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Winter Quarter 2009 Vassilis Angelopoulos Robert Strangeway Date Topic [Instructor] 1/5 Organization and Introduction to Space Physics I [A&S] 1/7 Introduction.

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Presentation on theme: "Winter Quarter 2009 Vassilis Angelopoulos Robert Strangeway Date Topic [Instructor] 1/5 Organization and Introduction to Space Physics I [A&S] 1/7 Introduction."— Presentation transcript:

1 Winter Quarter 2009 Vassilis Angelopoulos Robert Strangeway Date Topic [Instructor] 1/5 Organization and Introduction to Space Physics I [A&S] 1/7 Introduction to Space Physics II [A] 1/12 Introduction to Space Physics III [S] 1/14 The Sun I [A] 1/21 The Sun II [S] 1/23 (Fri) The Solar Wind I [A] 1/26 The Solar Wind II [S] 1/ First Exam [A&S] 2/2 Bow Shock and Magnetosheath [A] 2/4 The Magnetosphere I [A] ESS 200C - Space Plasma Physics Date Topic 2/9 The Magnetosphere II [S] 2/11 The Magnetosphere III [A] 2/18 Planetary Magnetospheres [S] 2/20 (Fri) The Earth’s Ionosphere [S] 2/23 Substorms [A] 2/25 Aurorae [S] 3/2 Planetary Ionospheres [S] 3/4 Pulsations and waves [A] 3/9 Storms and Review [A&S] 3/ Second Exam [A&S] Schedule of Classes

2 ESS 200C – Space Plasma Physics There will be two examinations and homework assignments. The grade will be based on –35% Exam 1 –35% Exam 2 –30% Homework References –Kivelson M. G. and C. T. Russell, Introduction to Space Physics, Cambridge University Press, –Chen, F. F., Introduction of Plasma Physics and Controlled Fusion, Plenum Press, 1984 –Gombosi, T. I., Physics of the Space Environment, Cambridge University Press, 1998 –Kellenrode, M-B, Space Physics, An Introduction to Plasmas and Particles in the Heliosphere and Magnetospheres, Springer, –Walker, A. D. M., Magnetohydrodynamic Waves in Space, Institute of Physics Publishing, 2005.

3 Space Plasma Physics Space physics is concerned with the interaction of charged particles with electric and magnetic fields in space. Space physics involves the interaction between the Sun, the solar wind, the magnetosphere and the ionosphere. Space physics started with observations of the aurorae. –Old Testament references to auroras. –Greek literature speaks of “moving accumulations of burning clouds” –Chinese literature has references to auroras prior to 2000BC

4 Aurora over Los Angeles (courtesy V. Peroomian) Cro-Magnon “macaronis” may be earliest depiction of aurora (30,000 B.C.)

5 –Galileo theorized that aurora is caused by air rising out of the Earth’s shadow to be illuminated by sunlight. (He also coined the name aurora borealis meaning “northern dawn”.) –Descartes thought aurorae are reflections from ice crystals. –Halley suggested that auroral phenomena are ordered by the Earth’s magnetic field. –In 1731 the French philosopher de Mairan suggested they are connected to the solar atmosphere.

6 By the 11th century the Chinese had learned that a magnetic needle points north-south. By the 12th century the European records mention the compass. That there was a difference between magnetic north and the direction of the compass needle (declination) was known by the 16th century. William Gilbert (1600) realized that the field was dipolar. In 1698 Edmund Halley organized the first scientific expedition to map the field in the Atlantic Ocean.

7 By the beginning of the space age auroral eruptions had been placed in the context of the Sun-Earth Connection 1716Sir Edmund HalleyAurora is aligned with Earth’s field… 1741Anders Celsiusand has magnetic disturbances. 1790Henry CavendishIts light is produced at km 1806Alexander Humboldt but is related to geomagnetic storms 1859Richard Carringtonand to Solar eruptions. 1866Anders AngströmAuroral eruptions are self-luminous and… 1896Kristian Birkeland… due to currents from space: 1907Carl Störmerin fact to field-aligned electrons… 1932Chapman & Ferraroaccelerated in the magnetosphere by… 1950Hannes Alfvénthe Solar-Wind–Magnetosphere dynamo Single SatellitesPolar storms related to magnetospheric activity 1976Iijima and Potemra… communicated via Birkeland currents 1977AkasofuMagnetospheric substorm cycle is defined 1997GeotailResolves magnetic reconnection ion dynamics ISTP eraSolar wind energy tracked from cradle to grave 2002-Cluster eraSpace currents measured, space-time resolved 2008THEMIS Substorm onset is due to reconnection

8 It All Starts from the Sun… Solar Wind Properties: Comprised of protons (96%), He 2+ ions (4%), and electrons. Flows out in an Archimedean spiral. Average Values: –Speed (nearly Radial): km/s –Proton Density: cm -3 –Proton Temperature 1-10eV ( K)

9 Shaping Earth’s Magnetosphere Earth’s magnetic field is an obstacle in the supersonic magnetized solar wind flow. Solar wind confines Earth’s magnetic field to a cavity called the “Magnetosphere”

10 Auroral Displays: Direct Manifestation of Space Plasma Dynamics

11 Societal Consequences of Magnetic Storms Damage to spacecraft. Loss of spacecraft. Increased Radiation Hazard. Power Outages and radio blackouts. Damage to spacecraft. Loss of spacecraft. Increased Radiation Hazard. Power Outages and radio blackouts. GPS Errors

12 Stellar wind coupling to planetary objects is ubiquitous in astrophysical systems MERCURY: 10 min EARTH: 3.75 hrs JUPITER: 3 weeks ASTROSPHERE GALACTIC CONFINEMENT SUBSTORM RECURRENCE: Magnetized wind coupling to stellar and galactic systems is common thoughout the Universe Mira (a mass shedding red giant) and its 13 light-year long tail In this class we study the physics that enable and control such planetary and stellar interactions

13 Introduction to Space Physics I-III Reading material –Kivelson and Russell Ch. 1, 2, –Chen, Ch. 2

14 The Plasma State A plasma is an electrically neutral ionized gas. –The Sun is a plasma –The space between the Sun and the Earth is “filled” with a plasma. –The Earth is surrounded by a plasma. –A stroke of lightning forms a plasma –Over 99% of the Universe is a plasma. Although neutral a plasma is composed of charged particles- electric and magnetic forces are critical for understanding plasmas.

15 The Motion of Charged Particles Equation of motion SI Units –mass (m) - kg –length (l) - m –time (t) - s –electric field (E) - V/m –magnetic field (B) - T –velocity (v) - m/s –F g stands for non-electromagnetic forces (e.g. gravity) - usually ignorable.

16 B acts to change the motion of a charged particle only in directions perpendicular to the motion. –Set E = 0, assume B along z-direction.

17 Solution is circular motion dependent on initial conditions. Assuming at t=0: and –Equations of circular motion with angular frequency  c (cyclotron frequency or gyro frequency). Above signs are for positive charge, below signs are for negative charge. If q is positive particle gyrates in left handed sense If q is negative particle gyrates in a right handed sense

18 Radius of circle ( r c ) - cyclotron radius or Larmor radius or gyro radius. –The gyro radius is a function of energy. –Energy of charged particles is usually given in electron volts (eV) –Energy that a particle with the charge of an electron gets in falling through a potential drop of 1 Volt- 1 eV = 1.6X Joules (J). Energies in space plasmas go from electron Volts to kiloelectron Volts (1 keV = 10 3 eV) to millions of electron Volts (1 meV = 10 6 eV) Cosmic ray energies go to gigaelectron Volts ( 1 GeV = 10 9 eV). The circular motion does no work on a particle Only the electric field can energize particles! Particle energy remains constant in absence of E !

19 The electric field can modify the particles motion. –Assume but still uniform and F g =0. –Frequently in space physics it is ok to set Only can accelerate particles along Positive particles go along and negative particles go along Eventually charge separation wipes out – has a major effect on motion. As a particle gyrates it moves along and gains energy Later in the circle it losses energy. This causes different parts of the “circle” to have different radii - it doesn’t close on itself. Drift velocity is perpendicular to and No charge dependence, therefore no currents

20 Y X Z

21 Assuming E is along x-direction, B along z-direction: Solution is: In general, averaging over a gyration:

22 Note that V ExB is: –Independent of particle charge, mass, energy –V ExB is frame dependent, as an observer moving with same velocity will observe no drift. –The electric field has to be zero in that moving frame. Consistent with transformation of electric field in moving frame: E’=  (E+VxB). Ignoring relativistic effects, electric field in the frame moving with V= V ExB is E’=0. Mnemonics: –E is 1mV/m for 1000km/s in a 1nT field V[1000km/s] = E[mV/m] / B [nT] –Thermal velocities (kT=1/2 m v th 2 ): 1keV proton = 440km/s 1eV electron = 600km/s –Gyration: Proton gyro-period: 66s*(1nT/B) Electron: 28Hz*(B/1nT) –Gyroradii: 1keV proton in 1nT field: 4600km*(m/m p ) 1/2 *(W/keV)*(1nT/B) 1eV electron in 1nT field: 3.4km *(W/eV)*(1nT/B)

23 Any force capable of accelerating and decelerating charged particles can cause an average (over gyromotion) drift: –e.g., gravity –If the force is charge independent the drift motion will depend on the sign of the charge and can form perpendicular currents. –Forces resembling the above gravitational force can be generated by centrifugal acceleration of orbits moving along curved fields. This is the origin of the term “gravitational” instabilities which develop due to the drift of ions in a curved magnetic field (not really gravity). –In general 1 st order drifts develop when the 0 th order gyration motion occurs in a spatially or temporally varying external field. To evaluate 1 st order drifts we have to integrate over 0 th order motion, assuming small perturbations relative to  c, r L

24 The Concept of the Guiding Center –Separates the motion ( ) of a particle into motion perpendicular ( ) and parallel ( ) to the magnetic field. –To a good approximation the perpendicular motion can consist of a drift ( ) and the gyro-motion ( ) –Over long times the gyro-motion is averaged out and the particle motion can be described by the guiding center motion consisting of the parallel motion and drift. This is very useful for distances l such that and time scales  such that

25 Inhomogenious magnetic fields cause GradB drift. –If changes over a gyro-orbit r L will change. – gets smaller when particle goes into stronger B. –Assume  B is along Y –Average force over gyration: –u  B depends on charge, yields perpendicular currents. x Y Z B=B z z - +

26 The change in the direction of the magnetic field along a field line can also cause drift (Curvature drift). –The curvature of the magnetic field line introduces a drift motion. As particles move along the field they undergo centrifugal acceleration. R c is the radius of curvature of a field line ( ) where, is perpendicular to and points away from the center of curvature, is the component of velocity along Curvature drift can also cause currents.

27 At Earth’s dipole u  B, u c are same direction and comparable: –u  B, u c are ~ 1R E /min=100km/s for 100keV particle at 5R E, at 100nT –The drift around Earth is: 0.5hrs for the same particle at the same location At Earth’s magnetotail current sheet, u  B, u c are opposite each other: –Curvature dominates at Equator, Gradient dominates further away from equator

28 Parallel motion: Inhomogeniety along B (  ║ B) –As particles move along a changing field they experience force Parallel force is Lorenz force due to small  B perpendicular to nominal B (  W ║ ) Force along particle gyration is due to dB/dt in frame of gyrocenter (  W ┴ ) Total particle energy is conserved because there is no electric field in rest frame –Consider 1 st order force on 0 th order orbit in mirror field B change due to presence of  ║ B must be divergence-less (  B=0) so: –In cylindical coordinates gyration is: –The mirror field is: –The Lorenz force is: –From gyro-orbit averaging: –Defining: we get: –This is the mirror force. Note that is conserved during the particle motion: Y X Z r dr dd dzdz

29 Another way of viewing  –As a particle gyrates the current will be where –The force on a dipole magnetic moment is Where I.e., same as we derived earlier by averaging over gyromotion

30 In a Magnetic Mirror: The force is along and away from the direction of increasing B. Since and kinetic energy must be conserved a decrease in must yield an increase in Particles will turn around when The loss cone at a given point is the pitch angle below which particles will get lost:

31 Time varying fields: B –As particle moves into changing field or –As imposed/background field increases (adiabatic compression/heating) An electric field appears affecting particle orbit Along gyromotion, speed v ┴ increases, but μ is conserved: Flux through Larmor orbit:  =  r L 2 B=(2  m/q 2 )  remains constant

32 Time varying fields: E –See Chen, Ch 2

33 Maxwell’s equations –Poisson’s Equation is the electric field is the charge density is the electric permittivity (8.85 X Farad/m) –Gauss’ Law (absence of magnetic monopoles) is the magnetic field –Faraday’s Law –Ampere’s Law c is the speed of light. Is the permeability of free space, H/m is the current density

34 Maxwell’s equations in integral form Note: use Gauss and Stokes theorems; identities A1.33; A1.40 in Kivelson and Russell) – is a unit normal vector to surface: outward directed for closed surface or in direction given by the right hand rule around C for open surface, and is magnetic flux through the surface. – is the differential element around C.

35 The first adiabatic invariant – says that changing drives (electromotive force). This means that the particles change energy in changing magnetic fields. –Even if the energy changes there is a quantity that remains constant provided the magnetic field changes slowly enough. – is called the magnetic moment. In a wire loop the magnetic moment is the current through the loop times the area. –As a particle moves to a region of stronger (weaker) B it is accelerated (decelerated).

36 For a coordinate in which the motion is periodic the action integral is conserved. Here p i is the canonical momentum: where A is the vector potential). First term: Second term: For a gyrating particle: Note: All action integrals are conserved when the properties of the system change slowly compared to the period of the coordinate.

37 The second adiabatic invariant –The integral of the parallel momentum over one complete bounce between mirrors is constant (as long as B doesn’t change much in a bounce). B m is the magnetic field at the mirror point –Note the integral depends on the field line, not the particle –If the length of the field line decreases, u || will increase Fermi acceleration

38 The total particle drift in static E and B fields is: For equatorial particle in electrostatic potential  (E=-  ): –Particle conserves total (potential plus kinetic) energy Bounce-averaged motion for particles with finite J –Particle’s equatorial trace conserves total energy

39 Drift paths for equatorially mirroring (J=0) particles, or … for bounce-averaged particles’ equatorial traces in a realistic magnetosphere.

40 –As particles bounce they also drift because of gradient and curvature drift motion and in general gain/lose kinetic energy in the presence of electric fields. –If the field is a dipole and no electric field is present, then their trajectories will take them around the planet and close on themselves. The third adiabatic invariant –As long as the magnetic field doesn’t change much in the time required to drift around a planet the magnetic flux inside the orbit must be constant. –Note it is the total flux that is conserved including the flux within the planet.


42 Limitations on the invariants – is constant when there is little change in the field’s strength over a cyclotron path. –All invariants require that the magnetic field not change much in the time required for one cycle of motion where is the cycle period.

43 A plasma as a collection of particles –The properties of a collection of particles can be described by specifying how many there are in a 6 dimensional volume called phase space. There are 3 dimensions in “real” or configuration space and 3 dimensions in velocity space. The volume in phase space is The number of particles in a phase space volume is where f is called the distribution function. –The density of particles of species “s” (number per unit volume) –The average velocity (bulk flow velocity) The Properties of a Plasma

44 –Average random energy –The partial pressure of s is given by where N is the number of independent velocity components (usually 3). –In equilibrium the phase space distribution is a Maxwellian distribution where

45 For monatomic particles in equilibrium The ideal gas law becomes –where k is the Boltzman constant (k=1.38x JK -1 ) This is true even for magnetized particles. The average energy per degree of freedom is: –for a 1keV, 3-dimensional proton distribution, we mean: kT=1keV, get E average =1.5keV, and define v themal =(2kT/m p ) 1/2 =440km/s –for a 1keV beam with no thermal spread kT=0 and V=440km/s

46 –Other frequently used distribution functions. The bi-Maxwellian distribution –where –It is useful when there is a difference between the distributions perpendicular and parallel to the magnetic field The kappa distribution –Κ characterizes the departure from Maxwellian form. –E Ts is an energy. –At high energies E>>κE Ts it falls off more slowly than a Maxwellian (similar to a power law) –For it becomes a Maxwellian with temperature kT=E Ts

47 What makes an ionized gas a plasma? –The electrostatic potential of an isolated charge q 0 –The electrons in the gas will be attracted to the ion and will reduce the potential at large distances, so the distribution will differ from vacuum. –If we assume neutrality Poisson’s equation around q 0 is –The particle distribution is Maxwellian subject to the external potential assuming n i =n e =n  far away –At intermediate distances (not at charge, not at infinity): –Expanding in a Taylor series for r>0 for both electrons and ions

48 The Debye length ( ) is where n is the electron number density and now e is the electron charge. Note: colder species dominates. The number of particles within a Debye sphere needs to be large for shielding to occur (N D >>1). Far from the central charge the electrostatic force is shielded.


50 The plasma frequency –Consider a slab of plasma of thickness L. –At t=0 displace the electron part of the slab by <

51 –The frequency of this oscillation is the plasma frequency –Because m ion >>m e

52 Useful formulas:

53 A note on conservation laws –Consider a quantity that can be moved from place to place. –Let be the flux of this quantity – i.e. if we have an element of area then is the amount of the quantity passing the area element per unit time. –Consider a volume V of space, bounded by a surface S. –If  is the density of the substance then the total amount in the volume is –The rate at which material is lost through the surface is –Use Gauss’ theorem –An equation of the preceeding form means that the quantity whose density is  is conserved.

54 Magnetohydrodynamics (MHD) –The average properties are governed by the basic conservation laws for mass, momentum and energy in a fluid. –Continuity equation –S s and L s represent sources and losses. S s -L s is the net rate at which particles are added or lost per unit volume. –The number of particles changes only if there are sources and losses. –S s,L s,n s, and u s can be functions of time and position. –Assume S s =0 and L s =0, where M s is the total mass of s and dr is a volume element (e.g. dxdydz) where is a surface element bounding the volume.

55 –Momentum equation where is the charge density, is the current density, and the last term is the density of non- electromagnetic forces. –The operator is called the convective derivative and gives the total time derivative resulting from intrinsic time changes and spatial motion. –If the fluid is not moving (u s =0) the left side gives the net change in the momentum density of the fluid element. –The right side is the density of forces If there is a pressure gradient then the fluid moves toward lower pressure. The second and third terms are the electric and magnetic forces.

56 –The term means that the fluid transports momentum with it. Combine the species for the continuity and momentum equations –Drop the sources and losses, multiply the continuity equations by m s, assume n p =n e and add. Continuity –Add the momentum equations and use m e <

57 Energy equation where is the heat flux, U is the internal energy density of the monatomic plasma and N is the number of degrees of freedom – adds three unknowns to our set of equations. It is usually treated by making approximations so it can be handled by the other variables. –Many treatments make the adiabatic assumption (no change in the entropy of the fluid element) instead of using the energy equation or where c s is the speed of sound and c p and c v are the specific heats at constant pressure and constant volume. It is called the polytropic index. In thermodynamic equilibrium

58 Maxwell’s equations – doesn’t help because –There are 14 unknowns in this set of equations - –We have 11 equations. Ohm’s law –Multiply the momentum equations for each individual species by q s /m s and subtract. where and  is the electrical conductivity

59 – Often the last terms on the right in Ohm’s Law can be dropped – If the plasma is collisionless, may be very large so

60 Frozen in flux –Combining Faraday’s law ( ), and Ampere’ law ( ) with where is the magnetic viscosity –If the fluid is at rest this becomes a “diffusion” equation –The magnetic field will exponentially decay (or diffuse) from a conducting medium in a time where L B is the system size.

61 –On time scales much shorter than –The electric field vanishes in the frame moving with the fluid. –Consider the rate of change of magnetic flux –The first term on the right is caused by the temporal changes in B –The second term is caused by motion of the boundary –The term is the area swept out per unit time –Use the identity and Stoke’s theorem –If the fluid is initially on surface s as it moves through the system the flux through the surface will remain constant even though the location and shape of the surface change.

62 Magnetic pressure and tension since – A magnetic pressure analogous to the plasma pressure ( ) – A “cold” plasma has and a “warm” plasma has –In equilibrium Pressure gradients form currents

63 Frozen-in Theorem Recap – 2 Rate of change of line element: r1r1 r2r2 r2'r2' r1'r1' drdr dr'dr' U 1 dt U 2 dt r 1 ' = r 1 + U 1 dt r 2 ' = r 2 + U 2 dt Taylor Expansion:

64 Frozen-in Theorem Recap – 3 Rate of change of magnetic field: Mass Conservation:

65 Magnetic pressure and tension since – A magnetic pressure analogous to the plasma pressure ( ) – A “cold” plasma has and a “warm” plasma has –In equilibrium Pressure gradients form currents

66 – cancels the parallel component of the term. Thus only the perpendicular component of the magnetic pressure exerts a force on the plasma. – is the magnetic tension and is directed antiparallel to the radius of curvature (R C ) of the field line. Note that is directed outward. – The second term in can be written as a sum of two terms

67 Some elementary wave concepts –For a plane wave propagating in the x-direction with wavelength and frequency f, the oscillating quantities can be taken to be proportional to sines and cosines. For example the pressure in a sound wave propagating along an organ pipe might vary like –A sinusoidal wave can be described by its frequency and wave vector. (In the organ pipe the frequency is f and. The wave number is ).

68 The exponent gives the phase of the wave. The phase velocity specifies how fast a feature of a monotonic wave is moving Information propagates at the group velocity. A wave can carry information provided it is formed from a finite range of frequencies or wave numbers. The group velocity is given by The phase and group velocities are calculated and waves are analyzed by determining the dispersion relation

69 When the dispersion relation shows asymptotic behavior toward a given frequency,, v g goes to zero, the wave no longer propagates and all the wave energy goes into stationary oscillations. This is called a resonance.

70 MHD waves - natural wave modes of a magnetized fluid –Sound waves in a fluid Longitudinal compressional oscillations which propagate at and is comparable to the thermal speed.

71 –Incompressible Alfvén waves Assume, incompressible fluid with background field and homogeneous Incompressibility We want plane wave solutions b=b(z,t), u=u(z,t), b z =u z =0 Ampere’s law gives the current Ignore convection ( )=0 z y x B0B0 J b, u

72 Since and the x-component of momentum becomes Faraday’s law gives The y-component of the momentum equation becomes Differentiating Faraday’s law and substituting the y- component of momentum

73 where is called the Alfvén velocity. The most general solution is. This is a disturbance propagating along magnetic field lines at the Alfvén velocity.

74 Compressible solutions –In general incompressibility will not always apply. –Usually this is approached by assuming that the system starts in equilibrium and that perturbations are small. Assume uniform B 0, perfect conductivity with equilibrium pressure p 0 and mass density

75 –Continuity –Momentum –Equation of state –Differentiate the momentum equation in time, use Faraday’s law and the ideal MHD condition where

76 –For a plane wave solution –The dispersion relationship between the frequency ( ) and the propagation vector ( ) becomes  This came from replacing derivatives in time and space by

77 – Case 1 The fluid velocity must be along and perpendicular to These are magnetosonic waves

78 – Case 2 A longitudinal mode with with dispersion relationship (sound waves) A transverse mode with and (Alfvén waves)

79 Alfven waves propagate parallel to the magnetic field. The tension force acts as the restoring force. The fluctuating quantities are the electromagnetic field and the current density.

80 –Arbitrary angle between and F I S VAVA Phase Velocities V A =2C S

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