The energy spectrum for cosmic rays
The
Moon's cosmic ray shadow, as seen in secondary muons detected 700m below ground, at the Soudan 2 detector
'Cosmic rays' are energetic particles originating from space that impinge on
Earth's atmosphere. Almost 90% of all the incoming cosmic ray particles are
protons, about 9% are
helium nuclei (
alpha particles) and about 1% are
electrons. Note that the term "ray" is a misnomer, as cosmic ray particles arrive individually, not in the form of a ray or beam of particles. See ''
wave-particle duality''.
The
kinetic energies of cosmic ray particles span over fourteen orders of magnitude, with the
flux of cosmic rays on Earth's surface falling approximately as the inverse-cube of the energy. The wide variety of particle energies reflects the wide variety of sources. Cosmic rays originate from energetic processes on the
Sun all the way to the farthest reaches of the visible
universe. Cosmic rays can have energies of over 10
20 eV, far higher than the 10
12 to 10
13 eV that man-made particle accelerators can produce. (The article on
Ultra-high-energy cosmic rays describes the detection of a single particle with an energy of about 50 J, the same as a well-hit tennis ball at 42 m/s.) There has been interest in investigating cosmic rays of even greater energies.
[1]
Cosmic ray sources
Most cosmic rays originate from extrasolar sources within our own galaxy such as rotating
neutron stars,
supernovae, and
black holes. However, the fact that some cosmic rays have extremely high energies provides evidence that at least some must be of extra-galactic origin (e.g.
radio galaxies and
quasars); the local galactic magnetic field would not be able to contain particles with such a high energy. The origin of cosmic rays with energies up to 10
14 eV can be accounted for in terms of shock-wave acceleration in supernova shells. The origin of cosmic rays with energy greater than 10
14 eV remains unknown; however, a large collaborative experiment at the
Pierre Auger Observatory is underway to try to answer this question.
Observations have shown that cosmic rays with an energy above 10 GeV (10 x 10
9 eV) approach the Earth’s surface isotropically (equally from all directions); it has been hypothesised that this is not due to an even distribution of cosmic ray sources, but instead is due to galactic magnetic fields causing cosmic rays to travel in spiral paths. This limits cosmic ray’s usefulness in positional
astronomy as they carry no information of their direction of origin. At energies below 10 GeV there is a directional dependence, due to the interaction of the charged component of the cosmic rays with the
Earth's magnetic field.
Solar cosmic rays
Solar cosmic rays are cosmic rays that originate from the
Sun, with relatively low energy (10-100 keV or 1.6 - 16 fJ per particle). The average composition is similar to that of the Sun itself.
The name solar cosmic ray itself is a misnomer because the term cosmic implies that the rays are from the cosmos and not the solar system, but it has stuck. The misnomer arose because there is continuity in the energy spectra, i.e., the flux of particles as a function of their energy, because the low-energy solar cosmic rays fade more or less smoothly into the galactic ones as one looks at increasingly higher energies. Until the mid-1960s the energy distributions were generally averaged over long time intervals, which also obscured the difference. Later, it was found that the solar cosmic rays vary widely in their intensity and spectrum, increasing in strength after some solar events such as solar flares. Further, an increase in the intensity of solar cosmic rays is followed by a decrease in all other cosmic rays, called the
Forbush decrease after their discoverer, the physicist Scott Forbush. These decreases are due to the solar wind with its entrained magnetic field sweeping some of the galactic cosmic rays outwards, away from the Sun and Earth. The overall or average rate of Forbush decreases tends to follow the 11-year sunspot cycle, but individual events are tied to events on the Sun, as explained above.
There are further differences between cosmic rays of solar and galactic origin, mainly in that the galactic cosmic rays show an enhancement of heavy elements such as
calcium,
iron and
gallium, as well as of cosmically rare light elements such as
lithium and
beryllium. The latter result from the
cosmic ray spallation (fragmentation) of heavy nuclei due to collisions in transit from the distant sources to the solar system.
Galactic cosmic rays
See ''
Galactic cosmic ray''.
Extragalactic cosmic rays
See ''
Extragalactic cosmic ray''.
Ultra-high-energy cosmic rays
See ''
Ultra-high-energy cosmic ray''.
Anomalous cosmic rays
Anomalous cosmic rays (ACRs) are cosmic rays with unexpectedly low energies. They are thought to be created near the edge of our solar system, in the
heliosheath, the border region between the
heliosphere and the
interstellar medium. When electrically neutral atoms are able to enter the heliosheath (being unaffected by its magnetic fields) subsequently become ionized, they are thought to be accelerated into low-energy cosmic rays by the
solar wind's
termination shock which marks the inner edge of the heliosheath. It is also possible that high energy
galactic cosmic rays which hit the
shock front of the solar wind near the
heliopause might be decelerated, resulting in their transformation into lower-energy anomalous cosmic rays.
The ''
Voyager 1'' space probe crossed the termination shock on
December 16,
2004, according to papers published in the journal ''Science''.
[2] Readings showed particle acceleration, but not of the kind that generates ACRs. It is unclear at this stage (
September 2005) if this is typical of the termination shock (requiring a major rethink of the origin of ACRs), or a localised feature of that part of the termination shock that ''Voyager 1'' passed through. ''
Voyager 2'' is expected to cross the termination shock during or after
2008, which will provide more data.
Composition
Cosmic rays may broadly be divided into two categories, primary and secondary.
The cosmic rays that arise in extrasolar astrophysical sources are primary cosmic rays; these primary cosmic rays can interact with
interstellar matter to create secondary cosmic rays. The sun also emits low energy cosmic rays associated with
solar flares. The exact composition of primary cosmic rays, outside the
Earth’s atmosphere, is dependent on which part of the
energy spectrum is observed. However, in general, almost 90% of all the incoming cosmic rays are
protons, about 9% are
helium nuclei (
alpha particles) and about 1% are
electrons. The remaining fraction is made up of the other heavier nuclei which are abundant end products of star’s nuclear synthesis. Secondary cosmic rays consist of the other nuclei which are not abundant nuclear synthesis end products, or products of the
big bang, primarily
lithium,
beryllium and
boron. These light nuclei appear in cosmic rays in much greater abundance (about 1:100 particles) than in solar atmospheres, where their abundance is about 10
-7 that of
helium.
This abundance difference is a result of the way secondary cosmic rays are formed. When the heavy nuclei components of primary cosmic rays, namely the carbon and oxygen nuclei, collide with interstellar matter, they break up into lighter nuclei (in a process termed
cosmic ray spallation), into lithium, beryllium and boron. It is found that the energy spectra of Li, Be and B falls off somewhat steeper than that of carbon or oxygen, indicating that less
cosmic ray spallation occurs for the higher energy nuclei presumably due to their escape from the
galactic magnetic field. Spallation is also responsible for the abundances of Sc, Ti, V and Mn elements in cosmic rays, which are produced by collisions of Fe and Ni nuclei with
interstellar matter; see
Environmental radioactivity#Naturals.
In the past, it was believed that the cosmic ray
flux has remained fairly constant over time. Recent research has, however, produced evidence for 1.5 to 2-fold millennium-timescale changes in the cosmic ray flux in the past forty thousand years.
[3]
Modulation
The
flux (flow rate) of cosmic rays incident on the Earth’s upper atmosphere is modulated (varied) by two processes; the sun’s
solar wind and the
Earth's magnetic field.
Solar wind is expanding magnetized
plasma generated by the sun, which has the effect of decelerating the incoming particles as well as partially excluding some of the particles with energies below about 1 GeV. The amount of
solar wind is not constant due to changes in solar activity over its regular eleven-year cycle. Hence the level of modulation varies in autocorrelation with solar activity. Also the
Earth's magnetic field deflects some of the cosmic rays, which is confirmed by the fact that the intensity of cosmic radiation is dependent on
latitude,
longitude and
azimuth. The cosmic flux varies from eastern and western directions due to the
polarity of the Earth’s geomagnetic field and the positive charge dominance in primary cosmic rays; this is termed the
east-west effect. The cosmic ray intensity at the equator is lower than at the poles as the geomagnetic cutoff value is greatest at the equator. This can be understood by the fact that charged particle tend to move in the direction of field lines and not across them. This is the reason the
Aurorae occur at the poles, since the field lines curve down towards the Earth’s surface there. Finally, the
longitude dependence arises from the fact that the geomagnetic
dipole axis is not parallel to the Earth’s rotation axis.
This modulation which describes the change in the interstellar intensities of cosmic rays as they propagate in the heliosphere is highly energy and spatial dependent, and it is described by the Parker's Transport Equation in the heliosphere. At large radial distances, far from the Sun ~ 94 AU, there exists the region where the solar wind undergoes a transition from supersonic to subsonic speeds called the solar wind termination shock. The region between the termination shock and the heliospause (the boundary marking the end of the heliosphere) is called the heliosheath. This region acts as a barrier to cosmic rays and it decreases their intensities at lower energies by about 90% indicating that it is not only the Earth's magnetic field that protect us from cosmic ray bombardment. For more on this topic and how the barrier effects occur the agile reader is referred to Mabedle Donald Ngobeni and Marius Potgieter (2007), and Mabedle Donald Ngobeni (2006).
From modelling point of view, there is a challenge in determining the Local Interstellar spectra (LIS) due to large adiabatic energy changes these particles experience owing to the diverging solar wind in the heliosphere. However, significant progress has been made in the field of cosmic ray studies with the development of an improved state-of-the-art 2D numerical model that includes the simulation of the solar wind termination shock, drifts and the heliosheath coupled with fresh descriptions of the diffusion tensor, see Langner et al. (2004). But challenges also exist because the structure of the solar wind and the turbulent magnetic field in the heliosheath is not well understood indicating the heliosheath as the region unknown beyond. With lack of knowledge of the diffusion coefficient perpendicular to the magnetic field our knowledge of the heliosphere and from the modelling point of view is far from complete. There exist promising theories like ab initio approaches, but the drawback is that such theories produce poor compatibility with observations (Minnie, 2006) indicating their failure in describing the mechanisms influencing the cosmic rays in the heliosphere.
Detection
The nuclei that make up cosmic rays are able to travel from their distant sources to the Earth because of the low density of matter in space. Nuclei interact strongly with other matter, so when the cosmic rays approach Earth they begin to collide with the nuclei of atmospheric gases. These collisions, in a process known as a
shower, result in the production of many
pions and
kaons, unstable
mesons which quickly decay into
muons. Because muons do not interact strongly with the atmosphere and because of the relativistic effect of
time dilation many of these muons are able to reach the surface of the Earth. Muons are
ionizing radiation, and may easily be detected by many types of particle detectors such as
bubble chambers or
scintillation detectors. If several muons are observed by separated detectors at the same instant it is clear that they must have been produced in the same shower event.
Interaction with the Earth's Atmosphere
When cosmic ray particles enter the
Earth’s atmosphere they collide with
molecules, mainly oxygen and nitrogen, to produce a cascade of lighter particles, a so-called
air shower. The general idea is shown in the figure which shows a cosmic ray shower produced by a high energy proton of cosmic ray origin striking an atmospheric molecule.
400 px
This image is a simplified picture of an air shower: in reality, the number of particles created in an air shower event can reach in the billions, depending on the energy of the primary particle. All of the produced particles stay within about one degree of the primary particle's path. Typical particles produced in such collisions are charged
mesons (e.g. positive and negative
pions and
kaons); one common collision is:
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:
Cosmic rays have kept the level of
carbon-14 in the atmosphere roughly constant (70 tons) for at least the past 100,000 years. This an important fact used in
radiocarbon dating which is used in
archaeology.
Research and experiments
There are a number of cosmic ray research initiatives. These include, but are not limited to:
★
CHICOS
★
PAMELA
★
Alpha Magnetic Spectrometer
★
MARIACHI
★
Pierre Auger Observatory
★
Spaceship Earth
History
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 (isotopes of
radon) they produce. 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. Then, in 1912,
Victor Hess carried three
Wulf electrometers (a device to measure the rate of ion production inside a hermetically sealed container) 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. 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 1913-14,
Werner Kolhörster confirmed Victor Hess' results by measuring the increased ionization rate at an altitude of 9 km. Hess received the
Nobel Prize in Physics in 1936 for his discovery of what came to be called "cosmic rays".
For many years it was generally believed that cosmic rays were high-energy
photons (
gamma rays) with some secondary
electrons produced by
Compton scattering of the gamma rays. Then, during the decade from 1927 to 1937 a wide variety of experimental investigations demonstrated that the primary cosmic rays are mostly positively charged particles, and the secondary radiation observed at ground level is composed primarily of a "soft component" of electrons and photons and a "hard component" of penetrating particles,
muons. The muon was initially believed to be the unstable particle predicted by
Hideki Yukawa in 1935 in his theory of the
nuclear force. Experiments proved that the muon decays with a
mean life of 2.2 microseconds into an electron and two
neutrinos, but that it does not
interact strongly with
nuclei, so it could not be the Yukawa particle. The mystery was solved by the discovery in 1947 of the
pion, which is produced directly in high-energy nuclear interactions. It decays into a muon and one neutrino with a mean life of 0.0026 microseconds. The pion→muon→electron decay sequence was observed directly in a microscopic examination of particle tracks in a special kind of photographic plate called a nuclear emulsion that had been exposed to cosmic rays at a high-altitude mountain station. In 1948, observations with nuclear emulsions carried by balloons to near the top of the atmosphere by
Gottlieb and
Van Allen showed that the primary cosmic particles are mostly
protons with some helium nuclei (
alpha particles) and a small fraction heavier nuclei.
In 1934
Bruno Rossi reported an observation of near-simultaneous discharges of two
Geiger counters widely separated in a horizontal plane during a test of equipment he was using in a measurement of the so-called
east-west effect. 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. Unfortunately, he did not have the time to study this phenomenon more closely." In 1937
Pierre Auger, unaware of Rossi's earlier report, detected the same phenomenon and investigated it in some detail. He concluded that extensive
particle showers are generated by high-energy primary cosmic-ray particles that interact with air nuclei high in the atmosphere, initiating a cascade of secondary interactions that ultimately yield a shower of electrons, photons, and muons that reach ground level.
Homi Bhabha derived an expression for the probability of scattering positrons by electrons, a process now known as Bhabha scattering. His classic paper, jointly with W. 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. In 1938 Bhabha concluded that observations of the properties of such particles would lead to the straightforward experimental verification of Albert Einstein's theory of relativity.
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. 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 10
20 eV (past the
GZK cutoff, beyond which very few cosmic rays should be observed). 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. The results are expected to have important implications for particle physics and cosmology.
Three varieties of
neutrino are produced when the unstable particles produced in cosmic ray showers decay. Since neutrinos interact only
weakly with matter most of them simply pass through the Earth and exit the other side. They very occasionally interact, however, and these atmospheric neutrinos have been detected by several deep underground experiments. The
Super-Kamiokande in Japan provided the first convincing evidence for
neutrino oscillation in which one
flavour of neutrino changes into another. The evidence was found in a difference in the ratio of electron neutrinos to muon neutrinos depending on the distance they have traveled through the air and earth.
Effects
Role in Ambient Radiation
Cosmic rays constitute a fraction of the annual radiation exposure of human beings on earth. For example, the average radiation exposure in Australia is 0.3
mSv due to cosmic rays, out of a total of 2.3 mSv.
[1]
Significance to Space Travel
Understanding the effects of cosmic rays on the body will be vital for assessing the risks of
space travel. R.A. Mewaldt estimated humans unshielded in interplanetary space receive annually roughly 400 to 900 mSv (compared to 2.4 mSv on Earth) and that a 30 month Mars mission might expose astronauts to 460 mSv (at Solar Maximum) to 1140 mSv (at Solar Minimum).
[4] These doses approach the 1 to 4 Sv career limits advised by the
National Council on Radiation Protection and Measurements for
Low Earth Orbit activities.
High speed cosmic rays can damage
DNA, increasing the risk of
cancer,
cataracts,
neurological disorders, and non-cancer mortality risks.
[5]
Due to the potential negative effects of astronaut exposure to cosmic rays, solar activity may play a role in future space travel via the
Forbush decrease effect.
Coronal mass ejections (CMEs) can temporarily lower the local cosmic ray levels, and radiation from CMEs is easier to shield against than cosmic rays.
Role in Lightning
Cosmic rays have been implicated in the triggering of electrical breakdown in
lightning. It has been proposed (see Gurevich and Zybin, ''Physics Today'', May 2005, "Runaway Breakdown and the Mysteries of Lightning") 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.
Role in climate change
Whether cosmic rays have any role in climate change is disputed. Different groups have made different arguments for the role of cosmic ray forcing in climate change.
Shaviv et. al. have argued that ''galactic cosmic ray'' (GCR) climate signals on geological time scales are attributable to changing positions of the galactic spiral arms of the Milky Way, and that Cosmic Ray Flux variability is the most dominant climate driver over these time periods.
[6][7]
He also argues that GCR flux variability plays an important role in climate variability over shorter time scales, though the relative contribution of anthropogenic factors in relation to GCR flux presently is a matter of continued debate.
[8] Because there remains some uncertainty about which GCR energies are the most important drivers of cloud cover variation (if any), and because of the paucity of historical data on cosmic ray flux at various ranges of energies, controversies remain.
[9]
What is a mechanism whereby GCR flux variability may affect global climate?
Henrik Svensmark et al. have argued that solar variations modulate the cosmic ray signal seen at the earth and that this would affect cloud formation and hence climate. Cosmic rays have been experimentally determined to be able to produce ultra-small aerosol particles,
[10] orders of magnitude smaller than
cloud condensation nuclei (CCN). But the steps from this to modulation of
cloud formation and thence to be a contributor of
global warming have not been established. The analogy is with the
Wilson cloud chamber, however acting on a global scale, where
earth's atmosphere acts as the
cloud chamber and the cosmic rays
catalyze the production of
CCN. But unlike a cloud chamber, where the air is carefully purified, the real atmosphere always has many CCN naturally. Various proposals have been made for the exact mechanism by which cosmic rays might affect clouds, including Ion Mediated Nucleation, and through an indirect effect on current flow density in the Global electric circuit (see Tinsley 2000, and F. Yu 1999).
Claims have been made of identification of GCR climate signals in atmospheric parameters such as high latitude precipitation (Todd & Kniveton), and Svensmark's annual cloud cover variations, which were said to be correlated to GCR variation.
That Svensmark's work can be extrapolated to suggest any meaningful connection with global warming is disputed.
[11]
:''At the time we pointed out that while the experiments were potentially of interest, they are a long way from actually demonstrating an influence of cosmic rays on the real world climate, and in no way justify the hyperbole that Svensmark and colleagues put into their press releases and more 'popular' pieces. Even if the evidence for solar forcing were legitimate, any bizarre calculus that takes evidence for solar forcing of climate as evidence against greenhouse gases for current climate change is simply wrong. Whether cosmic rays are correlated with climate or not, they have been regularly measured by the neutron monitor at Climax Station (Colorado) since 1953 and show no long term trend. No trend = no explanation for current changes.''
[12]
See-also
Global warming#Solar variation.
Cosmic rays and fiction
Because of the metaphysical connotations of the word "cosmic", the very name of these particles enables their misinterpretation by the public, giving them an aura of mysterious powers. Were they merely referred to as "high-speed protons and atomic nuclei" this might not be so.
In fiction, cosmic rays have been used as a catchall, mostly in comics (notably the ''
Marvel Comics'' group the
Fantastic Four), as a source for
mutation and therefore the powers gained by being bombarded with them.
References
1. Luis Anchordoqui, Thomas Paul, Stephen Reucroft, John Swain. ''Ultrahigh Energy Cosmic Rays: The state of the art before the Auger Observatory''. (2002) arxiv:hep-ph/0206072
2. ''Science'', 23 September 2005, Vol 309, Issue 5743
3.
Evidence for large century time-scale changes in solar activity in the past 32 Kyr, based on in-situ cosmogenic 14C in ice at Summit, Greenland, , Devendra, Lal, Earth and Planetary Science Letters,
4. The Cosmic Ray Radiation Dose in Interplanetary Space – Present Day and Worst-Case Evaluations R.A. Mewaldt et al, page 103, 29th International Cosmic Ray Conference Pune (2005) 00, 101-104
5. NASA Facts: Understanding Space Radiation
6. sciencebits.com/CosmicRaysClimate
7. sciencebits.com/ice-ages
8. sciencebits.com/CO2orSolar
9. sciencebits.com/ClimateDebate
10. Henrik Svensmark, Jens Olaf Pepke Pedersen, Nigel Marsh, Martin Enghoff and Ulrik Uggerhøj, "Experimental Evidence for the role of Ions in Particle Nucleation under Atmospheric Conditions",
''Proceedings of the Royal Society A'', (Early Online Publishing), 2006.
11. RealClimate: Taking Cosmic Rays for a spin retrieved 22-Feb-2007
12. RealClimate: Nigel Calder in the Times, retrieved 22-Feb-2007
★ C. D. Anderson and S. H. Neddermeyer, Cloud Chamber Observations of Cosmic Rays at 4300 Meters Elevation and Near Sea-Level, Phys. Rev 50, 263,(1936).
★ M. Boezio et al, Measurement of the flux of atmospheric muons with the CAPRICE94 apparatus, Phys. Rev. D 62, 032007, (2000).
★ R. Clay and B. Dawson, Cosmic Bullets, Allen & Unwin, 1997.
★ P. K. F. Grieder, Cosmic Rays at Earth: Researcher’s Reference Manual and Data Book, Elsevier, 2001.
★ J. Kremer et al, Measurement of Ground-Level Muons at Two Geomagnetic Locations, Phys. Rev. Lett. 83, 4241, (1999).
★ S. H. Neddermeyer and C. D. Anderson, Note on the Nature of Cosmic-Ray Particles, Phys. Rev. 51, 844, (1937).
★ D. Perkins, Particle Astrophysics, Oxford University Press, 2003. - Very interesting and well written book.
★ C. E. Rolfs and S. R. William, Cauldrons in the Cosmos, The University of Chicago Press, 1988.
★ J. F. Ziegler, The Background In Detectors Caused By Sea Level Cosmic Rays, Nuclear Instruments and Methods 191, 419, (1981).
★ 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.
★ Martin Walt, Introduction to Geomagnetically Trapped Radiation, 1994.
★ A. M. Hillas, ''Cosmic Rays'', Pergamon Press, Oxford, 1972 - A good overview of the history and science of cosmic ray research including reprints of seminal papers by Hess, Anderson, Auger and others.
★ B. Rossi, ''Cosmic Rays'', McGraw-Hill, New York, 1964.
★ Thomas Gaisser, ''Cosmic Rays and Particle Physics'', Cambridge University Press, 1990.
★ TRACER Long Duration Balloon Project: the largest cosmic ray detector launched on balloons.
★
HiRes Fly's Eye
★
Particle Data Group review of Cosmic Rays by W.-M. Yao et al., Journal of Physics G 33, 1 (2006).
★
Introduction to Cosmic Ray Showers by Konrad Bernlöhr.
★ [ftp://ftp.ncdc.noaa.gov/pub/data/paleo/icecore/Greenland/summit/gisp2/cosmoiso/gisp2-14c-2005.txt NOAA FTP]: Lal, D., et al., 2005. Data on cosmic ray flux derived from C14 concentrations in the GISP2 Greenland
ice core.
★
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.
★
Links to on-line tool to estimate the soft error sensitivity of circuits.
★
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
★
Composition of Solar cosmic rays
★
"Who's Afraid of a Solar Flare? Solar activity can be surprisingly good for astronauts." Oct. 7, 2005, at Science@NASA]
See also
★
cosmogenic nuclides
★
cosmic ray spallation
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