Dip in UHECR spectrum as signature of proton interaction with CMB

被引：175
作者：
Berezinsky, V [1 ]
Gazizov, AZ
Grigorieva, SI
机构：
[1] Ist Nazl Fis Nucl, Lab nazl Gran Sasso, I-67010 Assergi, AQ, Italy
[2] DESY, D-157 Zeuthen, Germany
[3] Russian Acad Sci, Inst Nucl Res, Moscow 117312, Russia
来源：
PHYSICS LETTERS B | 2005年 / 612卷 / 3-4期
基金：
俄罗斯基础研究基金会;
关键词：
ultrahigh energy cosmic rays;
D O I：
10.1016/j.physletb.2005.02.058
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Ultrahigh energy (UHE) extragalactic protons propagating through cosmic microwave radiation (CMB) acquire the spectrum features in the form of the dip, bump (pile-up protons) and the Greisen-Zatsepin-Kuzmin (GZK) cutoff. We have performed the analysis of these features in terms of the modification factor. This analysis is weakly model-dependent, especially in case of the dip. The energy shape of the dip is confirmed by the Akeno-AGASA data with chi(2) = 19.06 for d.o.f. = 17 with two free parameters used for comparison. The agreement with HiRes data is also very good. This is the strong evidence that UHE cosmic rays observed at energies 1 X 10(18)-4 x 10(19) eV are extragalactic protons propagating through CMB. The dip is also present in case of diffusive propagation in magnetic field.. (c) 2005 Elsevier B.V. All rights reserved.
引用
收藏
页码：147 / 153
页数：7
相关论文
共 37 条
  • [31] Photodisintegration of ultra-high-energy cosmic rays: A new determination
    Stecker, FW
    Salamon, MH
    [J]. ASTROPHYSICAL JOURNAL, 1999, 512 (02) : 521 - 526
  • [32] TAKEDA M, ASTROPH0209422
  • [33] BL Lacertae are probable sources of the observed ultrahigh energy cosmic rays
    Tinyakov, PG
    Tkachev, II
    [J]. JETP LETTERS, 2001, 74 (09) : 445 - 448
  • [34] WATSON A, 2004, P CRIS 2004 C CAT
  • [35] High-energy cosmic rays from γ-ray bursts
    Wick, SD
    Dermer, CD
    Atoyan, A
    [J]. ASTROPARTICLE PHYSICS, 2004, 21 (02) : 125 - 148
  • [36] ENERGY-SPECTRUM OF ULTRA-HIGH ENERGY COSMIC-RAYS WITH EXTRA-GALACTIC ORIGIN
    YOSHIDA, S
    TESHIMA, M
    [J]. PROGRESS OF THEORETICAL PHYSICS, 1993, 89 (04): : 833 - 845
  • [37] [No title captured]
1234