Editing Cosmic ray (section)

===Secondary cosmic rays===
When cosmic rays enter the [[Earth's atmosphere]], they collide with [[atom]]s and [[molecule]]s, 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]], protons, alpha particles, pions, muons, electrons, neutrinos, and [[neutron]]s.<ref>{{cite book|last=Morison|first=Ian|title=Introduction to Astronomy and Cosmology|year=2008|publisher=John Wiley & Sons|isbn=978-0-470-03333-3|page=198|bibcode=2008iac..book.....M}}</ref> All of the secondary particles produced by the collision continue onward on paths within about one degree of the primary particle's original path.

Typical particles produced in such collisions are neutrons and charged [[meson]]s such as positive or negative pions and [[kaon]]s. 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 photons, 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 chamber]]s, [[bubble chamber]]s, [[High Altitude Water Cherenkov Experiment|water-Cherenkov]], or [[scintillation (physics)|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. These are distinguished from radioactive decay processes by their higher energies above about 10&nbsp;MeV.