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Search for EeV protons of galactic origin

Title
Search for EeV protons of galactic origin
Authors
Abbasi, R. U.Abe, M.Abu-Zayyad, T.Allen, M.Azuma, R.Barcikowski, E.Belz, J. W.Bergman, D. R.Blake, S. A.Cady, R.Cheon, B. G.Chiba, J.Chikawa, M.Fujii, T.Fukushima, M.Goto, T.Hanlon, W.Hayashi, Y.Hayashi, M.Hayashida, N.Hibino, K.Honda, K.Ikeda, D.Inoue, N.Ishii, T.Ishimori, R.Ito, H.Ivanov, D.Jui, C. C. H.Kadota, K.Kakimoto, E.Kalashev, K.Kasahara, K.Kawai, H.Kawakami, S.Kawana, S.Kawata, K.Kido, E.Kim, H. B.Kim, J. H.Kishigami, S.Kitamura, S.Kitamura, Y.Kuzmin, V.Kwon, Y. J.Lan, J.Lubsandorzhiev, B.Lundquist, J. P.Machida, K.Martens, K.Matsuda, T.Matsuyama, T.Matthews, J. N.Minamino, M.Mukai, K.Myers, I.Nagasawa, K.Nagataki, S.Nakamura, T.Nonaka, T.Nozato, A.Ogio, S.Ogura, J.Ohnishi, M.Ohoka, H.Oki, K.Okuda, T.Ono, M.Onogi, R.Oshima, A.Ozawa, S.Park, I. H.Pshirkov, M. S.Rodriguez, D. C.Rubtsov, G.Ryu, D.Sagawa, H.Saito, K.Saito, Y.Sakaki, N.Sakurai, N.Scott, L. M.Sekino, K.Shah, P. D.Shibata, T.Shibata, F.Shimodaira, H.Shin, B. K.Shin, H. S.Smith, J. D.Sokolsky, P.Stokes, B. T.Stratton, S. R.Stroman, T. A.Suzawa, T.Takahashi, Y.Takamura, M.Takeda, M.Takeishi, R.Taketa, A.Takita, M.Tameda, Y.Tanaka, M.Tanaka, K.Tanakai, H.Thomas, S. B.Thomson, G. B.Tinyakov, P.Tirone, A. H.Tkachev, I.Tokuno, H.Tomida, T.Troitsky, S.Tsunesada, Y.Tsutsumi, K.Uchihori, Y.Udo, S.Urban, F.Wong, T.Yamane, R.Yamaoka, H.Yamazaki, K.Yang, J.Yashiro, K.Yoneda, Y.Yoshida, S.Yoshii, H.Zollinger, R.Zundel, Z.
Ewha Authors
양종만
SCOPUS Author ID
양종만scopus
Issue Date
2017
Journal Title
ASTROPARTICLE PHYSICS
ISSN
0927-6505JCR Link1873-2852JCR Link
Citation
vol. 86, pp. 21 - 26
Keywords
Cosmic rayGalactic protonsTelescope arraySurface detector
Publisher
ELSEVIER SCIENCE BV
Indexed
SCI; SCIE; SCOPUS WOS scopus
Abstract
Cosmic rays in the energy range 10(18.0)-10(18.5) eV are thought to have a light, probably protonic, composition. To study their origin one can search for anisotropy in their arrival directions. Extragalactic cosmic rays should be isotropic, but galactic cosmic rays of this type should be seen mostly along the galactic plane, and there should be a shortage of events coming from directions near the galactic anticenter. This is due to the fact that, under the influence of the galactic magnetic field, the transition from ballistic to diffusive behavior is well advanced, and this qualitative picture persists over the whole energy range. Guided by models of the galactic magnetic field that indicate that the enhancement along the galactic plane should have a standard deviation of about 20 degrees in galactic latitude, and the deficit in the galactic anticenter direction should have a standard deviation of about 50 degrees in galactic longitude, we use the data of the Telescope Array surface detector in 10(18.0) to 10(18.5) eV energy range to search for these effects. The data are isotropic. Neither an enhancement along the galactic plane nor a deficit in the galactic anticenter direction is found. Using these data we place an upper limit on the fraction of EeV cosmic rays of galactic origin at 1.3% at 95% confidence level. Published by Elsevier B.V.
DOI
10.1016/j.astropartphys.2016.11.001
Appears in Collections:
자연과학대학 > 물리학전공 > Journal papers
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