Solar Energetic Particle Spectrum on 2006 December 13 Determined by IceTop

Abbasi, Rasha; Ackermann, M.; Adams, J.; Ahlers, M.; Ahrens, J.; Andeen, K.; Auffenberg, J.; Bai, X.; Baker, M. D.; Baret, B.; Barwick, S. W.; Bay, R.; Alba, J. L. Bazo; Beattie, K.; Becka, T.; Becker, J.; Becker, K. H.; Berghaus, P.; Berley, D.; Bernardini, E.; Bertrand, D.; Besson, D. Z.; Bieber, J. W.; Blaufuss, E.; Boersma, D. J.; Böhm, C.; Bolmont, J.; Böser, S.; Botner, O.; Braun, J.; Breder, D.; Burgess, T.; Castermans, T.; Chirkin, D.; Christy, B.; Clem, J.; Cowen, D. F.; D’Agostino, M. V.; Danninger, M.; Davour, Anna; Day, C. T.; Clercq, C. De; Demirörs, L.; Depaepe, O.; Descamps, F.; Desiati, P.; Vries-Uiterweerd, G. de; DeYoung, T.; Díaz–Vélez, Juan Carlos; Dreyer, J.; Dumm, J.; Duvoort, M. R.; Edwards, W. R.; Ehrlich, R.; Eisch, J.; Ellsworth, R. W.; Engdegaard, O.; Euler, S.; Evenson, P. A.; Fadiran, O.; Fazely, A. R.; Filimonov, K.; Finley, C.; Foerster, M. M.; Fox, B. D.; Franckowiak, A.; Franke, Robert; Gaisser, T. K.; Gallagher, J.; Ganugapati, R.; Gerhardt, L.; Gladstone, L.; Goldschmidt, A.; Goodman, J. A.; Gozzini, R.; Grant, D.; Griesel, T.; Groß, A.; Grullon, S.; Gunasingha, R. M.; Gurtner, M.; Ha, C.; Hallgren, A.; Halzen, F.; Han, K.; Hanson, K.; Hardtke, D.; Hardtke, R.; Hasegawa, Y.; Heise, J.; Helbing, K.; Hellwig, M.; Herquet, P.; Hickford, S.; Hill, G. C.; Hoffman, K. D.; Hoshina, K.; Hubert, D.; Hülß, J.-P.; Hulth, P. O.; Hultqvist, K.; Hundertmark, S.; Imlay, R.; Inaba, M.; Ishihara, A.; Jacobsen, J.; Japaridze, G. S.; Johansson, H.; Joseph, J.; Kampert, K.‐H.; Kappes, A.; Karg, T.; Karle, A.; Kawai, H.; Kelley, J. L.; Kiryluk, J.; Kislat, Fabian; Klein, S. R.; Klepser, S.; Kohnen, G.; Kolanoski, H.; Köpke, L.; Kowalski, M.; Kowarik, T.; Krasberg, M.; Kuêhn, K.; Kuwabara, T.; Labare, M.; Laihem, K.; Landsman, H.; Lauer, R.; Leich, H.; Leier, Dominik; Lücke, Andreas; Lundberg, J.; Lünemann, J.; Madsen, J.; Maruyama, R.; Mase, K.; Matis, H. S.; McParland, C.; Meagher, K.; Meli, A.; Merck, M.; Messarius, T.; Mészáros, P.; Miyamoto, H.; Mohr, Anna; Montaruli, T.; Morse, R.; Movit, S. M.; Münich, K.; Nahnhauer, R.; Nam, J. W.; Nießen, P.; Nygren, D. R.; Odrowski, S.; Olivas, A.; Olivo, M.; Ono, M.; Panknin, S.; Patton, S.; Heros, C. Pérez de los; Petrović, J.; Piegsa, A.; Pieloth, D.; Pohl, A. C.; Porrata, R.; Potthoff, Nils; Pretz, J.; Price, P. B.; Przybylski, G. T.; Pyle, R.; Rawlins, K.; Razzaque, S.; Redl, P.; Resconi, E.; Rhode, W.; Ribordy, M.; Rizzo, A.; Robbins, William; Rodrigues, J. P.; Roth, Peter M.; Rothmaier, F.; Rott, C.; Roucelle, C.; Rutledge, D.; Ryckbosch, D.; Sander, H. G.; Sarkar, S.; Satalecka, K.; Schlenstedt, S.; Schmidt, T.; Schneider, D.; Schultz, O.; Seckel, D.; Semburg, B.; Seo, S. h.; Sestayo, Y.; Seunarine, S.; Silvestri, A.; Smith, A. J.; Song, Cui-Ying; Spiczak, G. M.; Spiering, Christian; Stanev, T.; Stezelberger, T.; Stokstad, R. G.; Stoufer, M. C.; Stoyanov, S.; Strahler, E. A.; Straszheim, T.; Sulanke, K.-H.; Sullivan, G. W.; Swillens, Q.; Taboada, I.; Tarasova, O.; Tepe, A.; Ter–Antonyan, S.; Tilav, S.; Tluczykont, M.; Toale, P. A.; Tosi, D.; Turčan, D.; Eijndhoven, N. van; Vandenbroucke, J.; Overloop, A. Van; Viscomi, V.; Vogt, Christian; Voigt, B.; Walck, C.; Waldenmaier, T.; Waldmann, H.; Walter, Michael; Wendt, C.; Westerhoff, S.; Whitehorn, N.; Wiebusch, C. H.; Wiedemann, C.; Wikström, G.; Williams, D. R.; Wischnewski, R.; Wissing, H.; Woschnagg, K.; Xu, X. W.; Yodh, G.; Yoshida, Shigeru

doi:10.1086/595679

Cited by 39 publications

(10 citation statements)

References 9 publications

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“…Some large SEP events are so intense that the intensity of the accompanying highenergy (>1 GeV) protons exceeds the lower-energy portion of the galactic cosmic ray (GCR) background in at least one of the many ground-based neutron monitors (e.g., Lopate 2006), muon detectors (Falcone et al 2003;Abbasi et al 2008), or ionization chambers (Forbush 1946). Such increases in the radiation levels on Earth's surface that are detected by neutron monitors are commonly known as GLEs.…”

Section: Ground Level Enhancementsmentioning

confidence: 99%

Large gradual solar energetic particle events

Desai

Giacalone

2016

Living Rev. Sol. Phys.

420

305

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Solar energetic particles, or SEPs, from suprathermal (few keV) up to relativistic (∼few GeV) energies are accelerated near the Sun in at least two ways: (1) by magnetic reconnection-driven processes during solar flares resulting in impulsive SEPs, and (2) at fast coronal-mass-ejection-driven shock waves that produce large gradual SEP events. Large gradual SEP events are of particular interest because the accompanying high-energy (>10s MeV) protons pose serious radiation threats to human explorers living and working beyond low-Earth orbit and to technological assets such as communications and scientific satellites in space. However, a complete understanding of these large SEP events has eluded us primarily because their properties, as observed in Earth orbit, are smeared due to mixing and contributions from many important physical effects. This paper provides a comprehensive review of the current state of knowledge of these important phenomena, and summarizes some of the key questions that will be addressed by two upcoming missions-NASA's Solar Probe Plus and ESA's Solar Orbiter. Both of these missions are designed to directly and repeatedly sample the near-Sun environments where interplanetary scattering and transport effects are significantly reduced, allowing us to discriminate between different acceleration sites and mechanisms and to isolate the contributions of numerous physical processes occurring during large SEP events.

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Section: Ground Level Enhancementsmentioning

confidence: 99%

Large gradual solar energetic particle events

Desai

Giacalone

2016

Living Rev. Sol. Phys.

420

305

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“…This means the polar stations have essentially the same energy response, and there is no need to invoke complex analysis procedures to disentangle anisotropy effects from spectrum effects. Abbasi et al (2008) concluded that these procedures can yield misleading results during the early anisotropic phase of a GLE. Third, the polar stations have excellent directional sensitivity.…”

Section: Overview Of the Giant Ground Level Enhancementmentioning

confidence: 99%

Giant Ground Level Enhancement of Relativistic Solar Protons on 2005 January 20. I. Spaceship Earth Observations

Bieber

Clem

Evenson

et al. 2013

ApJ

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A ground level enhancement (GLE) is a solar event that accelerates ions (mostly protons) to GeV range energies in such great numbers that ground-based detectors, such as neutron monitors, observe their showers in Earth's atmosphere above the Galactic cosmic ray background. GLEs are of practical interest because an enhanced relativistic ion flux poses a hazard to astronauts, air crews, and aircraft electronics, and provides the earliest direct indication of an impending space radiation storm. The giant GLE of 2005 January 20 was the second largest on record (and largest since 1956), with up to 4200% count rate enhancement at sea level. We analyzed data from the Spaceship Earth network, supplemented to comprise 13 polar neutron monitor stations with distinct asymptotic viewing directions and Polar Bare neutron counters at South Pole, to determine the time evolution of the relativistic proton density, energy spectrum, and three-dimensional directional distribution. We identify two energy-dispersive peaks, indicating two solar injections. The relativistic solar protons were initially strongly beamed, with a peak maximum-to-minimum anisotropy ratio over 1000:1. The directional distribution is characterized by an axis of symmetry, determined independently for each minute of data, whose angle from the magnetic field slowly varied from about 60 • to low values and then rose to about 90 • . The extremely high relativistic proton flux from certain directions allowed 10 s tracking of count rates, revealing fluctuations of period 2 minutes with up to 50% fractional changes, which we attribute to fluctuations in the axis of symmetry.

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“…Besides its high-energy cosmicray physics program IceTop also allows the study of heliospheric events through the variation of individual DOM trigger rates. 9 Furthermore, a search for air showers without muons in IceCube allowed setting a limit on the relative abundance of PeV photons. 10 A study of the anisotropy of cosmic rays is currently in progress.…”

Section: Other Results and Conclusionmentioning

confidence: 99%

Status of the Icetop Air Shower Array at the South Pole

Kislat¹

2012

Astroparticle, Particle, Space Physics, Radiation Interaction, Detectors and Medical Physics Applications

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The IceTop air shower array is the surface component of the IceCube Neutrino Observatory at the geographic South Pole. The combination of IceTop and IceCube provides a new and powerful tool to measure cosmic ray composition in the energy range between about 300 TeV and 1 EeV by detecting the electromagnetic component at the surface in coincidence with the muon bundle in the deep underground detector. The paper will give an overview of the current status of the detector and the first physics results will be presented.

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Solar Energetic Particle Spectrum on 2006 December 13 Determined by IceTop

Cited by 39 publications

References 9 publications

Large gradual solar energetic particle events

Large gradual solar energetic particle events

Giant Ground Level Enhancement of Relativistic Solar Protons on 2005 January 20. I. Spaceship Earth Observations

Status of the Icetop Air Shower Array at the South Pole

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