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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. 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
2190:; 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".
964:; 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".
598:. However, since the angular correlation scale used is fairly large (3.1°) 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
427:
Pierre Auger
Observatory is an international cosmic ray observatory designed to detect ultra-high-energy cosmic ray particles (with energies beyond 10 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
686:
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 in Saint Petersburg hypothesize that dark matter particles are about 15 times heavier than protons,
613:
MCG 6-30-15 with time-variability in their inner accretion disks. Black hole spin is a potentially effective agent to drive UHECR production, provided ions are suitably launched to circumvent limiting factors deep within the galactic nucleus, notably curvature radiation and inelastic scattering with
744:
Alves
Batista, Rafael; Biteau, Jonathan; Bustamante, Mauricio; Dolag, Klaus; Engel, Ralph; Fang, Ke; Kampert, Karl-Heinz; Kostunin, Dmitriy; Mostafa, Miguel; Murase, Kohta; Oikonomou, Foteini; Olinto, Angela V.; Panasyuk, Mikhail I.; Sigl, Guenter; Taylor, Andrew M.; Unger, Michael (2019).
593:
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
691:. Some of those particles will collide with incoming particles; these are very high energy collisions which, according to Pavlov, can form ordinary visible protons with very high energy. Pavlov then claims that evidence of such processes are ultra-high-energy cosmic ray particles.
206:, 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. A more speculative suggestion by Grib and Pavlov (2007, 2008) envisages the decay of superheavy
111:(GZK limit). This limit should be the maximum energy of cosmic ray protons that have traveled long distances (about 160 million light years), since higher-energy protons would have lost energy over that distance due to scattering from photons in the
687:
and that they can decay into pairs of heavier virtual particles of a type that interacts with ordinary matter. Near an active galactic nucleus, one of these particles can fall into the black hole, while the other escapes, as described by the
528:). 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
290:. 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 (see
440:. 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
317:, 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.
480:. This magnetic field is the strongest stable field in the observed universe and creates the relativistic MHD wind believed to accelerate iron nuclei remaining from the supernova to the necessary energy.
194:
could accelerate an iron nucleus to ZeV ranges. In 2007, the Pierre Auger
Observatory observed a correlation of EECR with extragalactic supermassive black holes at the center of nearby galaxies called
495:
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
476:
accelerate iron nuclei to UHECR velocities. The neutron superfluid in rapidly rotating stars creates a magnetic field of 10 to 10 teslas, at which point the neutron star is classified as a
294:). 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
451:
In
September 2017, data from 12 years of observations from PAO supported an extragalactic source (outside of Earth's galaxy) for the origin of extremely high energy cosmic rays.
360:(Gamma Ray Astronomy PeV EnergieS 3rd establishment) is a project for cosmic ray study with air shower detector array and large area muon detectors at Ooty in southern India.
532:. This magnetic field breakdown releases large amplitude electromagnetic waves (LAEMWs). The LAEMWs accelerate light ion remnants from the supernova to UHECR energies.
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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
363:
314:
1613:
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".
410:
615:
183:, and therefore capable of accelerating particles to 1 ZeV (10 eV, zetta-electronvolt). In 2004 there was a consideration of the possibility of
1348:
Tanaka, Y.; et al. (1995). "Gravitationally redshifted emission implying an accretion disk and massive black hole in the active galaxy MCG-6-30-15".
160:. However, nuclear physics processes lead to limits for iron nuclei similar to that of protons. Other abundant nuclei should have even lower limits.
326:
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198:. However, the strength of the correlation became weaker with continuing observations. Extremely high energies might be explained also by the
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The energy of this particle is some 40 million times that of the highest energy protons that have been produced in any terrestrial
1668:
Wang, X.-Y.; Razzaque, S.; Meszaros, P.; Dai, Z.-G. (2007). "High-energy cosmic rays and neutrinos from semirelativistic hypernovae".
385:
352:
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molecules as the shower particles traverse the sky, giving further directional information on the original cosmic ray particle.
62:, that is, about one such event every four weeks in the 3,000 km (1,200 sq mi) area surveyed by the observatory.
2315:
2300:
1853:
Milgrom, M.; Usov, V. (1995). "Possible
Association of Ultra–High-Energy Cosmic-Ray Events with Strong Gamma-Ray Bursts".
2290:
1727:; Loeb, A.; Chandra, P. (2011). "Ultra-high-energy cosmic ray acceleration in engine-driven relativistic supernovae".
564:
112:
152:
nuclei, rather than the protons that make up most cosmic rays. For an iron nucleus, the corresponding limit would be
1963:
Grib, A. A.; Pavlov, Yu. V. (2009). "Active galactic nuclei and transformation of dark matter into visible matter".
2295:
2078:
1615:
718:
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is developing technology for a distributed network of low-cost detectors for UHECR showers in collaboration with
400:
2259:
2187:
2020:
1965:
1507:
Levinson, A. (2000). "Particle Acceleration and Curvature TeV Emission by Rotating, Supermassive Black Holes".
961:
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249:
51:
2018:
Grib, A. A.; Pavlov, Yu. V. (2008). "Do Active Galactic Nuclei Convert Dark Matter Into Visible Particles?".
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number of these events, the Auger Observatory has created a detection area of 3,000 km (the size of
1729:
372:– Mixed Apparatus for Radar Investigation of Cosmic-rays of High Ionization located on Long Island, USA.
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of the total energy of the nucleus. There is evidence that these highest-energy cosmic rays might be
1176:
1724:
798:"A Bayesian analysis of the 27 highest energy cosmic rays detected by the Pierre Auger Observatory"
703: – very-high-energy particles that flow into the Solar System from beyond the Milky Way galaxy
2235:
2201:
2175:
2113:
2087:
2076:
Elbert, J. W.; Sommers, P. (1995). "In search of a source for the 320 EeV Fly's Eye cosmic ray".
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2000:
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observed by the University of Utah's Fly's Eye experiment on the evening of 15 October 1991 over
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limit the distance that these particles can travel before losing energy; this is known as the
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from the quasi-neutral fluid of superconducting protons and electrons existing in a neutron
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Cosmic ray particles with even higher energies have since been observed. Among them was the
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Waxman, E. (1995). "Cosmological Gamma-Ray Bursts and the Highest Energy Cosmic Rays".
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2004:
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Hansson, J; Sandin, F (2005). "Preon stars: a new class of cosmic compact objects".
1776:
1493:
1278:"First detection of photons with energy beyond 100 TeV from an astrophysical source"
1086:
Linsley, J. (1963). "Evidence for a Primary Cosmic-Ray Particle with Energy 10 eV".
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1941:
1839:
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Another hypothesized source of UHECRs from neutron stars is during neutron star to
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These particles are extremely rare; between 2004 and 2007, the initial runs of the
283:(5 ounces or 142 grams) traveling at about 100 kilometers per hour (60 mph).
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nucleons, then the GZK limit applies to its nucleons, which carry only a fraction
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Honda, M.; Honda, Y. S. (2004). "Filamentary Jets as a Cosmic-Ray "Zevatron"".
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Mahajan, Swadesh; Machabeli, George; Osmanov, Zaza; Chkheidze, Nino (2013).
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quarks in equilibrium acting as a single hadron (as opposed to a number of
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The details of the event from the official site of the Fly's Eye detector.
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The first observation of a cosmic ray particle with an energy exceeding
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559:. The feasibility of electron acceleration to this energy scale in the
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468:. In young neutron stars with spin periods of <10 ms, the
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2148:
Seife, C. (2000). "Fly's Eye Spies Highs in Cosmic Rays' Demise".
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1979:
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One suggested source of UHECR particles is their origination from
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40:
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intergalactic shocks created during the epoch of galaxy formation
1156:
149:
1027:
Osmanov, Z.; Mahajan, S.; Machabeli, G.; Chkheidze, N. (2014).
349:
believed to be caused by ultra-high-energy cosmic ray particles
54:(PAO) detected 27 events with estimated arrival energies above
1125:"Could the end be in sight for ultrahigh-energy cosmic rays?"
1029:"Extremely efficient Zevatron in rotating AGN magnetospheres"
747:"Open Questions in Cosmic-Ray Research at Ultrahigh Energies"
855:
853:
115:(CMB). It follows that EECR could not be survivors from the
16:
Cosmic-ray particle with a kinetic energy greater than 1 EeV
487:
combustion. This hypothesis relies on the assumption that
119:, but are cosmologically "young", emitted somewhere in the
1554:"Non-thermal transient sources from rotating black holes"
1203:"Ultra High Energy Electrons Powered by Pulsar Rotation"
659:, left over from phase transitions in the early universe
1177:"Study confirms cosmic rays have extragalactic origins"
714:
Pages displaying short descriptions of redirect targets
563:
magnetosphere is supported by the 2019 observation of
2127:
Cosmic Bullets: High Energy Particles in Astrophysics
796:
Watson, L. J.; Mortlock, D. J.; Jaffe, A. H. (2011).
727: – Ultra-high-energy cosmic ray detected in 1991
705:
Pages displaying wikidata descriptions as a fallback
411:
Cosmic-Ray Extremely Distributed Observatory (CREDO)
47:
and energies typical of other cosmic ray particles.
571:, a young pulsar with a spin period of 33 ms.
1395:"The variable iron K emission line in MCG-6-30-15"
1559:Monthly Notices of the Royal Astronomical Society
1453:Monthly Notices of the Royal Astronomical Society
1400:Monthly Notices of the Royal Astronomical Society
1033:Monthly Notices of the Royal Astronomical Society
803:Monthly Notices of the Royal Astronomical Society
712: – High-energy, heavy ions of cosmic origin
302:, roughly 50 times the collision energy of the
126:If an EECR is not a proton, but a nucleus with
2271:Origin of energetic space particles pinpointed
1552:van Putten, M. H. P. M.; Gupta, A. C. (2009).
655:decay products of supermassive particles from
163:The hypothetical sources of EECR are known as
364:High Resolution Fly's Eye Cosmic Ray Detector
8:
267:, who estimated its energy at approximately
609:in AGN are known to be rotating, as in the
35:with an energy greater than 1 EeV (10
721: – High-energy particles from the Sun
321:Ultra-high-energy cosmic ray observatories
2254:The Highest Energy Particle Ever Recorded
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751:Frontiers in Astronomy and Space Sciences
626:Other possible sources of the UHECR are:
345:(ANITA) detects ultra-high-energy cosmic
69:(EECR) is an UHECR with energy exceeding
327:Category:High energy particle telescopes
263:, Utah. Its observation was shocking to
1448:"Cosmic rays from remnants of quasars?"
736:
622:Other possible sources of the particles
339:– Akeno Giant Air Shower Array in Japan
107:% the speed of light), the so-called
584:cosmic microwave background radiation
549:Centrifugal mechanism of acceleration
200:centrifugal mechanism of acceleration
169:Lawrence Berkeley National Laboratory
7:
309:Since the first observation, by the
343:Antarctic Impulse Transient Antenna
123:by some unknown physical process.
386:Yakutsk Extensive Air Shower Array
353:Extreme Universe Space Observatory
14:
1856:The Astrophysical Journal Letters
1393:Iwasawa, K.; et al. (1996).
906:The Astrophysical Journal Letters
275:(50 J)—essentially an
1591:10.1111/j.1365-2966.2009.14492.x
1485:10.1046/j.1365-8711.1999.02600.x
835:10.1111/j.1365-2966.2011.19476.x
470:magnetohydrodynamic (MHD) forces
279:with kinetic energy equal to a
2311:Unsolved problems in astronomy
2188:The Pierre Auger Collaboration
2164:10.1126/science.288.5469.1147a
1942:10.1016/j.physletb.2005.04.034
1312:10.1103/PhysRevLett.123.051101
1276:Amenomori, M. (13 June 2019).
1123:Sakar, S. (1 September 2002).
962:The Pierre Auger Collaboration
535:"Ultra-high-energy cosmic ray
1:
2277:, published January 13, 2005.
2125:Clay, R.; Dawson, B. (1997).
588:Greisen–Zatsepin–Kuzmin limit
551:in the magnetospheres of the
315:Fly's Eye Cosmic Ray Detector
109:Greisen–Zatsepin–Kuzmin limit
1647:10.1088/0004-637X/693/2/1261
1446:Boldt, E.; Gosh, P. (1999).
862:"Cosmic-ray theory unravels"
860:Hand, E (22 February 2010).
596:active galactic nuclei (AGN)
565:ultra-high-energy gamma rays
547:) might be explained by the
196:active galactic nuclei (AGN)
25:ultra-high-energy cosmic ray
1153:"Open Questions in Physics"
292:Collider § Explanation
113:cosmic microwave background
2332:
2264:analysis of the 1991 event
1824:10.1103/PhysRevLett.75.386
1723:Chakraborti, S.; Ray, A.;
1702:10.1103/PhysRevD.76.083009
1531:10.1103/PhysRevLett.85.912
1110:10.1103/PhysRevLett.10.146
679:
420:
401:Florida A&M University
324:
221:
2079:The Astrophysical Journal
2052:10.1142/S0217732308027072
1997:10.1134/S0202289309010125
1966:Gravitation and Cosmology
1616:The Astrophysical Journal
1151:Baez, J. C. (July 2012).
719:Solar energetic particles
676:Relation with dark matter
662:particles undergoing the
202:in the magnetospheres of
67:extreme-energy cosmic ray
2021:Modern Physics Letters A
1432:10.1093/mnras/282.3.1038
782:10.3389/fspas.2019.00023
701:Extragalactic cosmic ray
630:radio lobes of powerful
607:supermassive black holes
423:Pierre Auger Observatory
417:Pierre Auger Observatory
376:Pierre Auger Observatory
250:Volcano Ranch experiment
248:and Livio Scarsi at the
244:(16 J) was made by
52:Pierre Auger Observatory
2224:10.1126/science.1151124
1793:Physical Review Letters
1510:Physical Review Letters
1089:Physical Review Letters
998:10.1126/science.1151124
381:Telescope Array Project
252:in New Mexico in 1962.
43:), far beyond both the
455:Suggested explanations
331:Cosmic-ray observatory
224:Cosmic ray observatory
210: by means of the
167:, named in analogy to
2316:Unexplained phenomena
2301:Astroparticle physics
2274:, by Mark Peplow for
1730:Nature Communications
1213:(1). Springer: 1262.
1064:10.1093/mnras/stu2042
575:Active galactic cores
304:Large Hadron Collider
261:Dugway Proving Ground
218:Observational history
81:, or the energy of a
39:, approximately 0.16
21:astroparticle physics
543:with energies of ≥10
288:particle accelerator
85:traveling at ≈
2291:Subatomic particles
2266:, published in 1994
2216:2007Sci...318..938P
2158:(5469): 1147–1149.
2102:1995ApJ...441..151E
2044:2008MPLA...23.1151G
1989:2009GrCo...15...44G
1934:2005PhLB..616....1H
1879:1995ApJ...449L..37M
1816:1995PhRvL..75..386W
1753:2011NatCo...2..175C
1694:2007PhRvD..76h3009W
1639:2009ApJ...693.1261M
1582:2009MNRAS.394.2238V
1523:2000PhRvL..85..912L
1476:1999MNRAS.307..491B
1423:1996MNRAS.282.1038I
1364:1995Natur.375..659T
1304:2019PhRvL.123e1101A
1229:2013NatSR...3E1262M
1183:. 21 September 2017
1102:1963PhRvL..10..146L
1055:2014MNRAS.445.4155O
990:2007Sci...318..938P
929:2004ApJ...617L..37H
826:2011MNRAS.418..206W
773:2019FrASS...6...23B
657:topological defects
1761:10.1038/ncomms1178
1207:Scientific Reports
725:Oh-My-God particle
579:Interactions with
311:University of Utah
257:Oh-My-God particle
232:Amaterasu particle
228:Oh-My-God particle
121:Local Supercluster
2200:(5852): 938–943.
2140:978-0-7382-0139-9
2028:(16): 1151–1159.
1911:Physics Letters B
1671:Physical Review D
1358:(6533): 659–661.
1237:10.1038/srep01262
974:(5852): 938–943.
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1623:(2): 1261–1267.
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1467:astro-ph/9902342
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1407:(3): 1038–1048.
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1133:. pp. 23–24
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567:coming from the
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391:Tunka experiment
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2306:Cosmic rays
2260:John Walker
1181:EurekAlert!
682:Dark matter
670:Preon stars
600:megaparsecs
569:Crab Nebula
561:Crab pulsar
530:strangelets
399:project at
208:dark matter
2285:Categories
2262:'s lively
1295:1906.05521
1187:2017-09-22
1162:2014-07-21
1137:2014-07-21
764:1903.06714
732:References
646:supernovae
640:hypernovae
474:superfluid
436:, western
325:See also:
300:10 eV
273:10 eV
242:10 eV
222:See also:
158:10 eV
75:10 eV
60:10 eV
33:cosmic ray
2240:118376969
2207:0711.2256
2180:117341691
2035:0712.2667
1980:0810.1724
1950:119063004
1895:118923079
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1073:119195822
1046:1404.3176
1014:118376969
981:0711.2256
844:119068104
817:1010.0911
541:electrons
537:electrons
438:Argentina
347:neutrinos
165:Zevatrons
45:rest mass
2232:17991855
2172:10841723
2118:15510276
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2005:13867079
1832:10060008
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890:20182484
710:HZE ions
695:See also
478:magnetar
446:nitrogen
405:MARIACHI
370:MARIACHI
358:GRAPES-3
281:baseball
181:Tevatron
177:Fermilab
173:Bevatron
2212:Bibcode
2193:Science
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1985:Bibcode
1930:Bibcode
1875:Bibcode
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557:Pulsars
526:baryons
505:strange
491:is the
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2030:arXiv
2001:S2CID
1975:arXiv
1946:S2CID
1920:arXiv
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1335:2019
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1259:PMID
1241:ISSN
1157:DESY
1002:PMID
886:PMID
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501:down
395:The
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150:iron
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