-dipolar
components vary rapidly (timescale < 100 years). Changes in the geomagnetic field
intensity and magnetic pole locations are known as secular variation.
The Geodynamo
Currents flowing in the core give rise to the geomagnetic field: the Earth is not a
“giant bar magnet” since the iron core is well above its Curie temperature! Both the
liquid outer core and solid inner core can carry electrical currents. The “geodynamo”
which gives rise to the Earth’s field must be self-exciting since the dissipative effects
of ohmic heating have not caused the currents and field to fade away over the Earth’s
geological history. The precise mechanism of the self-sustaining geodynamo is not
known. However, the so-called alpha-omega theory, illustrated below, shows how
convective motion in the outer core (basically powered by cooling of the core) can
lead to a self-sustaining magnetic field.
The inner core may rotate a couple
of degrees longitude per year faster
than the mantle and crust. The
difference in rotation speed feeds
back from the torque on the core
due to the magnetic field. This
omega effect “wraps up” the field
lines helically (b,c) to give a
toroidal field in the core (d).
Convection in the outer core causes
field lines to become helical via the
Coriolis force (e) leading to loops
of field which reinforce the original
dipolar field (f).
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PX266 Geophysics (2010/11)

Lecture 15 Handout – Earth’s Magnetic Field and Paleomagnetism

Dr. Gavin Bell Magnetic declination: angle between magnetic and geographical meridians. Magnetic inclination: angle I at which local field dips below horizontal, depending only on latitude  for a cylindrically symmetric (dipole) field.

tan I  2 tan 

Where are the geomagnetic poles (GMPs) right now? NGMP: Canadian Arctic, 82°N 248°E. SGMP: Antarctic Ocean, 65°S 138°E. These are not antipodal (i.e. opposite each other)! They also drift (see animation on course web site). The Earth’s field is quite close to but not precisely a dipole field – there are higher order components which alter the detailed form of the field, including breaking its N-S and longitudinal symmetry. Actually, symmetry-breaking is required in the “alpha-omega” theory of the self-exciting geodynamo. The non-dipolar components vary rapidly (timescale < 100 years). Changes in the geomagnetic field intensity and magnetic pole locations are known as secular variation. The Geodynamo Currents flowing in the core give rise to the geomagnetic field: the Earth is not a “giant bar magnet” since the iron core is well above its Curie temperature! Both the liquid outer core and solid inner core can carry electrical currents. The “geodynamo” which gives rise to the Earth’s field must be self-exciting since the dissipative effects of ohmic heating have not caused the currents and field to fade away over the Earth’s geological history. The precise mechanism of the self-sustaining geodynamo is not known. However, the so-called alpha-omega theory, illustrated below, shows how convective motion in the outer core (basically powered by cooling of the core) can lead to a self-sustaining magnetic field. The inner core may rotate a couple of degrees longitude per year faster than the mantle and crust. The difference in rotation speed feeds back from the torque on the core due to the magnetic field. This omega effect “wraps up” the field lines helically (b,c) to give a toroidal field in the core (d). Convection in the outer core causes field lines to become helical via the Coriolis force (e) leading to loops of field which reinforce the original dipolar field (f).

Geomagnetic Polarity Reversals Why are the field reversals rather random? It may be that outer core convection acts to reverse the field on a fast timescale but this is inhibited by the slow response of the solid inner core, so reversal ‘attempts’ rarely succeed. When they do, supercomputer simulations of the magnetohydrodynamics of the geodynamo indicate that field reversal is very rapid (~ 1000 years) in agreement with the geological record. Magnetic minerals Ferrimagnetic minerals including haematite and magnetite are found in oceanic basalts and other rocks. Note that ferrimagnets are “almost” ferromagnetic: while some spins orient antiferromagnetically the net spin of the crystal structure is non- zero. When a ferrimagnet is cooled through its Curie temperature TC , the magnetisation spontaneously aligns. If there is a small external magnetic field, it will align along this field. Provided the mineral remains well below TC then changes in the (sufficiently small) external field will not affect the magnetisation of the mineral. Magnetite Fe 3 O 4 TC = 570°C (^) (possibly a “half-metal”) Haematite Fe 2 O 3 TC = 680°C Further study Check you understand the basics of the geomagnetic field (approximately dipole form outside the core, something about its origin, reversals) - useful links on the web site. Make sure you understand how the local field can be ‘frozen’ in rocks cooling through their minerals’ Curie points, leading to inclination and polarity records. We don’t cover other forms of remanent magnetisation, e.g. sedimentary, though it’s good to be aware of them (see text books).