1. the Ionosphere as a Plasma
Begin

2. Questions Why is it called the ionosphere?
How do we study the ionosphere?
What can we measure in the ionosphere?

3. Why the Ionosphere?
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UV light from the sun hits atoms in Earth’s upper atmosphere. The energy from this light knocks an electron off the atom, leaving a free electron and an Ion. This type of ionized gas is called a plasma. Unlike other gases, it can conduct an electric charge and is affected by magnetic fields. (learn more)

4. How high up are the ions?
Upper altitudes have fewer atoms to ionize. Less radiation reaches lower altitudes, and there ions recapture electrons more easily.
Most ions are created at an intermediate height.
Once ionized, the ions distribute themselves according to their weight with the heaviest closest to the Earth.

5. Just as temperatures define the layers of the atmosphere, electron concentrations define the different layers of the ionosphere.

6. Each layer plays an important role in absorbing some of the sun’s radiation.

7. Ions and Electrons move around in the Ionosphere
Above 80 km, ions are pushed around by collisions with a wind of neutral particles. Electrons are smaller and are able to avoid these collisions. Instead, they spiral around magnetic field lines. This causes a current at this altitude known as the electrojet (learn more).
Above 200 km, the neutral wind is too sparse to push ions around. They too begin to spiral around the magnetic field lines.
The frequency of these rotations is the plasma’s cyclotron frequency (learn more).
As a charged particle rotates about a field line, it emits radiation.
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8. this motion contributes to day - night differences in the ionosphere
Daytime – In the northern hemisphere, winds blow from the hot south to the cool north and push the spiraling ions down.
Nighttime – Winds blow from north to south and push the spiraling ions up
wind
wind
Daytime
Nighttime

9. How do we study the ionosphere
Incoherent Scatter
Heating facilities
Rockets & Spacecraft

10. Incoherent Scattering
Reflecting photons off of electrons
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Some of the energy from the photon is converted to the electron’s kinetic energy. The reflected photon has less energy and therefore a longer wavelength.
The change in wavelength of the photon is due to the Compton Effect (learn more). For reflection, the change in wavelength is
Dl = 2 h / c me
h = Planck’s constant (6.63 * J sec)
c = speed of light (3.00 * 108 m/s)
me = mass of electron (9.11 * kg )

11. Ne = number of electrons per cubic meter
Plasma frequency
The electron in the previous slide was pushed to the right. As it moves from its original position, it is attracted back by the surrounding positive ions. (learn more)
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It will oscillate around its equilibrium position. The frequency of these oscillations is called the plasma frequency.
freqplasma = 9 √Ne
Ne = number of electrons per cubic meter

12. Reflections can be used to measure the height and density of the ionosphere
The photon is reflected when its frequency equals the plasma frequency.
The longer it takes for the wave to be reflected back, the higher up the plasma layer.
Current research is being conducted at Millstone Hill (learn more)
Lower frequency
Higher frequency

13. Heating Facilities
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These programs pump the ionosphere with so much energy that the temperature of a small part of it increases. Radio telescopes then study the plasma as it cools down. Current research is being conducted by EISCAT (learn more).

14. Rockets and Spacecraft
Since the 1950’s, scientists have been able to probe the ionosphere directly with rockets.
They have also been able to look at it from space with man-made satellites Although it may look like the astronauts in the space shuttle are in “outer space” they are still in the ionosphere. There is plenty of matter and plenty of activity going on outside the shuttle. Current research is being conducted by NASA (learn more).

15. What can we measure?
The incoherent scattering technique uses a radio telescope to fire radiation at the ionosphere. The telescope then listens for the echo. It records the reflected signal which typically looks something like this:

16. With it, we can measure density ion temperature electron temperature
electron drift (current)
velocity of neutral particles (wind)
electric field

17. Density
The density of a region of plasma is proportional to the total power reflected back. The top graph was made of a denser region than the bottom graph

18. Ion temperature
Cool Ions
The velocity of the ions are proportional to the width of the signal. This is due to Doppler broadening. An ion’s temperature can be calculated from its velocity and its mass with the following equation (learn more):
Hot Ions
m v2 = 3 k T
m – mass of ion
v – velocity of ion
k – Boltzmann’s constant (1.38 * J/K)
T – temperature in Kelvins

19. Electron temperature
Electrons are generally hotter than ions. Their relative temperatures are proportional to the relative heights of the peaks and valley on the graph
Hot electrons
Cool electrons

20. Electron Drift
Electrons are much lighter than ions and can therefore move much faster. If a group of electrons are all moving in the same direction, an electric current is established. The reflected signal will then be Doppler shifted.

21. neutral wind velocity
Below 200 km, the ionosphere is so dense that ions and neutral particles collide frequently enough to reach thermal equilibrium – the same temperature. The incoherent scattering techniques described above can be used at these heights to measure the temperature of the neutral gases and thus their velocities.

22. Electric Field
An electric field in the ionosphere can be measured by the relative polarization of the collected radiation.
Vertical
Right handed
Horizontal
left handed