Ultra-high-energy gamma ray
Ultra-high-energy gamma rays are gamma rays with photon energies higher than 100 TeV (0.1 PeV). They have a frequency higher than 2.42 × 1028 Hz and a wavelength shorter than 1.24 × 10−20 m. As of 2014[update], they are theoretical only and have not been detected. The highest energy astronomical sourced gamma rays detected are very-high-energy gamma rays.
Ultra-high-energy gamma rays are of importance because they may reveal the source of cosmic rays. Discounting the relatively weak effect of gravity, they travel in a straight line from their source to an observer. This is unlike cosmic rays which have their direction of travel scrambled by magnetic fields. Sources that produce cosmic rays will almost certainly produce gamma rays as well, as the cosmic ray particles interact with nuclei or electrons to produce photons or neutral pions which in turn decay to ultra-high-energy photons.
The ratio of primary cosmic ray hadrons to gamma rays also gives a clue as to the origin of cosmic rays. Although gamma rays could be produced near the source of cosmic rays, they could also be produced by interaction with cosmic microwave background by way of the Greisen–Zatsepin–Kuzmin limit cutoff above 50 EeV.
Ultra-high-energy gamma rays interact with magnetic fields to produce positron electron pairs. In the earth's magnetic field, a 1021 eV photon is expected to interact about 5000 km above the earth's surface. The high-energy particles then go on to produce more lower energy photons that can suffer the same fate. This effect creates a beam of several 1017 eV gamma ray photons heading in the same direction as the original UHE photon. This beam is less than 0.1 m wide when it strikes the atmosphere. These gamma rays are too low-energy to show the Landau–Pomeranchuk–Migdal effect. Only magnetic field perpendicular to the path of the photon causes pair production, so that photons coming in parallel to the geomagnetic field lines can survive intact till they meet the atmosphere. These photons that come through the magnetic window can make a Landau–Pomeranchuk–Migdal shower.
|1||1||0.1602 aJ||241.8 THz||1.2398 μm||near infrared photon||for comparison|
|100 GeV||1 × 1011||0.01602 μJ||2.42 × 1025 Hz||1.2 × 10−17 m||Z boson|
|1 TeV||1 × 1012||0.1602 μJ||2.42 × 1026 Hz||1.2 × 10−18 m||flying mosquito||produces Cherenkov light|
|10 TeV||1 × 1013||1.602 μJ||2.42 × 1027 Hz||1.2 × 10−19 m||air shower reaches ground|
|100 TeV||1 × 1014||0.01602 mJ||2.42 × 1028 Hz||1.2 × 10−20 m||ping pong ball falling off a bat||causes nitrogen to fluoresce|
|1 PeV||1 × 1015||0.1602 mJ||2.42 × 1029 Hz||1.2 × 10−21 m|
|10 PeV||1 × 1016||1.602 mJ||2.42 × 1030 Hz||1.2 × 10−22 m||potential energy of golf ball on a tee|
|100 PeV||1 × 1017||0.01602 J||2.42 × 1031 Hz||1.2 × 10−23 m||penetrate geomagnetic field|
|1 EeV||1 × 1018||0.1602 J||2.42 × 1032 Hz||1.2 × 10−24 m|
|10 EeV||1 × 1019||1.602 J||2.42 × 1033 Hz||1.2 × 10−25 m||air rifle shot|
- Search for Galactic PeV Gamma Rays with the IceCube Neutrino Observatory
- Air shower detection of diffuse PeV gamma-rays
- Aharonian, Felix (24 August 2010). "The Fascinating TeV Sky" (PDF). WSPC - Proceedings. Retrieved 27 November 2011.
- Vankov, H. P.; Inoue, N.; Shinozaki, K. (2 February 2008). "Ultra-High Energy Gamma Rays in Geomagnetic Field and Atmosphere" (PDF). Retrieved 3 December 2011.