### The Ionosphere

May 13, 2013

As a teenager of my generation, my choices for entertainment were limited. There was no Internet, there were just three television stations, two of which were very fuzzy, and the local radio stations played music that could have been background music at an ice skating rink or in an elevator. As a consequence, I did a lot of reading, which, in retrospect, wasn't a bad thing. Now, I can split infinitives with the best bloggers.

Another refuge besides reading was AM radio after sunset. The US AM radio broadcast band presently has frequency assignments between 540 and 1700 kilohertz (kHz); but, at that time, only between 540 kHz to 1600 kHz. Why after sunset? At night, the only active layer of Earth's ionosphere is its highest layer, the F-layer, and this allows long distance AM radio reception.

The F-layer consists of ionization at altitudes from about 120 miles (200 kilometers) to about 310 miles (500 km). This ionization will reflect radio waves, so transmissions from about double these distances can be received after a single "bounce." This allowed my reception of the more powerful Detroit (450 miles) and Chicago (650 miles) radio stations from the west, and Boston (250 miles) radio stations from the east.

The ionosphere doesn't reflect all radio frequencies, just those above a certain wavelength. The electrons in the ionosphere are ineffective at reflecting radio waves above a certain critical frequency, which is a simple function of the square-root of the electron density. Under some conditions, it's possible for all radio waves below about 50 megahertz (MHz) to be reflected; but, since the very high frequencies (VHF) are defined to start at 30 MHz, we usually consider that point to be a useful cut-off.

So, we're blessed in two ways. First, the easily generated frequencies (those used by Marconi and his colleagues), propagated much farther than expected. Then, the transparency of the ionosphere above a certain frequency means that the Earth is not isolated from the radio universe. At high enough frequencies, we still have radio astronomy and the ability to signal our satellites and spacecraft.

Radio astronomy pioneer, Grote Reber, who was the world's second radio astronomer (Karl Jansky was the first), decided that he wasn't going to let the ionosphere come between him and the low frequency radio waves of outer space. I wrote about Reber in a previous article (LOFAR, Not LOTR, March 2, 2011).

Grote Reber's first radio telescope antenna, built at his home in Wheaton, Illinois, a suburb of Chicago, in 1937.

Reber was an an amateur radio operator (W9GFZ). He built this 31.4 foot diameter parabolic antenna from iron, which was a cheap, conducting metal.

(NRAO photograph by Grote Reber, via Wikimedia Commons.)

Reber's first step in his quest for extraterrestrial radio signals around the AM broadcast frequencies was to move to Tasmania. In that region of the Earth, most of the ionosphere will neutralize during long and cold winter nights. Tasmania was also removed from much of mankind's interfering radio signals. Reber made his low frequency observations, generally in the range 0.3-3 MHz, with support from the University of Tasmania.

A recently commissioned radio telescope, LOFAR, has been designed for observations in the 10-240 MHz frequency range, which includes frequencies below the ionospheric cutoff. LOFAR is composed of thousands of antennas distributed across The Netherlands, Germany, Great Britain, France and Sweden. Digital signal processing by a Blue Gene/P supercomputer combines these signals into one huge interferometer.

Because of its low frequency monitoring capability, LOFAR can observe changes in ionospheric transparency. One application of this is detection of distant gamma ray bursts. Gamma radiation incident on Earth's atmosphere will cause additional ionization, so extraterrestrial signals will be blocked, and the strength of long-distance terrestrial signals will be enhanced.

This effect has been noted for several sources; namely, SGR 1806-20, a magnetar and gamma ray repeater detected on December 27, 2004;[vlf.stanford] GRB 030329, a gamma-ray burst detected on March 29, 2003; GRB 830801, detected on August 1, 1983; XRF 020427, an Xray flare detected on April 27, 2002; and a flare from SGR 1900+14, a soft gamma ray repeater, detected on Aug. 27, 1998.[4]

These gamma ray events can pack quite a punch. SGR 1806-20 is about 50,000 light years from Earth, but it ionized the atmosphere down to about 50,000 feet (20 kilometers), nearly down to the level of commercial aircraft.[5] The signal had a peak lasting a few seconds, followed by smaller intensity signals for an hour. This gamma ray event increased the density of ions at 60 kilometer altitude by a huge factor, from 0.1 to 10,000 free electrons per cubic foot.[5]

The ionosphere also has small-scale, local variations in its properties. One example is the ionization created by meteors,[6] but the transition time from the daytime to the nighttime ionosphere can be turbulent, with violent ionospheric storms evident in the equatorial F-layer a few hours after sunset. These storms can affect even high frequency communications.[7]

Local disturbances in the ionosphere cause problems for even higher frequency signals, such as those of the Global Positioning System.

(Air Force Research Laboratory image.)

NASA launched a sounding rocket mission, called EVEX (Equatorial Vortex Experiment), on May 1-9 from the Kwajalein Atoll in the Marshall Islands to study these ionospheric disturbances. One portion of EVEX consisted of two sounding rockets, launched a few minutes apart. One of these sounding rockets traveled to a high altitude, and the other to about half that altitude, to record data about electric field strength and the density of the charged particles.[7-8]

These rockets also released a tracer chemical, trimethylaluminum, which decomposes into fine particles of aluminum oxide. The tracer stream was optically triangulated to show wind direction.[7] This wind, called a neutral wind, is thought to be an important element in the formation of ionospheric storms.[7]

Stanford University has a program in which high school students can participate in ionosphere research. High schools can participate in the Space Weather Monitor Program by installing an inexpensive receiver to monitor a very low frequency (VLF) transmitter. Data are collected on a personal computer, and they are uploaded to the program site.[9]

### References:

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