The history of High-Energy Astrophysics may be said to have begun in 1912 with Hess's discovery of Cosmic Rays showering in the upper reaches of Earth's atmosphere, though what we would regard today as HEA research emerged in the 1960's with the coming of the space programme. Most methods of detecting high-energy photons (which may come from a variety of sources such as the Sun, active galaxies, supernovae and so on) rely on the production of electrons resulting from collision with the incoming high-energy particles. Depending on the energy of these particles, different methods of detection can be used because higher energy levels give rise to different phenomena. Compton Scattering can be detected at energies between 1 - 30 MeV (Mega electron volts, i.e., 1 000 000 to 30 000 000 electron Volts) and is a cascading effect produced by incoming energetic photons interacting with atomic nuclei as in the diagram below.
|With higher energies than this, at the intensity of gamma-rays, the phenomenon of pair scattering obtains. This is similar to Compton scattering, but with the production of an electron and its anti-particle, a positron. The production of this pair results in the annihilation of the incoming particle.|
In addition, there are several other projects in the pipeline whilst not strictly HEA by definition, nevertheless relate to non-visual methods of detection, such as the AMANDA project in Antarctica which will perform neutrino astronomy, and space-based gravitational wave detectors for such phenomena as coalescing black holes. Space is a much better place to observe gravitational waves due to the presence of tides and Earth tremors of all sizes on terra firma.