Contents 1 Etymology 2 Massive cosmic rays compared to photons 3 Composition 4 Energy 5 History 5.1 Discovery 5.2 Identification 5.3 Energy distribution 6 Sources of cosmic rays 7 Types 7.1 Primary cosmic rays 7.1.1 Primary cosmic ray antimatter 7.2 Secondary cosmic rays 7.3 Cosmic-ray flux 8 Detection methods 9 Effects 9.1 Changes in atmospheric chemistry 9.2 Role in ambient radiation 9.3 Effect on electronics 9.4 Significance to aerospace travel 9.5 Role in lightning 9.6 Postulated role in climate change 10 Research and experiments 10.1 Ground-based 10.2 Satellite 10.3 Balloon-borne 11 See also 12 References 13 Further references 14 External links

Etymology[edit] The term ray is somewhat of a misnomer due to a historical accident, as cosmic rays were at first, and wrongly, thought to be mostly electromagnetic radiation. In common scientific usage,[6] high-energy particles with intrinsic mass are known as "cosmic" rays, while photons, which are quanta of electromagnetic radiation (and so have no intrinsic mass) are known by their common names, such as gamma rays or X-rays, depending on their photon energy.

Massive cosmic rays compared to photons[edit] In current usage, the term cosmic ray almost exclusively refers to massive particles, as opposed to photons which have no rest mass. Massive particles – those that have rest mass – have additional, kinetic, mass-energy when they are moving, due to relativistic effects. Through this process, some particles acquire tremendously high mass-energies. These are significantly higher than the photon energy of even the highest-energy photons detected to date. The energy of the massless photon depends solely on frequency, not speed, as photons always travel at the same speed. At the higher end of the energy spectrum, relativistic kinetic energy is the main source of the mass-energy of cosmic rays. The Oh-My-God particle, the highest-energy fermionic cosmic ray detected to date, had an energy of about 7020300000000000000♠3×1020 eV, while the highest-energy gamma rays to be observed, very-high-energy gamma rays, are photons with energies of up to 6995160217648700000♠1014 eV. Hence, the highest-energy detected fermionic cosmic ray was around 7006300000000000000♠3×106 times more energetic than the highest-energy detected cosmic photons.

Composition[edit] Of primary cosmic rays, which originate outside of Earth's atmosphere, about 99% are the nuclei of well-known atoms (stripped of their electron shells), and about 1% are solitary electrons (similar to beta particles). Of the nuclei, about 90% are simple protons (i.e., hydrogen nuclei); 9% are alpha particles, identical to helium nuclei; and 1% are the nuclei of heavier elements, called HZE ions.[7] A very small fraction are stable particles of antimatter, such as positrons or antiprotons. The precise nature of this remaining fraction is an area of active research. An active search from Earth orbit for anti-alpha particles has failed to detect them.

Energy[edit] Cosmic rays attract great interest practically, due to the damage they inflict on microelectronics and life outside the protection of an atmosphere and magnetic field, and scientifically, because the energies of the most energetic ultra-high-energy cosmic rays (UHECRs) have been observed to approach 3 × 1020 eV,[8] about 40 million times the energy of particles accelerated by the Large Hadron Collider.[9] One can show that such enormous energies might be achieved by means of the centrifugal mechanism of acceleration in active galactic nuclei. At 50 J,[10] the highest-energy ultra-high-energy cosmic rays have energies comparable to the kinetic energy of a 90-kilometre-per-hour (56 mph) baseball. As a result of these discoveries, there has been interest in investigating cosmic rays of even greater energies.[11] Most cosmic rays, however, do not have such extreme energies; the energy distribution of cosmic rays peaks at 0.3 gigaelectronvolts (4.8×10−11 J).[12]

History[edit] After the discovery of radioactivity by Henri Becquerel in 1896, it was generally believed that atmospheric electricity, ionization of the air, was caused only by radiation from radioactive elements in the ground or the radioactive gases or isotopes of radon they produce.[13] Measurements of ionization rates at increasing heights above the ground during the decade from 1900 to 1910 showed a decrease that could be explained as due to absorption of the ionizing radiation by the intervening air.[14] Discovery[edit] In 1909, Theodor Wulf developed an electrometer, a device to measure the rate of ion production inside a hermetically sealed container, and used it to show higher levels of radiation at the top of the Eiffel Tower than at its base. However, his paper published in Physikalische Zeitschrift was not widely accepted. In 1911, Domenico Pacini observed simultaneous variations of the rate of ionization over a lake, over the sea, and at a depth of 3 meters from the surface. Pacini concluded from the decrease of radioactivity underwater that a certain part of the ionization must be due to sources other than the radioactivity of the Earth.[15] Pacini makes a measurement in 1910. In 1912, Victor Hess carried three enhanced-accuracy Wulf electrometers[16] to an altitude of 5300 meters in a free balloon flight. He found the ionization rate increased approximately fourfold over the rate at ground level.[16] Hess ruled out the Sun as the radiation's source by making a balloon ascent during a near-total eclipse. With the moon blocking much of the Sun's visible radiation, Hess still measured rising radiation at rising altitudes.[16] He concluded "The results of my observation are best explained by the assumption that a radiation of very great penetrating power enters our atmosphere from above." In 1913–1914, Werner Kolhörster confirmed Victor Hess' earlier results by measuring the increased ionization rate at an altitude of 9 km. Increase of ionization with altitude as measured by Hess in 1912 (left) and by Kolhörster (right) Hess received the Nobel Prize in Physics in 1936 for his discovery.[17][18] The Hess balloon flight took place on 7 August 1912. By sheer coincidence, exactly 100 years later on 7 August 2012, the Mars Science Laboratory rover used its Radiation Assessment Detector (RAD) instrument to begin measuring the radiation levels on another planet for the first time. On 31 May 2013, NASA scientists reported that a possible manned mission to Mars may involve a greater radiation risk than previously believed, based on the amount of energetic particle radiation detected by the RAD on the Mars Science Laboratory while traveling from the Earth to Mars in 2011–2012.[19][20][21] Hess lands after his balloon flight in 1912. Identification[edit] Bruno Rossi wrote that: In the late 1920s and early 1930s the technique of self-recording electroscopes carried by balloons into the highest layers of the atmosphere or sunk to great depths under water was brought to an unprecedented degree of perfection by the German physicist Erich Regener and his group. To these scientists we owe some of the most accurate measurements ever made of cosmic-ray ionization as a function of altitude and depth.[22] Ernest Rutherford stated in 1931 that "thanks to the fine experiments of Professor Millikan and the even more far-reaching experiments of Professor Regener, we have now got for the first time, a curve of absorption of these radiations in water which we may safely rely upon".[23] In the 1920s, the term cosmic rays was coined by Robert Millikan who made measurements of ionization due to cosmic rays from deep under water to high altitudes and around the globe. Millikan believed that his measurements proved that the primary cosmic rays were gamma rays; i.e., energetic photons. And he proposed a theory that they were produced in interstellar space as by-products of the fusion of hydrogen atoms into the heavier elements, and that secondary electrons were produced in the atmosphere by Compton scattering of gamma rays. But then, sailing from Java to the Netherlands in 1927, Jacob Clay found evidence,[24] later confirmed in many experiments, of a variation of cosmic ray intensity with latitude, which indicated that the primary cosmic rays are deflected by the geomagnetic field and must therefore be charged particles, not photons. In 1929, Bothe and Kolhörster discovered charged cosmic-ray particles that could penetrate 4.1 cm of gold.[25] Charged particles of such high energy could not possibly be produced by photons from Millikan's proposed interstellar fusion process.[citation needed] In 1930, Bruno Rossi predicted a difference between the intensities of cosmic rays arriving from the east and the west that depends upon the charge of the primary particles – the so-called "east-west effect."[26] Three independent experiments[27][28][29] found that the intensity is, in fact, greater from the west, proving that most primaries are positive. During the years from 1930 to 1945, a wide variety of investigations confirmed that the primary cosmic rays are mostly protons, and the secondary radiation produced in the atmosphere is primarily electrons, photons and muons. In 1948, observations with nuclear emulsions carried by balloons to near the top of the atmosphere showed that approximately 10% of the primaries are helium nuclei (alpha particles) and 1% are heavier nuclei of the elements such as carbon, iron, and lead.[30][31] During a test of his equipment for measuring the east-west effect, Rossi observed that the rate of near-simultaneous discharges of two widely separated Geiger counters was larger than the expected accidental rate. In his report on the experiment, Rossi wrote "... it seems that once in a while the recording equipment is struck by very extensive showers of particles, which causes coincidences between the counters, even placed at large distances from one another."[32] In 1937 Pierre Auger, unaware of Rossi's earlier report, detected the same phenomenon and investigated it in some detail. He concluded that high-energy primary cosmic-ray particles interact with air nuclei high in the atmosphere, initiating a cascade of secondary interactions that ultimately yield a shower of electrons, and photons that reach ground level.[33] Soviet physicist Sergey Vernov was the first to use radiosondes to perform cosmic ray readings with an instrument carried to high altitude by a balloon. On 1 April 1935, he took measurements at heights up to 13.6 kilometers using a pair of Geiger counters in an anti-coincidence circuit to avoid counting secondary ray showers.[34][35] Homi J. 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 1937 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.[36][citation needed][37] Energy distribution[edit] 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 1954 by members of the Rossi Cosmic Ray Group at the Massachusetts Institute of Technology.[38] The experiment employed eleven scintillation detectors arranged within a circle 460 meters in diameter on the grounds of the Agassiz Station of the Harvard College Observatory. From that work, and from many other experiments carried out all over the world, the energy spectrum of the primary cosmic rays is now known to extend beyond 1020 eV. 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, led by James Cronin, winner of the 1980 Nobel Prize in Physics from the University of Chicago, and Alan Watson of the University of Leeds. Their aim is to explore the properties and arrival directions of the very highest-energy primary cosmic rays.[39] The results are expected to have important implications for particle physics and cosmology, due to a theoretical Greisen–Zatsepin–Kuzmin limit to the energies of cosmic rays from long distances (about 160 million light years) which occurs above 1020 eV because of interactions with the remnant photons from the Big Bang origin of the universe. High-energy gamma rays (>50 MeV photons) were finally discovered in the primary cosmic radiation by an MIT experiment carried on the OSO-3 satellite in 1967.[40] Components of both galactic and extra-galactic origins were separately identified at intensities much less than 1% of the primary charged particles. Since then, numerous satellite gamma-ray observatories have mapped the gamma-ray sky. 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.

Sources of cosmic rays[edit] Early speculation on the sources of cosmic rays included a 1934 proposal by Baade and Zwicky suggesting cosmic rays originated from supernovae.[41] A 1948 proposal by Horace W. Babcock suggested that magnetic variable stars could be a source of cosmic rays.[42] Subsequently, in 1951, Y. Sekido et al. identified the Crab Nebula as a source of cosmic rays.[43] Since then, a wide variety of potential sources for cosmic rays began to surface, including supernovae, active galactic nuclei, quasars, and gamma-ray bursts.[44] Sources of ionizing radiation in interplanetary space. Later experiments have helped to identify the sources of cosmic rays with greater certainty. In 2009, 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.[45] However, no correlation was found between the incidence of gamma-ray bursts and cosmic rays, causing the authors to set upper limits as low as 3.4 × 10−6 erg·cm−2 on the flux of 1 GeV – 1 TeV cosmic rays from gamma-ray bursts.[46] In 2009, 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.[47] This analysis, however, was disputed in 2011 with data from PAMELA, which revealed that "spectral shapes of [hydrogen and helium nuclei] are different and cannot be described well by a single power law", suggesting a more complex process of cosmic ray formation.[48] In February 2013, though, research analyzing data from Fermi revealed through an observation of neutral pion decay that supernovae were indeed a source of cosmic rays, with each explosion producing roughly 3 × 1042 – 3 × 1043 J of cosmic rays.[3][4] However, supernovae do not produce all cosmic rays, and the proportion of cosmic rays that they do produce is a question which cannot be answered without further study.[49] In 2017, a research paper using data from the International Space Station identified a possible source as dark matter being "a self-annihilating WIMP".[50]

Types[edit] Cosmic rays can be divided into two types, galactic cosmic rays (GCR), high energy particles originating outside the solar system, and solar energetic particles, high energy particles (predominantly protons) emitted by the sun, primarily in solar particle events. However, the term "cosmic ray" is often used to refer to only the GCR flux. Despite the nomenclature galactic, GCRs may originate within or outside the galaxy (as discussed in the source section above). Primary cosmic particle collides with a molecule of atmosphere. Cosmic rays originate as primary cosmic rays, which are those originally produced in various astrophysical processes. Primary cosmic rays are composed primarily of protons and alpha particles (99%), with a small amount of heavier nuclei (~1%) and an extremely minute proportion of positrons and antiprotons.[7] Secondary cosmic rays, caused by a decay of primary cosmic rays as they impact an atmosphere, include neutrons, pions, positrons, and muons. Of these four, the latter three were first detected in cosmic rays. Primary cosmic rays[edit] 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. The mass ratio of helium to hydrogen nuclei, 28%, is similar to the primordial elemental abundance ratio of these elements, 24%.[51] The remaining fraction is made up of the other heavier nuclei that are typical nucleosynthesis end products, primarily lithium, beryllium, and boron. These nuclei appear in cosmic rays in much greater abundance (~1%) than in the solar atmosphere, where they are only about 10−11 as abundant as helium. 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.[52] Primary cosmic ray antimatter[edit] See also: Alpha Magnetic Spectrometer Satellite experiments have found evidence of positrons and a few antiprotons in primary cosmic rays, amounting to less than 1% of the particles in primary cosmic rays. 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-02) on board the International Space Station show that positrons in the cosmic rays arrive with no directionality. In September, 2014, new results with almost twice as much data were presented in a talk at CERN and published in Physical Review Letters.[53][54] A new measurement of positron fraction up to 500 GeV was reported, showing that positron fraction peaks at a maximum of about 16% of total electron+positron events, around an energy of 275±32 GeV. At higher energies, up to 500 GeV, the ratio of positrons to electrons begins to fall again. The absolute flux of positrons also begins to fall before 500 GeV, but peaks at energies far higher than electron energies, which peak about 10 GeV.[55] These results on interpretation have been suggested to be due to positron production in annihilation events of massive dark matter particles.[56] Cosmic ray antiprotons also have a much higher average energy than their normal-matter counterparts (protons). They arrive at Earth with a characteristic energy maximum of 2 GeV, indicating their production in a fundamentally different process from cosmic ray protons, which on average have only one-sixth of the energy.[57] There is no evidence of complex antimatter atomic nuclei, such as antihelium nuclei (i.e., anti-alpha particles), in cosmic rays. These are actively being searched for. A prototype of the AMS-02 designated AMS-01, was flown into space aboard the Space Shuttle Discovery on STS-91 in June 1998. By not detecting any antihelium at all, the AMS-01 established an upper limit of 1.1 × 10−6 for the antihelium to helium flux ratio.[58] The moon in cosmic rays The Moon's cosmic ray shadow, as seen in secondary muons detected 700 m below ground, at the Soudan 2 detector The Moon as seen by the Compton Gamma Ray Observatory, in gamma rays with energies greater than 20 MeV. These are produced by cosmic ray bombardment on its surface.[59] Secondary cosmic rays[edit] 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.[60] All of the produced particles stay within about one degree of the primary particle's path. 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, which are able to reach the surface of the Earth, and even penetrate for some distance into shallow mines. The muons can be easily detected by many types of particle detectors, such as cloud chambers, bubble chambers 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. These are distinguished from radioactive decay processes by their higher energies above  about 10 MeV. Cosmic-ray flux[edit] An overview of the space environment shows the relationship between the solar activity and galactic cosmic rays.[61] 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. At distances of ~94 AU from the Sun, the solar wind undergoes a transition, called the termination shock, from supersonic to subsonic speeds. The region between the termination shock and the heliopause acts as a barrier to cosmic rays, decreasing the flux at lower energies (≤ 1 GeV) by about 90%. 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. 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[62] and are inferred from lower energy radiation reaching the ground[63] Particle energy (eV) Particle rate (m−2s−1) 7009100000000000000♠1×109 (GeV) 7004100000000000000♠1×104 7012100000000000000♠1×1012 (TeV) 1 7016100000000000000♠1×1016 (10 PeV) 6993100000000000000♠1×10−7 (a few times a year) 7020100000000000000♠1×1020 (100 EeV) 6985100000000000000♠1×10−15 (once a century) In the past, it was believed that the cosmic ray flux remained fairly constant over time. However, recent research suggests 1.5 to 2-fold millennium-timescale changes in the cosmic ray flux in the past forty thousand years.[64] The magnitude of the energy of cosmic ray flux in interstellar space is very comparable to that of other deep space energies: cosmic ray energy density averages about one electron-volt per cubic centimeter of interstellar space, or ~1 eV/cm3, which is comparable to the energy density of visible starlight at 0.3 eV/cm3, the galactic magnetic field energy density (assumed 3 microgauss) which is ~0.25 eV/cm3, or the cosmic microwave background (CMB) radiation energy density at ~ 0.25 eV/cm3.[65]

Detection methods[edit] The VERITAS array of air Cherenkov telescopes. There are several ground-based methods of detecting cosmic rays currently in use. The first detection method is called the air Cherenkov telescope, designed to detect low-energy (<200 GeV) cosmic rays by means of analyzing their Cherenkov radiation, which for cosmic rays are gamma rays emitted as they travel faster than the speed of light in their medium, the atmosphere.[66] While these telescopes are extremely good at distinguishing between background radiation and that of cosmic-ray origin, they can only function well on clear nights without the Moon shining, and have very small fields of view and are only active for a few percent of the time. Another Cherenkov telescope uses water as a medium through which particles pass and produce Cherenkov radiation to make them detectable.[67] Comparison of radiation doses, including the amount detected on the trip from Earth to Mars by the RAD on the MSL (2011 – 2013).[19][20][21] Extensive air shower (EAS) arrays, a second detection method, measure the charged particles which pass through them. EAS arrays measure much higher-energy cosmic rays than air Cherenkov telescopes, and can observe a broad area of the sky and can be active about 90% of the time. However, they are less able to segregate background effects from cosmic rays than can air Cherenkov telescopes. EAS arrays employ plastic scintillators in order to detect particles. Another method was developed by Robert Fleischer, P. Buford Price, and Robert M. Walker for use in high-altitude balloons.[68] In this method, sheets of clear plastic, like 0.25 mm Lexan polycarbonate, are stacked together and exposed directly to cosmic rays in space or high altitude. The nuclear charge causes chemical bond breaking or ionization in the plastic. At the top of the plastic stack the ionization is less, due to the high cosmic ray speed. As the cosmic ray speed decreases due to deceleration in the stack, the ionization increases along the path. The resulting plastic sheets are "etched" or slowly dissolved in warm caustic sodium hydroxide solution, that removes the surface material at a slow, known rate. The caustic sodium hydroxide dissolves the plastic at a faster rate along the path of the ionized plastic. The net result is a conical etch pit in the plastic. The etch pits are measured under a high-power microscope (typically 1600× oil-immersion), and the etch rate is plotted as a function of the depth in the stacked plastic. This technique yields a unique curve for each atomic nucleus from 1 to 92, allowing identification of both the charge and energy of the cosmic ray that traverses the plastic stack. The more extensive the ionization along the path, the higher the charge. In addition to its uses for cosmic-ray detection, the technique is also used to detect nuclei created as products of nuclear fission. A fourth method involves the use of cloud chambers[69] to detect the secondary muons created when a pion decays. Cloud chambers in particular can be built from widely available materials and can be constructed even in a high-school laboratory. A fifth method, involving bubble chambers, can be used to detect cosmic ray particles.[70] Another method detects the light from nitrogen fluorescence caused by the excitation of nitrogen in the atmosphere by the shower of particles moving through the atmosphere. This method allows for accurate detection of the direction from which the cosmic ray came.[71] Finally, the CMOS devices in pervasive smartphone cameras have been proposed as a practical distributed network to detect air showers from ultra-high energy cosmic rays (UHECRs) which is at least comparable with that of conventional cosmic ray detectors.[72] The app, which is currently in beta and accepting applications, is CRAYFIS (Cosmic RAYs Found In Smartphones).[73][74]

Effects[edit] Changes in atmospheric chemistry[edit] Cosmic rays ionize the nitrogen and oxygen molecules in the atmosphere, which leads to a number of chemical reactions. One of the reactions results in ozone depletion. Cosmic rays are also responsible for the continuous production of a number of unstable isotopes in the Earth's atmosphere, such as carbon-14, via the reaction: n + 14N → p + 14C Cosmic rays kept the level of carbon-14[75] in the atmosphere roughly constant (70 tons) for at least the past 100,000 years,[citation needed] until the beginning of above-ground nuclear weapons testing in the early 1950s. This is an important fact used in radiocarbon dating used in archaeology. Reaction products of primary cosmic rays, radioisotope half-lifetime, and production reaction.[76] Tritium (12.3 years): 14N(n, 3H)12C (spallation) Beryllium-7 (53.3 days) Beryllium-10 (1.39 million years): 14N(n,p α)10Be (spallation) Carbon-14 (5730 years): 14N(n, p)14C (neutron activation) Sodium-22 (2.6 years) Sodium-24 (15 hours) Magnesium-28 (20.9 hours) Silicon-31 (2.6 hours) Silicon-32 (101 years) Phosphorus-32 (14.3 days) Sulfur-35 (87.5 days) Sulfur-38 (2.84 hours) Chlorine-34 m (32 minutes) Chlorine-36 (300,000 years) Chlorine-38 (37.2 minutes) Chlorine-39 (56 minutes) Argon-39 (269 years) Krypton-85 (10.7 years) Role in ambient radiation[edit] Cosmic rays constitute a fraction of the annual radiation exposure of human beings on the Earth, averaging 0.39 mSv out of a total of 3 mSv per year (13% of total background) for the Earth's population. However, the background radiation from cosmic rays increases with altitude, from 0.3 mSv per year for sea-level areas to 1.0 mSv per year for higher-altitude cities, raising cosmic radiation exposure to a quarter of total background radiation exposure for populations of said cities. Airline crews flying long distance high-altitude routes can be exposed to 2.2 mSv of extra radiation each year due to cosmic rays, nearly doubling their total exposure to ionizing radiation. Average annual radiation exposure (millisieverts) Radiation UNSCEAR[77][78] Princeton[79] Wa State[80] MEXT[81] Remark Type Source World average Typical range USA USA Japan Natural Air 1.26 0.2–10.0a 2.29 2.00 0.40 Primarily from radon, (a)depends on indoor accumulation of radon gas. Internal 0.29 0.2–1.0b 0.16 0.40 0.40 Mainly from radioisotopes in food (40K, 14C, etc.) (b)depends on diet. Terrestrial 0.48 0.3–1.0c 0.19 0.29 0.40 (c)Depends on soil composition and building material of structures. Cosmic 0.39 0.3–1.0d 0.31 0.26 0.30 (d)Generally increases with elevation. Subtotal 2.40 1.0–13.0 2.95 2.95 1.50 Artificial Medical 0.60 0.03–2.0 3.00 0.53 2.30 Fallout 0.007 0 – 1+ - - 0.01 Peaked in 1963 with a spike in 1986; still high near nuclear test and accident sites. For the United States, fallout is incorporated into other categories. Others 0.0052 0–20 0.25 0.13 0.001 Average annual occupational exposure is 0.7 mSv; mining workers have higher exposure. Populations near nuclear plants have an additional ~0.02 mSv of exposure annually. Subtotal 0.6 0 to tens 3.25 0.66 2.311 Total 3.00 0 to tens 6.20 3.61 3.81 Figures are for the time before the Fukushima Daiichi nuclear disaster. Human-made values by UNSCEAR are from the Japanese National Institute of Radiological Sciences, which summarized the UNSCEAR data. Effect on electronics[edit] Cosmic rays have sufficient energy to alter the states of circuit components in electronic integrated circuits, causing transient errors to occur (such as corrupted data in electronic memory devices or incorrect performance of CPUs) often referred to as "soft errors." This has been a problem in electronics at extremely high-altitude, such as in satellites, but with transistors becoming smaller and smaller, this is becoming an increasing concern in ground-level electronics as well.[82] Studies by IBM in the 1990s suggest that computers typically experience about one cosmic-ray-induced error per 256 megabytes of RAM per month.[83] To alleviate this problem, the Intel Corporation has proposed a cosmic ray detector that could be integrated into future high-density microprocessors, allowing the processor to repeat the last command following a cosmic-ray event.[84] Cosmic rays were suspected as a possible cause of an in-flight incident in 2008 where an Airbus A330 airliner of Qantas twice plunged hundreds of feet after an unexplained malfunction in its flight control system. Many passengers and crew members were injured, some seriously. After this incident, the accident investigators for NW Australia gave the ruling that, "there was a design flaw in the air data inertial reference unit and a limitation of the aircraft's computer software. The serious Qantas A330 upset was caused by a long dormant computer flaw triggered by chance."[85] This has prompted a software upgrade to all A330 and A340 airliners, worldwide, so that any data spikes in this system are filtered out electronically.[86] See also: radiation hardening See also: ECC memory Significance to aerospace travel[edit] Main article: Health threat from cosmic rays Galactic cosmic rays are one of the most important barriers standing in the way of plans for interplanetary travel by crewed spacecraft. Cosmic rays also pose a threat to electronics placed aboard outgoing probes. In 2010, a malfunction aboard the Voyager 2 space probe was credited to a single flipped bit, probably caused by a cosmic ray. Strategies such as physical or magnetic shielding for spacecraft have been considered in order to minimize the damage to electronics and human beings caused by cosmic rays.[87][88] Flying 12 kilometres (39,000 ft) high, passengers and crews of jet airliners are exposed to at least 10 times the cosmic ray dose that people at sea level receive. Aircraft flying polar routes near the geomagnetic poles are at particular risk.[89][90][91][92] Role in lightning[edit] Cosmic rays have been implicated in the triggering of electrical breakdown in lightning. It has been proposed that essentially all lightning is triggered through a relativistic process, "runaway breakdown", seeded by cosmic ray secondaries. Subsequent development of the lightning discharge then occurs through "conventional breakdown" mechanisms.[93] Postulated role in climate change[edit] A role of cosmic rays directly or via solar-induced modulations in climate change was suggested by Edward P. Ney in 1959[94] and by Robert E. Dickinson in 1975.[95] It has been postulated that cosmic rays may have been responsible for major climatic change and mass-extinction in the past. According to Adrian Mellott and Mikhail Medvedev, 62 million year cycles in biological marine populations correlate with the motion of the earth relative to the galactic plane and increases in exposure to cosmic rays.[96] The researchers suggest that this and gamma ray bombardments deriving from local supernovae could have affected cancer and mutation rates, and might be linked to decisive alterations in the Earth's climate, and to the mass-extinctions of the Ordovician.[97][98] Dutch physicist Henrik Svensmark has argued that because solar variation modulates the cosmic ray flux on Earth, they would consequently affect the rate of cloud formation and hence be an indirect cause of global warming.[99][100] Svensmark is one of several scientists outspokenly opposed to the mainstream scientific assessment of global warming, leading to concerns that the proposition that cosmic rays are connected to global warming could be ideologically biased rather than scientifically based.[101] Other scientists have vigorously criticized Svensmark for sloppy and inconsistent work: one example is adjustment of cloud data that understates error in lower cloud data, but not in high cloud data;[102] another example is "incorrect handling of the physical data" resulting in graphs that do not show the correlations they claim to show.[103] Despite Svensmark's assertions, galactic cosmic rays have shown no statistically significant influence on changes in cloud cover,[104] and demonstrated to have no causal relationship to changes in global temperature.[105]

Research and experiments[edit] See also: Cosmic-ray observatory There are a number of cosmic-ray research initiatives, listed below. Ground-based[edit] Akeno Giant Air Shower Array CHICOS CRIPT High Energy Stereoscopic System High Resolution Fly's Eye Cosmic Ray Detector MAGIC MARIACHI Pierre Auger Observatory Telescope Array Project Tunka experiment VERITAS Washington Large Area Time Coincidence Array CLOUD Spaceship Earth Milagro NMDB KASCADE GAMMA GRAPES-3 HEGRA Chicago Air Shower Array IceCube HAWC Satellite[edit] PAMELA Alpha Magnetic Spectrometer ACE (Advanced Composition Explorer) Voyager 1 and Voyager 2 Cassini–Huygens HEAO 1, HEAO 2, HEAO 3 Fermi Gamma-ray Space Telescope Solar and Heliospheric Observatory Interstellar Boundary Explorer Langton Ultimate Cosmic-Ray Intensity Detector Balloon-borne[edit] BESS Advanced Thin Ionization Calorimeter TRACER (cosmic ray detector) TIGER Cosmic Ray Energetics and Mass (CREAM) PERDaix HEAT (High Energy Antimatter Telescope)

See also[edit] Central nervous system effects from radiation exposure during spaceflight Cosmic ray visual phenomena Environmental radioactivity Extragalactic cosmic ray Forbush decrease Gilbert Jerome Perlow Health threat from cosmic rays Oh-My-God particle Solar energetic particle Track Imaging Cherenkov Experiment Ultra-high-energy cosmic ray (UHECR)

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Further references[edit] R.G. Harrison and D.B. Stephenson, Detection of a galactic cosmic ray influence on clouds, Geophysical Research Abstracts, Vol. 8, 07661, 2006 SRef-ID: 1607-7962/gra/EGU06-A-07661 Anderson, C. D.; Neddermeyer, S. H. (1936). "Cloud Chamber Observations of Cosmic Rays at 4300 Meters Elevation and Near Sea-Level". Phys. Rev. 50: 263–271. Bibcode:1936PhRv...50..263A. doi:10.1103/physrev.50.263.  Boezio, M.; et al. (2000). "Measurement of the flux of atmospheric muons with the CAPRICE94 apparatus". Phys. Rev. D. 62: 032007. arXiv:hep-ex/0004014 . Bibcode:2000PhRvD..62c2007B. doi:10.1103/physrevd.62.032007.  R. Clay and B. Dawson, Cosmic Bullets, Allen & Unwin, 1997. ISBN 1-86448-204-4 T. K. Gaisser, Cosmic Rays and Particle Physics, Cambridge University Press, 1990. ISBN 0-521-32667-2 P. K. F. Grieder, Cosmic Rays at Earth: Researcher's Reference Manual and Data Book, Elsevier, 2001. ISBN 0-444-50710-8 A. M. Hillas, Cosmic Rays, Pergamon Press, Oxford, 1972 ISBN 0-08-016724-1 Kremer, J.; et al. (1999). "Measurement of Ground-Level Muons at Two Geomagnetic Locations". Phys. Rev. Lett. 83: 4241–4244. Bibcode:1999PhRvL..83.4241K. doi:10.1103/physrevlett.83.4241.  Neddermeyer, S. H.; Anderson, C. D. (1937). "Note on the Nature of Cosmic-Ray Particles". Phys. Rev. 51: 884–886. Bibcode:1937PhRv...51..884N. doi:10.1103/physrev.51.884.  M. D. Ngobeni and M. S. Potgieter, Cosmic ray anisotropies in the outer heliosphere, Advances in Space Research, 2007. M. D. Ngobeni, Aspects of the modulation of cosmic rays in the outer heliosphere, M.Sc Dissertation, Northwest University (Potchefstroom campus) South Africa 2006. D. Perkins, Particle Astrophysics, Oxford University Press, 2003. ISBN 0-19-850951-0 C. E. Rolfs and S. R. William, Cauldrons in the Cosmos, The University of Chicago Press, 1988. ISBN 0-226-72456-5 B. B. Rossi, Cosmic Rays, McGraw-Hill, New York, 1964. Martin Walt, Introduction to Geomagnetically Trapped Radiation, 1994. ISBN 0-521-43143-3 Taylor, M.; Molla, M. (2010). "Towards a unified source-propagation model of cosmic rays". Publ. Astron. Soc. Pac. 424: 98.  Ziegler, J. F. (1981). "The Background In Detectors Caused By Sea Level Cosmic Rays". Nuclear Instruments and Methods. 191: 419–424. Bibcode:1981NIMPR.191..419Z. doi:10.1016/0029-554x(81)91039-9.  TRACER Long Duration Balloon Project: the largest cosmic ray detector launched on balloons. Carlson, Per; De Angelis, Alessandro (2011). "Nationalism and internationalism in science: the case of the discovery of cosmic rays". European Physical Journal H. 35 (4): 309–329. arXiv:1012.5068 . Bibcode:2010EPJH...35..309C. doi:10.1140/epjh/e2011-10033-6. 

External links[edit] Wikimedia Commons has media related to Cosmic rays. Aspera European network portal Animation about cosmic rays on Helmholtz Alliance for Astroparticle Physics Particle Data Group review of Cosmic Rays by C. Amsler et al., Physics Letters B667, 1 (2008). Introduction to Cosmic Ray Showers by Konrad Bernlöhr. BBC news, Cosmic rays find uranium, 2003. BBC news, Rays to nab nuclear smugglers, 2005. BBC news, Physicists probe ancient pyramid (using cosmic rays), 2004. Shielding Space Travelers by Eugene Parker. Anomalous cosmic ray hydrogen spectra from Voyager 1 and 2 Anomalous Cosmic Rays (From NASA's Cosmicopia) Review of Cosmic Rays "Who's Afraid of a Solar Flare? Solar activity can be surprisingly good for astronauts." 7 October 2005, at Science@NASA video of Muon detector in use at Smithsonian Air and Space Museum Dr. Lothar Frey "Cosmic rays and electronic devices" (YouTube Video) SpaceUp Stuttgart 2012 ARMAS, Real-time cosmic-ray radiation measurements at aviation altitudes. Padilla, Antonio (Tony). "Where do Cosmic Rays come from?". Sixty Symbols. 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life sciences Radioactive contamination Radiobiology Biological dose units and quantities Wireless electronic devices and health Radiation Heat-transfer Related articles Half-life Nuclear physics Radioactive source Radiation hardening List of civilian radiation accidents 1996 Costa Rica accident 1987 Goiânia accident 1984 Moroccan accident 1990 Zaragoza accident See also: the categories Radiation effects, Radioactivity, Radiobiology, and Radiation protection. v t e Molecules detected in outer space Molecules Diatomic Aluminium monochloride Aluminium monofluoride Aluminium monoxide Argonium Carbon monophosphide Carbon monosulfide Carbon monoxide Carborundum Cyanogen radical Diatomic carbon Fluoromethylidynium Hydrogen chloride Hydrogen fluoride Hydrogen (molecular) Hydroxyl radical Iron(II) oxide Magnesium monohydride cation Methylidyne radical Nitric oxide Nitrogen (molecular) Nitrogen monohydride Nitrogen sulfide Oxygen (molecular) Phosphorus monoxide Phosphorus mononitride Potassium chloride Silicon carbide Silicon mononitride Silicon monoxide Silicon monosulfide Sodium chloride Sodium iodide Sulfur monohydride Sulfur monoxide Titanium oxide Triatomic Aluminium hydroxide Aluminium isocyanide Amino radical Carbon dioxide Carbonyl sulfide CCP radical Chloronium Diazenylium Dicarbon monoxide Disilicon carbide Ethynyl radical Formyl radical Hydrogen cyanide (HCN) Hydrogen isocyanide (HNC) Hydrogen sulfide Hydroperoxyl Iron cyanide Isoformyl Magnesium cyanide Magnesium isocyanide Methylene radical N2H+ Nitrous oxide Nitroxyl Ozone Phosphaethyne Potassium cyanide Protonated molecular hydrogen Sodium cyanide Sodium hydroxide Silicon carbonitride c-Silicon dicarbide Silicon naphthalocyanine Sulfur dioxide Thioformyl Thioxoethenylidene Titanium dioxide Tricarbon Water Four atoms Acetylene Ammonia Cyanic acid Cyanoethynyl Cyclopropynylidyne Formaldehyde Fulminic acid HCCN Hydrogen peroxide Hydromagnesium isocyanide Isocyanic acid Isothiocyanic acid Ketenyl Methylene amidogen Methyl radical Propynylidyne Protonated carbon dioxide Protonated hydrogen cyanide Silicon tricarbide Thioformaldehyde Tricarbon monoxide Tricarbon sulfide Thiocyanic acid Five atoms Ammonium ion Butadiynyl Carbodiimide Cyanamide Cyanoacetylene Cyanoformaldehyde Cyanomethyl Cyclopropenylidene Formic acid Isocyanoacetylene Ketene Methane Methoxy radical Methylenimine Propadienylidene Protonated formaldehyde Protonated formaldehyde Silane Silicon-carbide cluster Six atoms Acetonitrile Cyanobutadiynyl radical E-Cyanomethanimine Cyclopropenone Diacetylene Ethylene Formamide HC4N Ketenimine Methanethiol Methanol Methyl isocyanide Pentynylidyne Propynal Protonated cyanoacetylene Seven atoms Acetaldehyde Acrylonitrile Vinyl cyanide Cyanodiacetylene Ethylene oxide Hexatriynyl radical Methylacetylene Methylamine Methyl isocyanate Vinyl alcohol Eight atoms Acetic acid Aminoacetonitrile Cyanoallene Ethanimine Glycolaldehyde Heptatrienyl radical Hexapentaenylidene Methylcyanoacetylene Methyl formate Propenal Nine atoms Acetamide Cyanohexatriyne Cyanotriacetylene Dimethyl ether Ethanol Methyldiacetylene Octatetraynyl radical Propene Propionitrile Ten atoms or more Acetone Benzene Benzonitrile Buckminsterfullerene (C60 fullerene, buckyball) C70 fullerene Cyanodecapentayne Cyanopentaacetylene Cyanotetra-acetylene Ethylene glycol Ethyl formate Methyl acetate Methyl-cyano-diacetylene Methyltriacetylene Propanal n-Propyl cyanide Pyrimidine Deuterated molecules Ammonia Ammonium ion Formaldehyde Formyl radical Heavy water Hydrogen cyanide Hydrogen deuteride Hydrogen isocyanide Methylacetylene N2D+ Trihydrogen cation Unconfirmed Anthracene Dihydroxyacetone Ethyl methyl ether Glycine Graphene H2NCO+ Linear C5 Naphthalene cation Phosphine Pyrene Silylidine Related Abiogenesis Astrobiology Astrochemistry Atomic and molecular astrophysics Chemical formula Circumstellar envelope Cosmic dust Cosmic ray Cosmochemistry Diffuse interstellar band Earliest known life forms 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NumberSpecial:BookSources/0-226-72456-5International Standard Book NumberSpecial:BookSources/0-521-43143-3BibcodeDigital Object IdentifierEuropean Physical Journal HArXivBibcodeDigital Object IdentifierSpaceUpBrady HaranUniversity Of NottinghamTemplate:RadiationTemplate Talk:RadiationRadiationNon-ionizing RadiationAcoustic Radiation ForceInfraredLightStarlightSunlightMicrowaveRadio WaveUltravioletIonizing RadiationRadioactive DecayCluster DecayBackground RadiationAlpha ParticleBeta ParticleGamma RayNeutron RadiationNuclear FissionNuclear FusionNuclear ReactorNuclear WeaponParticle AcceleratorRadionuclideX-rayEarth's Radiation BalanceElectromagnetic RadiationThermal RadiationBlack Body RadiationParticle RadiationGravitational RadiationCosmic Background RadiationCherenkov RadiationAskaryan RadiationBremsstrahlungUnruh RadiationDark RadiationAcute Radiation SyndromeHealth PhysicsDosimetryElectromagnetic Radiation And HealthLaser SafetyLasers And Aviation SafetyMedical RadiographyMobile 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MonohydrideMononitrogen MonosulfideOxygenPhosphorus MononitridePotassium ChlorideSilicon CarbideSilicon NitrideSulfanylSilicon MonosulfideSodium ChlorideSodium IodideSulfanylSulfur MonoxideTitanium OxideNitrous OxideEthanolBuckminsterfullereneTriatomic MoleculeAluminium HydroxideAmino RadicalCarbon DioxideCarbonyl SulfideHalonium IonDiazenyliumDicarbon MonoxideEthynyl RadicalHydrogen CyanideHydrogen IsocyanideHydrogen SulfideHydroperoxylMethylene (compound)DiazenyliumNitrous OxideNitroxylOzoneMethylidynephosphanePotassium CyanideTrihydrogen CationSodium CyanideSodium HydroxideSulfur DioxideThioxoethenylideneTitanium DioxideTricarbonWaterList Of Interstellar And Circumstellar MoleculesAcetyleneAmmoniaIsocyanic AcidPolyyneFormaldehydeFulminic AcidHydrogen PeroxideIsocyanic AcidThiocyanic AcidMethyl RadicalPropynylidyneProtonateCarbon DioxideProtonateHydrogen Cyanide1,3,5-TrithianeTricarbon MonoxideTricarbon SulfideThiocyanic AcidList Of Interstellar And Circumstellar MoleculesAmmoniumPolyyneCarbodiimideCyanamideCyanoacetyleneCyanomethylCyclopropenylideneFormic AcidKeteneMethaneMethoxyProtonateFormaldehydeSilaneGrapheneList Of Interstellar And Circumstellar MoleculesAcetonitrileCyclopropenoneDiacetyleneEthyleneFormamideKetenimineMethanethiolMethanolMethyl IsocyanidePolyynePropynalProtonateCyanoacetyleneList Of Interstellar And Circumstellar MoleculesAcetaldehydeAcrylonitrileVinyl CyanideCyanopolyyneEthylene OxideHexatriynyl RadicalPropyneMethylamineMethyl IsocyanateVinyl AlcoholList Of Interstellar And Circumstellar MoleculesAcetic AcidAminoacetonitrileEthanimineGlycolaldehydePolyynePolyyneMethyl FormateAcroleinList Of Interstellar And Circumstellar MoleculesAcetamidePolyynePolyyneDimethyl EtherEthanolPolyyneOctatetraynyl RadicalPropenePropionitrileList Of Interstellar And Circumstellar MoleculesAcetoneBenzeneBenzonitrileBuckminsterfullereneC70 FullereneCyanopolyyneCyanopolyyneCyanopolyyneEthylene GlycolEthyl FormateMethyl 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