Gamma-ray astronomy

related topics
{math, energy, light}
{ship, engine, design}
{album, band, music}

Gamma-ray astronomy is the astronomical study of the cosmos with gamma rays. Gamma-rays are the most energetic form of light that travel across the universe for incredible distances and have the smallest wavelength of any other wave in the electromagnetic spectrum. Gamma-rays are created by and allow us to detect and observe celestial events such as supernova explosions, destruction of atoms, black holes and even the decay of radioactive material in space. [1]


Early history

Long before experiments could detect gamma rays emitted by cosmic sources, scientists had known that the universe should be producing these photons. Work by Eugene Feenberg and Henry Primakoff in 1948, Sachio Hayakawa and I.B. Hutchinson in 1952, and, especially, Philip Morrison in 1958[2] had led scientists to believe that a number of different processes which were occurring in the universe would result in gamma-ray emission. These processes included cosmic ray interactions with interstellar gas, supernova explosions, and interactions of energetic electrons with magnetic fields. However, it was not until the 1960s that our ability to actually detect these emissions came to pass.[3]

Most gamma rays coming from space are absorbed by the Earth's atmosphere, so gamma-ray astronomy could not develop until it was possible to get detectors above all or most of the atmosphere using balloons and spacecraft. The first gamma-ray telescope carried into orbit, on the Explorer 11 satellite in 1961, picked up fewer than 100 cosmic gamma-ray photons. They appeared to come from all directions in the Universe, implying some sort of uniform "gamma-ray background". Such a background would be expected from the interaction of cosmic rays (very energetic charged particles in space) with interstellar gas.

The first true astrophysical gamma-ray sources were solar flares, which revealed the strong 2.223 MeV line predicted by Morrison. This line results from the formation of deuterium via the union of a neutron and proton; in a solar flare the neutrons appear as secondaries from interactions of high-energy ions accelerated in the flare process. These first gamma-ray line observations were from OSO-3, OSO-7, and the Solar Maximum Mission, the latter spacecraft launched in 1980. The solar observations inspired theoretical work by Reuven Ramaty and others.[4]

Full article ▸

related documents
Axial tilt
Terrestrial planet
Compton scattering
Zero-point energy
Hydrogen atom
Eta Carinae
Equatorial bulge
Elementary particle
Weak interaction
Weakly interacting massive particles
Quantum gravity
2 Pallas
Ganymede (moon)
Sudbury Neutrino Observatory
Rayleigh scattering
Proton decay
Gauss's law
Huygens–Fresnel principle