Ultra-high-energy cosmic ray

In astroparticle physics, an ultra-high-energy cosmic ray (UHECR) is a cosmic ray particle with a kinetic energy greater than 1×1018 eV, far beyond both the rest mass and energies typical of other cosmic ray particles.

An extreme-energy cosmic ray (EECR) is an UHECR with energy exceeding 5×1019 eV (about 8 joule), the so-called Greisen–Zatsepin–Kuzmin limit (GZK limit). This limit should be the maximum energy of cosmic ray particles that have traveled long distances (about 160 million light years), since higher-energy ray particles would have lost energy over that distance due to scattering from photons in the cosmic microwave background. It follows that EECR could not be survivors from the early universe but are cosmologically "young", emitted somewhere in the Local Supercluster by some unknown physical process.

These particles are extremely rare; between 2004 and 2007, the initial runs of the Pierre Auger Observatory detected 27 events with estimated arrival energies above 5.7×1019 eV, i.e., about one such event every four weeks in the 3000 km2 area surveyed by the observatory.[1]

There is evidence that these highest-energy cosmic rays might be iron nuclei, rather than the protons that make up most cosmic rays.[2]

The postulated (hypothetical) sources of EECR are known as Zevatrons, named in analogy to Lawrence Berkeley National Laboratory's Bevatron and Fermilab's Tevatron, and therefore capable of accelerating particles to 1 ZeV (1021 eV, zetta-electronvolt). In 2004 there was a consideration of the possibility of galactic jets acting as Zevatrons, due to diffusive acceleration of particles caused by shock waves inside the jets. In particular, models suggested that shock waves from the nearby M87 galactic jet could accelerate an iron nucleus to ZeV ranges.[3] In 2007, PAO tentatively associated EECR with extragalactic supermassive black holes at the center of nearby galaxies called active galactic nuclei (AGN).[4] Extremely high energies might be explained also by the Centrifugal mechanism of acceleration [5] in the magnetospheres of AGN. Although newer results indicate that fewer than 40% of these cosmic rays seemed to be coming from the AGN, a much weaker correlation than previously reported.[2] A more speculative suggestion by Grib and Pavlov (2007, 2008) envisages the decay of superheavy dark matter by means of the Penrose process.

Observational history

Main article: Oh-My-God particle

The first observation of a cosmic ray particle with an energy exceeding 1.0×1020 eV (16 J) was made by Dr John D Linsley and Livio Scarsi at the Volcano Ranch experiment in New Mexico in 1962.[6][7]

Cosmic ray particles with even higher energies have since been observed. Among them was the Oh-My-God particle observed on the evening of 15 October 1991 over Dugway Proving Ground, Utah. Its observation was a shock to astrophysicists, who estimated its energy to be approximately 3×1020 eV (50 J)[8]—in other words, an atomic nucleus with kinetic energy equal to that of a baseball (5 ounces or 142 grams) traveling at about 100 kilometers per hour (60 mph).

The energy of this particle is some 40 million times that of the highest energy protons that have been produced in any terrestrial particle accelerator. However, only a small fraction of this energy would be available for an interaction with a proton or neutron on Earth, with most of the energy remaining in the form of kinetic energy of the products of the interaction. The effective energy available for such a collision is the square root of double the product of the particle's energy and the mass energy of the proton, which for this particle gives 7.5×1014 eV, roughly 50 times the collision energy of the Large Hadron Collider.

Since the first observation, by the University of Utah's Fly's Eye Cosmic Ray Detector, at least fifteen similar events have been recorded, confirming the phenomenon. These very high energy cosmic ray particles are very rare; the energy of most cosmic ray particles is between 10 MeV and 10 GeV.

Ultra-high-energy cosmic ray observatories

See also: Category:High energy particle telescopes and Cosmic-ray observatory

Pierre Auger Observatory

Pierre Auger Observatory is an international cosmic ray observatory designed to detect ultra-high-energy cosmic ray particles (with energies beyond 1020 eV). These high-energy particles have an estimated arrival rate of just 1 per square kilometer per century, therefore, in order to record a large number of these events, the Auger Observatory has created a detection area of 3,000 km² (the size of Rhode Island, USA) in Mendoza Province, western Argentina. A larger cosmic-ray detector array is also planned for the northern hemisphere as part of the Pierre Auger complex. The Pierre Auger Observatory, in addition to obtaining directional information from the cluster of water tanks used to observe the cosmic-ray-shower components, also has four telescopes trained on the night sky to observe fluorescence of the nitrogen molecules as the shower particles traverse the sky, giving further directional information on the original cosmic ray particle.

Suggested explanations

Neutron Stars accelerating particles to UHECR energies

One suggested source of UHECR particles is their origination from neutron stars. In young neutron stars with spin periods of <10ms, the magnetohydrodynamic (MHD) forces from the quasi-neutral fluid of superconducting protons and electrons existing in a neutron superfluid accelerate iron nuclei to UHECR velocities. The magnetic field produced by the neutron superfluid in rapidly-rotating stars creates a magnetic field of 108–1011 tesla, at which point the neutron star is classified as a magnetar. This magnetic field is the strongest in the observed universe and creates the relativistic MHD wind believed to accelerate iron nuclei remaining from the supernova to the necessary energy.

Another hypothesized source of UHECRs from neutron stars is during neutron star to strange star combustion. This hypothesis relies on the assumption that strange matter is the ground state of matter which has no experimental or observational data to support it. Due to the immense gravitational pressures from the neutron star, it is believed that small pockets of matter consisting of up, down, and strange quarks in equilibrium acting as a single hadron (as opposed to a number of Σ0 baryons). This will then combust the entire star to strange matter, at which point the neutron star becomes a strange star and its magnetic field breaks down, which occurs because the protons and neutrons in the quasi-neutral fluid have become strangelets. This magnetic field breakdown releases large amplitude electromagnetic waves (LAEMWs). The LAEMWs accelerate light ion remnants from the supernova to UHECR energies.

Very high energy cosmic ray electrons might be explained by the Centrifugal mechanism of acceleration in the magnetospheres of the Crab-like Pulsars.[9]

Active galactic cores as one possible source of the particles

Interactions with blue-shifted cosmic microwave background radiation limit the distance that these particles can travel before losing energy; this is known as the Greisen–Zatsepin–Kuzmin limit or GZK limit.

The source of such high energy particles has been a mystery for many years. Recent results from the Pierre Auger Observatory show that ultra-high-energy cosmic ray arrival directions appear to be correlated with extragalactic supermassive black holes at the center of nearby galaxies called active galactic nuclei (AGN).[4] However, since the angular correlation scale used is fairly large (3.1 degrees) these results do not unambiguously identify the origins of such cosmic ray particles. The AGN could merely be closely associated with the actual sources, for example in galaxies or other astrophysical objects that are clumped with matter on large scales within 100 Mpc.

Some of the supermassive black holes in AGN are known to be rotating, as in the Seyfert galaxy MCG 6-30-15[10] with time-variability in their inner accretion disks.[11] Black hole spin is a potentially effective agent to drive UHECR production,[12] provided ions are suitably launched to circumvent limiting factors deep within the galactic nucleus, notably curvature radiation[13] and inelastic scattering with radiation from the inner disk. Low-luminosity, intermittent Seyfert galaxies may meet the requirements with the formation of a linear accelerator several light years away from the nucleus, yet within their extended ion tori whose UV radiation ensures a supply of ionic contaminants.[14] The corresponding electric fields are small, on the order of 10 V/cm, whereby the observed UHECRs are indicative for the astronomical size of the source. Improved statistics by the Pierre Auger Observatory will be instrumental in identifying the presently tentative association of UHECRs (from the Local Universe) with Seyferts and LINERs.[15]

Other possible sources of the particles

Other possible sources of the UHECR are:

Relation with dark matter

Main article: Dark matter

It is hypothesized that active galactic nuclei are capable of converting dark matter into high energy protons. Yuri Pavlov and Andrey Grib at the Alexander Friedmann Laboratory for Theoretical Physics at St. Petersburg hypothesize that dark matter particles are about 15 times heavier than protons, and that they can decay into pairs of heavier virtual particles of a type that interacts with ordinary matter.[20] Near an active galactic nucleus, one of these particles can fall into the black hole, while the other escapes, as described by the Penrose process. Some of the particles that escape will collide with incoming particles creating collisions of very high energy. It is in these collisions, according to Pavlov, that ordinary visible protons can form. These protons would have very high energies. Pavlov claims that evidence of this is present in the form of ultra-high-energy cosmic ray particles.[21] Ultra-high energy cosmic ray particles may also be produced by the decay of super-heavy dark matter "X particles"[22] such as Holeums.[23][24] Such very energetic decay products, carrying a fraction of the mass of the X particle, are believed to be a plausible explanation for the observed ultra-high energy cosmic rays (UHECR).

High energy cosmic ray particles traversing intergalactic space suffer the GZK cutoff above 1020 eV due to interactions with cosmic background radiation if the primary cosmic ray particles are protons or nuclei. The Pierre Auger Project, HiRes and Yakutsk Extensive Air Shower Array found the GZK cutoff, while Akeno-AGASA observed the events above the cutoff (11 events in the past 10 years). The result of the Akeno-AGASA experiment is smooth near the GZK cutoff energy. If one assumes that the Akeno-AGASA result is correct and consider its implication, a possible explanation for the AGASA data on GZK cutoff violation would be a shower caused by dark matter particles. A dark matter particle is not constrained by the GZK cutoff, since it interacts weakly with cosmic background radiation. Recent measurements by the Pierre Auger Project have found a correlation between the direction of high energy cosmic ray particles and the location of AGN.[25]

See also

References

  1. ↑ Watson, L. J.; Mortlock, D. J.; Jaffe, A. H. (2011). "A Bayesian analysis of the 27 highest energy cosmic rays detected by the Pierre Auger Observatory". Monthly Notices of the Royal Astronomical Society 418 (1): 206–213. arXiv:1010.0911. Bibcode:2011MNRAS.418..206W. doi:10.1111/j.1365-2966.2011.19476.x.
  2. 1 2 "Cosmic-ray theory unravels". Nature 463: 1011. 22 February 2010. doi:10.1038/4631011a.
  3. ↑ Honda, M.; Honda, Y. S. (2004). "Filamentary Jets as a Cosmic-Ray "Zevatron"". The Astrophysical Journal Letters 617: L37–L40. arXiv:astro-ph/0411101. Bibcode:2004ApJ...617L..37H. doi:10.1086/427067.
  4. 1 2 The Pierre Auger Collaboration; Abreu; Aglietta; Aguirre; Allard; Allekotte; Allen; Allison; Alvarez; Alvarez-Muniz; Ambrosio; Anchordoqui; Andringa; Anzalone; Aramo; Argiro; Arisaka; Armengaud; Arneodo; Arqueros; Asch; Asorey; Assis; Atulugama; Aublin; Ave; Avila; Backer; Badagnani; et al. (2007). "Correlation of the Highest-Energy Cosmic Rays with Nearby Extragalactic Objects". Science 318 (5852): 938–943. arXiv:0711.2256. Bibcode:2007Sci...318..938P. doi:10.1126/science.1151124. PMID 17991855.
  5. ↑ Osmanov Z., Mahajan S., Machabeli G. & Chkheidze N. Monthly Notices of the Royal Astronomical Society, Volume 445, Issue 4, p.4155-4160
  6. ↑ Linsley, J. (1963). "Evidence for a Primary Cosmic-Ray Particle with Energy 1020 eV". Physical Review Letters 10 (4): 146–148. Bibcode:1963PhRvL..10..146L. doi:10.1103/PhysRevLett.10.146.
  7. ↑ Sakar, S. (1 September 2002). "Could the end be in sight for ultrahigh-energy cosmic rays?". Physics World. pp. 23–24. Retrieved 2014-07-21.
  8. ↑ Baez, J. C. (July 2012). "Open Questions in Physics". DESY. Retrieved 2014-07-21.
  9. ↑ Mahajan Swadesh, Machabeli George, Osmanov Zaza & Chkheidze Nino. Nature Scientific Reports, Volume 3, id. 1262 (2013)
  10. ↑ Tanaka, Y.; et al. (1995). "Gravitationally redshifted emission implying an accretion disk and massive black hole in the active galaxy MCG-6-30-15". Nature 375 (6533): 659–661. Bibcode:1995Natur.375..659T. doi:10.1038/375659a0.
  11. ↑ Iwasawa, K.; et al. (1996). "The variable iron K emission line in MCG-6-30-15". Monthly Notices of the Royal Astronomical Society 282 (3): 1038–1048. arXiv:astro-ph/9606103. Bibcode:1996MNRAS.282.1038I. doi:10.1093/mnras/282.3.1038.
  12. ↑ Boldt, E.; Gosh, P. (1999). "Cosmic rays from remnants of quasars?". Monthly Notices of the Royal Astronomical Society 307 (3): 491–494. arXiv:astro-ph/9902342. Bibcode:1999MNRAS.307..491B. doi:10.1046/j.1365-8711.1999.02600.x.
  13. ↑ Levinson, A. (2000). "Particle Acceleration and Curvature TeV Emission by Rotating, Supermassive Black Holes". Physical Review Letters 85 (5): 912–915. Bibcode:2000PhRvL..85..912L. doi:10.1103/PhysRevLett.85.912.
  14. ↑ van Putten, M. H. P. M.; Gupta, A. C. (2009). "Non-thermal transient sources from rotating black holes". Monthly Notices of the Royal Astronomical Society 394 (4): 2238–2246. arXiv:0901.1674. Bibcode:2009MNRAS.394.2238V. doi:10.1111/j.1365-2966.2009.14492.x.
  15. ↑ Moskalenko, I. V.; Stawarz, L.; Porter, T. A.; Cheung, C.-C. (2009). "On the Possible Association of Ultra High Energy Cosmic Rays with Nearby Active Galaxies". The Astrophysical Journal 63 (2): 1261–1267. arXiv:0805.1260. Bibcode:2009ApJ...693.1261M. doi:10.1088/0004-637X/693/2/1261.
  16. ↑ Wang, X.-Y.; Razzaque, S.; Meszaros, P.; Dai, Z.-G. (2007). "High-energy cosmic rays and neutrinos from semirelativistic hypernovae". Physical Review D 76 (8): 083009. arXiv:0705.0027. Bibcode:2007PhRvD..76h3009W. doi:10.1103/PhysRevD.76.083009.
  17. ↑ Chakraborti, S.; Ray, A.; Soderberg, A. M.; Loeb, A.; Chandra, P. (2011). "Ultra-high-energy cosmic ray acceleration in engine-driven relativistic supernovae". Nature Communications 2: 175. arXiv:1012.0850. Bibcode:2011NatCo...2E.175C. doi:10.1038/ncomms1178.
  18. ↑ Waxman, E. (1995). "Cosmological Gamma-Ray Bursts and the Highest Energy Cosmic Rays". Physical Review Letters 75 (3): 386–389. arXiv:astro-ph/9505082. Bibcode:1995PhRvL..75..386W. doi:10.1103/PhysRevLett.75.386.
  19. ↑ Milgrom, M.; Usov, V. (1995). "Possible Association of Ultra–High-Energy Cosmic-Ray Events with Strong Gamma-Ray Bursts". The Astrophysical Journal Letters 449: L37. arXiv:astro-ph/9505009. Bibcode:1995ApJ...449L..37M. doi:10.1086/309633.
  20. ↑ Grib, A. A.; Pavlov, Yu. V. (2009). "Active galactic nuclei and transformation of dark matter into visible matter". Gravitation and Cosmology 15 (1): 44–48. arXiv:0810.1724. Bibcode:2009GrCo...15...44G. doi:10.1134/S0202289309010125.
  21. ↑ Grib, A. A.; Pavlov, Yu. V. (2008). "Do Active Galactic Nuclei Convert Dark Matter Into Visible Particles?". Modern Physics Letters A 23 (16): 1151–1159. arXiv:0712.2667. Bibcode:2008MPLA...23.1151G. doi:10.1142/S0217732308027072.
  22. ↑ Barbot, C. (2002). "Ultra-high energy cosmic rays from super-heavy X particle decay". arXiv:hep-ph/0210280 [hep-ph].
  23. ↑ Chavda, L. K.; Chavda, A. L. (2002). "Dark matter and stable bound states of primordial black holes". Classical and Quantum Gravity 19 (11): 2927–2938. arXiv:gr-qc/0308054. Bibcode:2002CQGra..19.2927C. doi:10.1088/0264-9381/19/11/311.
  24. ↑ Chavda, A. L.; Chavda, L. K. (2008). "Ultra High Energy Cosmic Rays from decays of Holeums in Galactic Halos". arXiv:0806.0454 [physics.gen-ph].
  25. ↑ Tomozawa, Y. (2008). "Search for a dark matter particle in high energy cosmic rays". arXiv:0804.1499 [astro-ph].

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