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5 February 2021.
Ultraviolet wavelengths.
Ultraviolet astronomy.
UV Communications and Emissions.
The All Frequency Database Index is here: http://sites.google.com/site/somaliaamateurradio/somaliaphotos10
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26. Ultraviolet Communications and Emissions and Somalia photos 45.
26.
Ultraviolet.
Ultraviolet communication.
Ultraviolet communication systems.
Ultraviolet communications.
Ultraviolet communications systems.
Ultraviolet research.
Ultraviolet experimentation.
Ultraviolet astronomy.
Astronomy on Ultraviolet frequencies.
Astronomy on Ultraviolet wavelengths.
750,000 – 30,000,000 GHz.
Ultraviolet electromagnetic radiation.
Electromagnetic ultraviolet radiation.
Frequency 750,000 – 30,000,000 GHz.
Wavelength 400 – 10 nm.
The frequency of ultraviolet is 750,000 GHz – 30,000,000 GHz.
The frequency of ultraviolet is 750 THz – 30,000 THz.
The wavelength of ultraviolet is 400 nm – 200 nm.
Ultraviolet - vacuum ultraviolet - extreme ultraviolet 10 nm – 400 nm (0.750 THz – 30000 THz).
10 – 400 nm (0.750 – 30000 THz).
Ultraviolet 400 – 200 nm (0.750 – 1.5 PHz).
Ultraviolet 400 – 200 nm (0.750 PHz – 1.5 PHz).
Ultraviolet 0.4 – 0.2 µm (0.750 – 1.5 PHz).
Ultraviolet 0.4 µm – 0.2 µm (0.750 PHz – 1.5 PHz).
Ultraviolet 400 – 200 nm (750 – 1500 THz).
Ultraviolet 400 µm – 200 µm (750 THz – 1500 THz).
Ultraviolet 0.4 – 0.2 µm (750 – 1500 THz).
Ultraviolet 0.4 µm – 0.2 µm (750 THz – 1500 THz).
Ultraviolet 400 – 200 nm (750000 – 1500000 GHz).
Ultraviolet 400 µm – 200 µm (750,000 GHz – 1,500,000 GHz).
Ultraviolet 0.4 – 0.2 µm (750000 – 1500000 GHz).
Ultraviolet 0.4 µm – 0.2 µm (750,000 GHz – 1,500,000 GHz).
Vacuum ultraviolet 200 – 100 µm (1.5 – 3 PHz).
Vacuum ultraviolet 200 µm – 100 µm (1.5 PHz – 3 PHz).
Vacuum ultraviolet 0.2 – 0.1 µm (1.5 – 3 PHz).
Vacuum ultraviolet 0.2 µm – 0.1 µm (1.5 PHz – 3 PHz).
Vacuum ultraviolet 200 – 100 nm (1,500 – 3,000 THz).
Vacuum ultraviolet 200 nm – 100 nm (1,500 THz – 3,000 THz).
Vacuum ultraviolet 0.2 – 0.1 µm (1500 – 3000 THz).
Vacuum ultraviolet 0.2 µm – 0.1 µm (1,500 THz – 3,000 THz).
Extreme ultraviolet 100 nm – 10 (3 – 30 PHz).
Extreme ultraviolet 100 nm – 10 nm (3 PHz – 30 PHz).
Extreme ultraviolet 0.1 – 0.01 µm (3 – 30 PHz).
Extreme ultraviolet 0.1 µm – 0.01 µm (3 PHz – 30 PHz).
Extreme ultraviolet 100 – 10 nm (3,000 – 30,000 THz).
Extreme ultraviolet 100 nm – 10 nm (3,000 – 30,000 THz).
Extreme ultraviolet 0.1 – 0.01 µm (3000 – 30000 THz).
Extreme ultraviolet 0.1 µm – 0.01 µm (3,000 THz – 30,000 THz).
Introduction to ultraviolet.
https://www.tnuda.org.il/en/table-use-frequencies
https://en.wikipedia.org/wiki/Optical_wireless_communications
https://www.photonics.com/Articles/Ultraviolet_Communications_Framework_Will_Help/a66050
http://science.hq.nasa.gov/kids/imagers/ems/uv.html
http://en.wikipedia.org/wiki/Ultraviolet
https://www.survival.org.au/radio.php
The Effect of Ultraviolet Radiation on the Signal Strength of Amateur Radio Satellite Transmissions.
https://csef.usc.edu/History/2018/Projects/S1005.pdf
https://radiojove.gsfc.nasa.gov/education/educ/radio/tran-rec/exerc/iono.htm
https://www.autodesk.com/products/eagle/blog/beginners-guide-ham-radio-make/
Ultraviolet telescopes.
https://www.sciencedirect.com/topics/earth-and-planetary-sciences/ultraviolet-telescopes
Solar Radio emission.
Ultraviolet astronomy looks at ultraviolet wavelengths.
The Sun photographed at the ultraviolet wavelength of 304 Angstrom (30.4 nm).
The sun seen at the ultra violet frequency of 9,861,594 GHz by the observatory in space known as Soho (Solar and Heliospheric Observatory).
The optical surface of the Sun has a temperature of about 6,000 degrees K.
The temperature above the Sun’s surface rises to 1,000,000 degrees Kelvin (1.8 million degrees Fahrenheit).
Every feature in the image is a result of the magnetic field structure of the Sun.
The hottest areas appear almost white, while the darker red areas indicate cooler temperatures.
Photo 28 June 2000 thanks to SOHO (ESA & NASA).
The Sun as seen in Extreme Ultraviolet.
The Sun as seen by the Extreme Ultraviolet Imaging Telescopes in Space known as STEREO (Solar TErrestrial RElations Observatory’s).
A photo of The Sun as seen in Extreme Ultraviolet wavelengths.
Courtesy of NASA’s STEREO mission.
Introduction to STEREO, the telescopes in Space that look at the Sun.
The Sun's surface before an explosion.
The Sun seen from Space in Ultraviolet before an explosion.
The Sun as seen by the Extreme Ultraviolet Imaging Telescope in Space known as STEREO (Solar TErrestrial RElations Observatory’s.
The Sun’s atmosphere are at temperatures around one million Kelvin (1.8 million degrees Fahrenheit).
The extreme ultraviolet light is not visible to the human eye, so it is represented here in blue.
The charged particles (mostly extremely hot protons and electrons) rising from the active region create a strong magnetic field that pulls the particles into the loops seen here.
Over time, magnetic stress builds in the Sun’s atmosphere until the energy is released in a massive explosion (see the next photo).
The explosion sends a giant cloud of charged particles (a coronal mass ejection) and X-ray solar flares hurtling into space with a force comparable to a billion megaton nuclear bombs.
When the charged particles and X-rays arrive at Earth, they can disrupt communications and power systems and are a threat to satellites and astronauts in space.
The active regions that produce flares are visible from Earth as Sun spots, but the streaming particles emitting ultraviolet light in this image are only visible from space.
Just one week after this image was taken, the Sun spot shown here produced a strong solar flare.
Courtesy of NASA’s STEREO mission.
STEREO, the telescope in Space that looks at the Sun.
Explosion on the Sun photographed at ultraviolet wavelength.
On the 4 January 2002 a Coronal Mass Ejection (CME) event was seen on the Sun on Extreme Ultra Violet wavelengths by the observatory in space known as Soho (Solar and Heliospheric Observatory).
Photo 4 January 2002 thanks to SOHO (ESA & NASA).
Introduction to SOHO, the telescope in Space that looks at the Sun.
http://en.wikipedia.org/wiki/SOHO_spacecraft
See current images of the Sun on your computer. See online how the Sun looks now.
How to build a radio station in Somalia.
How to build a radio station antenna in Somalia.
The completed short wave radio broadcast and amateur radio training antenna in Galkayo, North East Somalia.
The completed Radio Free Somalia (“Free for all to use” known later as Radio Galkayo) short wave radio antenna and the front wall of the Galkayo Police station, Galkayo, North East Somalia in August 1994.
Notice the spelling Boliska (The Somali language does not have the letter P, in Somali a P is written as B).
North East Somalia became the Puntland State of Somalia on the 1st August 1998.
(Photo Sam Voron 6O0A, VK2BVS).
Index https://sites.google.com/site/somaliaamateurradio/index1
Contact: Sam Voron VK2BVS, 6O0A.
Email somaliahamradio@yahoo.com
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