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Bhabha derived an expression for the probability of scattering positrons by electrons, a process now known as Bhabha scattering. His classic paper, jointly with Walter Heitler , published in described how primary cosmic rays from space interact with the upper atmosphere to produce particles observed at the ground level. Bhabha and Heitler explained the cosmic ray shower formation by the cascade production of gamma rays and positive and negative electron pairs.

Measurements of the energy and arrival directions of the ultra-high-energy primary cosmic rays by the techniques of density sampling and fast timing of extensive air showers were first carried out in by members of the Rossi Cosmic Ray Group at the Massachusetts Institute of Technology.

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A huge air shower experiment called the Auger Project is currently operated at a site on the pampas of Argentina by an international consortium of physicists. Their aim is to explore the properties and arrival directions of the very highest-energy primary cosmic rays. Currently the Pierre Auger Observatory undergoes an upgrade to improve its accuracy and find evidence for the yet unconfirmed origin of the most energetic cosmic rays.

Since then, numerous satellite gamma-ray observatories have mapped the gamma-ray sky.

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The most recent is the Fermi Observatory, which has produced a map showing a narrow band of gamma ray intensity produced in discrete and diffuse sources in our galaxy, and numerous point-like extra-galactic sources distributed over the celestial sphere. Early speculation on the sources of cosmic rays included a proposal by Baade and Zwicky suggesting cosmic rays originated from supernovae.


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Babcock suggested that magnetic variable stars could be a source of cosmic rays. Sekido et al. Later experiments have helped to identify the sources of cosmic rays with greater certainty. In , a paper presented at the International Cosmic Ray Conference ICRC by scientists at the Pierre Auger Observatory showed ultra-high energy cosmic rays UHECRs originating from a location in the sky very close to the radio galaxy Centaurus A , although the authors specifically stated that further investigation would be required to confirm Cen A as a source of cosmic rays. In , supernovae were said to have been "pinned down" as a source of cosmic rays, a discovery made by a group using data from the Very Large Telescope.

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In the Pierre Auger Collaboration published the observation of a weak anisotropy in the arrival directions of the highest energy cosmic rays. This implies that there must be a transition energy from galactic to extragalactic sources, and there may be different types of cosmic-ray sources contributing to different energy ranges. Cosmic rays can be divided into two types, galactic cosmic rays GCR and extragalactic cosmic rays , i. However, the term "cosmic ray" is often used to refer to only the extrasolar flux. Cosmic rays originate as primary cosmic rays, which are those originally produced in various astrophysical processes.

The latter three of these were first detected in cosmic rays. Primary cosmic rays primarily originate from outside the Solar System and sometimes even the Milky Way. When they interact with Earth's atmosphere, they are converted to secondary particles. Cosmic rays made up of charged nuclei heavier than helium are called HZE ions. Due to the high charge and heavy nature of HZE ions, their contribution to an astronaut's radiation dose in space is significant even though they are relatively scarce.

This abundance difference is a result of the way secondary cosmic rays are formed. Carbon and oxygen nuclei collide with interstellar matter to form lithium , beryllium and boron in a process termed cosmic ray spallation. Spallation is also responsible for the abundances of scandium , titanium , vanadium , and manganese ions in cosmic rays produced by collisions of iron and nickel nuclei with interstellar matter.

At high energies the composition changes and heavier nuclei have larger abundances in some energy ranges. Current experiments aim at more accurate measurements of the composition at high energies. These do not appear to be the products of large amounts of antimatter from the Big Bang, or indeed complex antimatter in the universe.

Rather, they appear to consist of only these two elementary particles, newly made in energetic processes. Preliminary results from the presently operating Alpha Magnetic Spectrometer AMS on board the International Space Station show that positrons in the cosmic rays arrive with no directionality. Cosmic ray antiprotons also have a much higher average energy than their normal-matter counterparts protons. There is no evidence of complex antimatter atomic nuclei, such as antihelium nuclei i.

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These are actively being searched for. By not detecting any antihelium at all, the AMS established an upper limit of 1.

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When cosmic rays enter the Earth's atmosphere they collide with atoms and molecules , mainly oxygen and nitrogen. The interaction produces a cascade of lighter particles, a so-called air shower secondary radiation that rains down, including x-rays , muons , protons, alpha particles , pions , electrons , and neutrons. Typical particles produced in such collisions are neutrons and charged mesons such as positive or negative pions and kaons. Some of these subsequently decay into muons and neutrinos , which are able to reach the surface of the Earth. Some high-energy muons even penetrate for some distance into shallow mines, and most neutrinos traverse the Earth without further interaction.

Others decay into photon , subsequently producing electromagnetic cascades. Hence, next to photons electrons and positrons usually dominate in air showers. These particles as well as muons can be easily detected by many types of particle detectors, such as cloud chambers , bubble chambers , water-Cherenkov or scintillation detectors. The observation of a secondary shower of particles in multiple detectors at the same time is an indication that all of the particles came from that event. Cosmic rays impacting other planetary bodies in the Solar System are detected indirectly by observing high-energy gamma ray emissions by gamma-ray telescope.

The flux of incoming cosmic rays at the upper atmosphere is dependent on the solar wind , the Earth's magnetic field , and the energy of the cosmic rays. However, the strength of the solar wind is not constant, and hence it has been observed that cosmic ray flux is correlated with solar activity.

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In addition, the Earth's magnetic field acts to deflect cosmic rays from its surface, giving rise to the observation that the flux is apparently dependent on latitude , longitude , and azimuth angle. The combined effects of all of the factors mentioned contribute to the flux of cosmic rays at Earth's surface. The following table of participial frequencies reach the planet [66] and are inferred from lower energy radiation reaching the ground.

In the past, it was believed that the cosmic ray flux remained fairly constant over time. However, recent research suggests one-and-a-half- to two-fold millennium-timescale changes in the cosmic ray flux in the past forty thousand years. There are two main classes of detection methods.