Space Weather Flashcards
1
Q
What region defines the near geospace
A
Up to around 200 Re
2
Q
What are the regions of the space environment
A
Troposphere
Stratosphere
Mesosphere
Thermosphere
Ionosphere
Exosphere
Plasmasphere
Magnetosphere
3
Q
What is a characteristic of dispersive waves
A
Angular frequency is a function of the wave number k
4
Q
Why does the Lorentz force arise
A
Interactions when a charged particle moves in an electric and magnetic field
5
Q
What is bulk ion plasma velocity
A
Average velocity of plasma ions
6
Q
At thermal equilibrium what does each degree of freedom relate to
A
kT/2
7
Q
What does the Debye length mean
A
Spatial charge separation scale in plasma
8
Q
What are the 3 plasma criteria
A
Debye length much smaller than system spatial scale
The parameter must be much greater than 1
The time between collisions between neutral and charged particles must be much longer than the period of oscillations at plasma frequency
9
Q
What physical parameters affect Larmor radius in uniform and constant electric and magnetic fields
A
Larger mass particles will have a larger Larmor radius
Higher energy particles will have a larger Larmor radius
10
Q
What kind of drift is independent of charge
A
Electric field drift - all particles drift in the same direction with average displacement perpendicular to electric field direction
11
Q
Which drifts are dependent on charge
A
Gravitational field
General force
Gradient
12
Q
What conditions are needed for GCA to be valid
A
Larmor (cyclotron) frequency must be greater than the wave frequency
Larmor radius is much smaller than spatial scale of the system
13
Q
How does the first adiabatic invariant come about and what does it mean
A
Comparing dynamical and mechanical systems
The perpendicular kinetic energy divided by the magnetic field strength at that point is constant
14
Q
What happens to velocity at the mirror point
A
The parallel velocity component is 0
15
Q
What condition must hold for transverse waves to propagate through the ionosphere
A
Angular frequency must be greater than the plasma electron frequency
16
Q
What are sunspots
A
“Darker” parts on the sun’s surface that are associated with increased solar activity
They are cooler than surroundings and have strong magnetic field
17
Q
Summarise the layers of solar interior
A
Core - nuclear fusion occurs
Radiative zone - energy from core radiates outwards
Tachocline - transition from rigid to fluid-type rotation generating magnetic field
Convective zone - energy transported by convective currents
18
Q
How does global magnetic field generation occur
A
Differential rotation
Difference in rotational speed stretches and twists magnetic field lines in plasma causing field to become distorted and wound up over time
Converts poloidal to toroidal magnetic fields
Also turbulent plasma rotation means small-scale twisted magnetic fields generated by solar convection motions
19
Q
What are the layers of the solar atmosphere
A
Photosphere
Chromosphere
Transition region
Corona
20
Q
What is the photosphere
A
Surface of sun
Mottled texture due to granules - convection cells
21
Q
What is the chromosphere
A
Emits hydrogen-alpha light
Filaments, spicules and faculae regions around active areas
Lighter elements with traces of heavier
22
Q
What is the transition region
A
Variable layer with dramatic temperature rise
Contains ionised atoms
23
Q
What is the corona
A
Contains highly ionised atoms of iron, neon, oxygen etc.
Produces emission lines in UV and X-ray
Source of solar wind
24
Q
How is solar wind produced
A
Extremely hot corona causes high energy particles to escape gravitational pull
Ionised particles stream from corona as highly conductive plasma
25
How does solar wind form interplanetary magnetic field
As wind flows outwards carries magnetic field lines with it
26
Where does fast solar wind originate
Regions of open magnetic field liens primarily in coronal holes
Low electron density
High velocity
High proton temp
Low electron temp
High magnetic field
27
What does slow solar wind do
Role in formation of heliospheric current sheet - large scale magnetic boundary that extends through heliosphere
28
What is Parker spiral
Spiral shape of magnetic field that forms from twist due to sun rotation
More distorted during solar maximum
29
What are stream interaction regions
Fast wind piles up behind slow wind so plasma denser and more complex magnetic field
30
What effects do SIRs have
Enhanced auroral activity
Fluctuations in ionosphere interfering with satellite operations and communication
31
What are solar flares
Sudden intense bursts of radiation
Mainly EM radiation and energetic particles
Short lived
32
What are coronal mass ejections
Large scale ejection of plasma and magnetic field
Slow travelling
Plasma cloud expands and moves outward sweeping up solar wind and creates shock waves
33
What the types of CME
Limb CME - headed away from earth - no effect
Partial halo CME - glancing blow on earth - weak geomagnetic storm
Halo CME - headed directly at earth - strong and long geomagnetic storm
34
What is magnetic reconnection
Antiparallel field lines forced towards each other
Fields connect resulting in X-configuration
Field lines cut and connected to those on other side and expelled
35
How do flares and CMEs cause effects
Reconnection during flares can release energy burst that accelerates particles
CME-driven shock wave accelerates particles
36
What are the types of solar energetic particles
Impulsive SEP - short lived, localised, associated with flares, high proportion of heavy ions and electrons, narrow spatial impact
Gradual SEP - long lived, widespread, associated with CMEs, broad range of particle energies, global effects including geo storms
37
Summarise the structures surrounding earth
Bow shock, magnetosheath, magnetopause, polar cusps, tail lobes, neutral sheet
38
What are the property changes through bow shock
Bulk velocity decrease
Density increases (pile-up)
Temperature increase
Pressure increase
Normal magnetic field constant
Tangential magnetic field increase (pile-up)
39
What are the components of terrestrial bow shock
Increased magnetic field - reflects ions and electrons
Increased electrostatic potential - reflects ions, pushes electron through shock front
40
How does ion reflection work
Process for redistribution of energy in front of strong shock
If angle between magnetic field and normal to shock < 45 reflected ions move far away into upstream (quasi-parallel)
If angle > 45 reflect ions turned back by magnetic field
41
How do spatial scales of quasi-parallel and quasi-perpendicular shocks differ
Quasi-parallel shock front many times wider than ion Larmor radius
Quasi-perpendicular about same as ion Larmor radius
42
How is position of subsolar day time magnetopause position determined
Balance of dynamic ram pressure and terrestrial magnetic field pressure
43
When does reconnection occur between solar wind magnetic field and terrestrial magnetic field
When direction of solar magnetic field is directed southward
44
What is the cusp
Separates closed dayside magnetic field lines from nightside
Region of easy access for solar wind ions into magnetosphere
45
What is the magnetotail
Region on night side where magnetic field lines are elongated
Contains north and south tail lobes where density is low
46
What is the neutral/plasma sheet
Separates tail lobes
Layer of weaker magnetic field and denser plasma
47
What are the magnetospheric currents
Cross tail - flows across neutral sheet from dawn to dusk
Nightside magnetopause - closes cross tail current
Dayside magnetopause - solar wind electrons/ions deflected in different directions
Field aligned - flow along field lines connecting magnetosphere to ionosphere
Ring - trapped electrons/ions drifting in opposite directions
48
What happens to particles in magnetospheric magnetic field
Move along field lines into regions of stronger field
Pitch angle increases and transverse energy increases
Particle reflected at point where parallel motion is 0 (mirror point)
49
What effect does pitch angle have on motion
Small equatorial pitch angle means large parallel velocity
Mirror points are at high latitudes close to earth and move towards equator with increasing pitch angle
Trapped particles have close to 90 degree angle
50
What is bounce period
Time for a particle to move from equatorial plane to one mirror point, to other mirror point, back to equatorial plane
51
What is loss cone
Region where particles are absorbed rather than reflected
If mirror point is deep in atmosphere particles collide with neutrals and are absorbed
Equatorial loss con defines pitch angle where particles with a smaller angle are lost to atmosphere
52
What is the ring current
Toroidal west flowing electric current with variable density
Satellites build surface charge in it
53
What are the regions of radiation belts
Inner belt - protons, electrons and ions, stable, occasional perturbation from geo storms
Outer belt - mostly high energy electrons, dynamic, produced by injection and energisation events following geo storms
Slot region
54
Summarise radiation belt characteristics
Formed from solar wind particles entering outer magnetosphere or plasma sheet
Accelerated by local wave-particle interaction resonance
Losses from: Coulomb collision in plasma/ionosphere, magnetopause shadowing, scattering of particles by wave-particle interaction in loss cone
55
Summarise ionosphere formulation
Plasma from ionisation of atmosphere molecules by solar photons
UV absorbed so intensity decreases - rate of ion production proportional to radiation absorbed
Intensity inc. with height, density dec. with height
Electron/ion density overall increase through D and E layer, decrease at sporadic E, increase through F with maximum at F2, decrease through top layer
56
What are sources of solar weather
Fast and slow solar wind, CME, solar flares
Cosmic rays, soft gamma repeaters, gamma ray bursts
57
How is solar wind accelerated
Pressure gradient between corona and distant point in space
58
What is co-rotating interaction region
When corona is quasi-stable, solar rotation produces series of SIRs which impact on earth every 27 days (sun axis rotation time)
59
How do SIRs affect technology
Enhancement of energetic electrons in radiation belts
Geo magnetic storms cause aurora and heat thermosphere increasing density (drag)
60
How do CMEs affect technology
Cause strong geomagnetic storms that affect transformers, rail networks, oil and gas pipelines, LEO drag
Also SEP events on solar panels, aircraft
61
How is solar wind measured
Spacecraft in upstream Lagrange point
62
How do solar flares affect technology
Increased ionisation leads to radio blackouts, degradation of solar panels, heating of thermosphere
63
How do galactic cosmic rays cause problems
High energy particles accelerated meaning deeper penetration in atmosphere, collide with neutral particles and create secondary SEPs
64
What are soft gamma repeaters
Emit large bursts of gamma and X-rays irregularly
65
What is Ampere's circuit law and how is it applicable to ring current
Electric current creates a magnetic field that encircles the current and is perpendicular
Magnetic field strength is proportional to the current and inversely proportional to distance from current centre
Ring current will create a magnetic field that is in opposite direction to terrestrial magnetic field
66
What is the Dst index
Quantifies the strength of geomagnetic storms
67
How are Dst calculations performed
Find a baseline
Eliminate solar quiet daily variations
Average over values obtained from four observatories
68
What is the Kp index
Reflects variations of geomagnetic field with respect to quiet day variations
Measured on quasi-logarithmic scale
Calculated every 3 hours using values for K-indices from 13 observatories
69
What can geo storms affect
Drilling that uses geomagnetic measurements for guidance
Surveying of subsurface features using magnetic field measurements
70
How is the field aligned current quantified
Amplitude upper/lower (AU/AL) are the envelopes of superposition of recordings from observatories
Auroral electrojet (AE) is difference between AU and AL
AO index is average of AU and AL
71
How does solar wind power magnetosphere and storm time dynamics
Kinetic energy flux - shaping of magnetosphere, inefficient
Poynting flux - EM power delivered by reconnection, efficiency determined by angle of solar wind magnetic field and shaping of magnetosphere
72
What are effects of geo storms on technology
Geomagnetically induced currents
Atmospheric drag
Ionospheric disturbances
Magnetic altitude control
73
What is Faraday's law of induction and what is effect on field aligned current
Time varying magnetic field induces an electric field
Auroral electrojets are time varying currents that generate time varying magnetic field (Ampere's law)
This in turn generates an electric field
74
How does the field aligned current cause GICs and what impact do they have
Generates electric field causing GICs to flow in conducting material
Can flow in power systems as quasi-DC current
Flow through transformer winding, extra magnetisation when AC current in same direction as GIC, saturates iron core and excess heat dissipation damages system
Also affect cathode corrosion protection in pipelines, railways with automatic traffic signals and safety equipment, cable outages in telecoms
75
What is relationship between group and phase velocity with speed of sound and plasma frequency
When wave frequency is much greater than plasma frequency both velocities are equal to speed f light
If wave frequency is greater but in same order as plasma frequency, group velocity slows down as is smaller in same order as speed of light, phase velocity speeds up and is greater but in same order as light speed - photons move at group velocity
76
What is the refractive index physically representing
Ratio of wave speed in a vacuum to the wave speed in the medium
77
What causes ionospheric plasma
Ionisation of atmospheric molecules by solar photons
78
What is the refractive index of neutral atmosphere and how does the refractive index vary with electron density in ionosphere
N = 1
As altitude increases so does electron density up to maximum value, plasma frequency increases to this point and so refractive index decreases
79
How is a radio wave reflected in the ionosphere
The angle relative to ionosphere normal is 90 degrees at the apex of trajectory
80
What is the critical frequency of an ionospheric layer
Highest frequency that reflects at a vertical incidence
Vertical incidence has 0 degree angle
Refractive index is 0 when plasma frequency = wave frequency
Reflection occurs when phase velocity is infinite and group velocity is 0
81
When are waves absorbed and when are waves reflected in the ionosphere
Absorbed when wave frequency < plasma frequency
Reflected when wave frequency < critical frequency
82
How can ionospheric electron density be found
Reflection of radio waves
Ionosonde generates vertical radio pulses
Travel time is determined to calculate distance to reflection point
By varying pulse frequency a plot of frequency vs height can be obtained
83
What are the characteristics of ionosphere D layer
Lowest layer
Results from ionisation of nitrogen and oxygen by X-rays and NO by Lyman-alpha
Low altitude = high recombination rate
High concentration of neutrals
84
What does a high concentration of neutrals cause
Waves cause passing ions and electrons to oscillate and collide with neutrals
Collisions dampen oscillations so energy absorbed from radio wave
Lower frequency = greater damping and signal absorption
85
What causes the formation of the F layer
Ionisation of oxygen and hydrogen by UV
86
What is the lowest usable frequency
Frequency below which the D-layer absorbs the signal
87
What is the maximum usable frequency
Frequency above which the wave will not reflect in F-layer
88
What is the relationship between ionospheric effects and frequency
Effects decrease as frequency increases
89
How are radio blackouts caused
SEPs guided into polar regions
Collide with atmospheric neutrals and produce ions and electrons
Prevalent in D layer
90
How do GNSS determine their position at a specific time
Atomic clocks for accurate time
Use ground stations to determine position
91
How are GNSS used to for navigation
They emit signals containing satellite identifier, time of emission and position
Time delay in receiving determines distance to satellite
Trilateration to calculate position but 4th needed to correct receiver clock errors
92
What causes the difference between the geometric path of propagation and the actual path
Group velocity is different to speed of light so signal delayed in ionosphere compared to vacuum propagation
93
What is total electron content
Integral of electron density with respect to the signal path
Time delay is proportional to TEC and inversely proportional to square of wave frequency
94
When does excess range error occur
If distance between receiver and GNSS is determined using vacuum speed of light
Error increases with non-vertical incidence
95
How can TEC be estimated and why does this work
Using two frequencies of signal
Ionosphere is dispersive with frequency dependence
96
What is ionising radiation
Has sufficient energy to free electrons
E.g. UV, X-rays, gamma rays
Causes displacement damage and total ionisation dose damage
97
What is non-ionising radiation
Sufficient energy to produce damage by heat or atomic damage
E.g. radio waves, microwaves, visible light
Causes non-ionising thermal damage, displacement damage and cell damage
98
What is total ionisation dose damage
Cumulative changing of electrical parameters
Single event phenomena are circuit upsets or changes
99
What is the relationship between electrical components and radiation resistance
Passive components are more resistant to radiation (resistors, capacitors, inductors)
Active components are more susceptible to radiation (transistors, integrated circuits, diodes)
100
What does the threshold for ionising radiation mean
The energy required to remove external electron
Dependent on the atom
101
What is the photoelectric effect
Interactions between incident photon and bound electron
Electron receives whole energy of photon and is ejected from atom
Dominant for photons < 50 keV
102
What is Compton scattering
Electron is ejected after receiving fraction of photon energy
Rest of energy is emitted as a lower energy photon
Dominant energy transfer process between 50 keV and 5 MeV
103
What is pair production
Interaction of incident photon and atomic nucleus results in electron-positron pair
Dominant for photons > 5 MeV
104
What are the characteristics of photon flux absorption
Absorption increases with thickness of material
Increases with linear attenuation coefficient
Coefficient decreases for higher energy photons
105
How are spacecraft surfaces charged
Sun lit surfaces are positively charged due to photoelectric effect
Shaded surfaces are negatively charged due to electron flux
Occurs when there is an imbalance of electric currents
106
How is spacecraft potential determined
Balance of different currents e.g. incidence electron and ion current, photoelectron current, secondary emitted electron currents
A system in equilibrium has 0 total electric current
107
How is spacecraft charging mitigated
Set maximum potential difference
Electrically connect structural and mechanical parts with lower resistance to ground them
108
When is a particle's energy increased
When electric field is in same direction of motion
109
What is magnetic rigidity of a charged particle
Quantifies the ability of a charged particle to penetrate magnetic field
Energy of a particle is the sum of its rest mass and its kinetic energy
110
What is magnetic rigidity cut-off
Particles with high magnetic rigidity are harder for geomagnetic field to deflect
Cut-off corresponds to threshold value of magnetic rigidity to access a particular point in region of magnetic field
Usually expressed in GV
111
What is excitation and de-excitation
Charged particle transfers energy to an electron in the atom, not enough to ionise but increases electron energy state
Electron emits a photon when returning to original energy state
112
What is Bremsstrahlung radiation
Breaking radiation
Charged particle transfers energy to nucleus accelerating it
Nucleus slows down by releasing radiation
113
What is electrostatic force
Main mechanism of interaction between a charged particle that travels through continuous medium and atoms of the medium
114
What is stopping power and range of a material
Energy lost per unit of distance when a charged particle moves through medium
Depth of penetration of a particle
115
What is the effect of radiation on electronic components
Production of impurities
Radiolysis (chemical breakdown)
Ionisation
Atom displacement within lattice structure
116
What types of damage from radiation are there
Single event effects (non-destructive and potentially destructive)
Deep dielectric charging/discharge
Displacement damage
Total ionising dose
117
Why do we need to forecast space weather what do we need to forecast
To mitigate effects on technological systems that are important for infrastructure
Parameters that affect technology operation and indices that characterise strength of disturbance
118
What methods are there to forecast
Physics/first principles based - taking physical knowledge, first principles and assumptions to come up with equations that describe situations, build these into numerical code for models
Data driven - taking input data, physical knowledge and output data to come up with an algorithm to model situations, use physical understanding to see how well it fits
119
Why can physics based models be computationally expensive
Models of complex systems often don't have exact solutions and have to be solved numerically with discretisation in time and space
120
What types of models come under data driven branch
Linear regression
System identification
Machine learning
121
Which Lagrange point is used to forecast and why
L1
Solar wind will impact on satellite there around an hour before impacting on earth
122
What is the range of measurement for prediction efficiency
Minus infinity to 1
123
What is the range of measurement for correlation
-1 to 1
124
What are binary skill scores
Metrics deduced from prediction of a binary event (event happens or it doesn't)
125
What do the 4 quadrants in a binary skill score represent
X - successful predictions the event happens (Hit)
Z - false prediction the event happens (False alarm)
Y - incorrect prediction the event doesn't happen (Miss)
W - successful prediction the event doesn't happen (Correct rejection)
126
What challenges exist with space weather forecasting
Reliable forecasts from the Sun to L1 to allow longer lead time
Forecasting GICs
Forecasting strong solar flares and CME eruptions
127
How is the phase velocity of a dispersive wave found
Divide the wave frequency by k (wave number)
128
How is the group velocity of a dispersive wave found
Take the partial derivative of wave frequency with respect to k
129
What is the cross product of two vectors A x B
Equal to determinant of 3x3 matrix with top row elements equal to x, y, z components of A, middle row elements equal to x, y, z components of B, bottom row elements equal to directional vectors in x, y, z direction
130
What calculations must be done for plasma criteria
Calculate the Debye length and check << spatial scale
Calculate electron density * Debye length cubed and check >> 1
Calculate plasma frequency * period of collisions and check >> 1
131
What calculations must be done for guiding centre approximation
Calculate cyclotron/Larmor frequency and check > wave frequency
Calculate Larmor radius and check << spatial scale to find perpendicular velocity requirement for GCA
132
What is the pitch angle equal to mathematicaly
Arctan of perpendicular/parallel velocity
133
What does the first adiabatic invariant mean and what can it be used for
Ratio of perpendicular kinetic energy/magnetic field strength is constant
Can find the velocity or field strength at a point given conditions
134
How is the angle or field strength at a mirror point found
Use first adiabatic invariant
Set up energy conservation
Replace mirror perpendicular velocity using adiabatic invariant
Rearrange for the parallel velocity at mirror point and set equal to 0
135
How is the spatial scale of a system calculated and what is done to compare with Larmor radius
Lambda = 2 * pi/k
Half * lambda to compare with Larmor radius
136
What is the speed of sound in plasma
sqrt(2*kb*T/m)
137
How are questions about the position of day time sub solar magnetopause solved
Set the dynamic ram pressure equal to the terrestrial magnetic field pressure
Find the strength of magnetic field using known equation and coefficient factor
Rearrange for the parameter of interest e.g. solar wind velocity
138
What is the relationship between magnetic field strength at points and the pitch angle at points
B1/B2 = (sin(a1)/sin(a2)^2
139
What is the thermal velocity of solar wind and how is it calculated
Vth = sqrt(2*kb*t/m)
Equate kinetic energy and thermal energy
140
What is the escape velocity and how is it calculated
Vesc = sqrt(2*G*M/r)
Equate kinetic energy with gravitational potential energy
141
How is the minimum electron density for radio wave reflection found
Use Snell's law for reflection so sin(incident angle) = N_reflection - because N_incidence = 1 and sin(reflection) = sin(90) = 1
Replace Nr with the ratio of c/Vph and square
Replace sin^2 + 1 = cos^2 and multiply wave frequency across
Replace plasma frequency with known equation
Rearrange for electron density
Set incidence angle to 0 for minimum value (cos(0) = 1)
142
How is the time delay in ionosphere calculated
Actual path minus geometric path is integral of 1/Vgr - 1/c
Replace for value of Vgr and factor out 1/c
Use binomial approximation to give time delay = 1/2cf^2 * integral of plasma frequency^2 ds
Factor everything out until it is just the integral of electron density which is equal to TEC
143
How is the TEC calculated
The time of arrival for a signal is t1 = R/c + time delay_1
Find the time delay using t1 - t2 and rearrange for TEC
144
How is the range of communication found
Time of arrival approximated is tv = R/c = t1 - time delay_1
Input expression for time delay and rearrange for range R
145
What are the photon relations for angular frequency, speed of light and wave number
w = 2 * pi * f
c = f * wavelength
k = 2 * pi * wavelength
146
What are the photon relations for energy and momentum
E = h * f
E/h = c/wavelength
E = h * w/2 * pi
p = h * k/2 * pi
Wavelength = h/p
147
What is the equation for flux density attenuation
I = I0 * e^(-mu * x)
148
How is magnetic rigidity calculated
Magnetic rigidity is R = p *c/q
Energy is E = Ek + mc^2 (Energy = kinetic energy + rest mass)
Equation is E^2 = (pc)^2 + (mc^2)^2
Insert energy sum into equation and expand out then rearrange to get pc = sqrt(Ek^2 + 2*Ek*m*c^2)
Insert value of pc into magnetic rigidity equation
149
How is the expression for drift velocity calculated using the GCA
Establish particle position vector as sum of Larmor radius vector and distance from centre of Larmor rotation
Find the equation of motion under magnetic field and gravitational force influence
Average the motion of period of Larmor rotation so all values of Larmor radius vector and derivatives are 0
Decompose velocity into perpendicular and parallel components
Product of two parallel vector is zero
This leaves only perpendicular components for parallel acceleration is 0 and parallel velocity is constant and 0 because of initial conditions
Assume perpendicular velocity is constant so perpendicular acceleration is 0
Take cross product with B
Use cross product relation to eliminate dot product of perpendicular vectors (equal to 0)
Rearrange for perpendicular velocity
150
In calculator which standard deviation is used
Sample standard deviation
Sx
4th option
