The TeV-scale cosmic ray proton and helium spectra: Contributions from the local sources

详细信息    查看全文

• 作者：YONG-YEON KEUM ; PIERRE SALATI
• 关键词：PAMELA–CREAM anomaly ; cosmic ray nuclei (proton–helium) spectrum ; diffusion and transport of cosmic ray. ; 98.70.Sa ; 98.62.Gq ; 98.58.Mj ; 95.30.Cq
• 刊名：Pramana
• 出版年：2016
• 出版时间：February 2016
• 年：2016
• 卷：86
• 期：2
• 页码：369-377
• 全文大小：303 KB
• 参考文献：[1]D Maurin, F Donato, R Taillet, and P Salati, Astrophys. J. 555, 19 (2001)
  [2]D Maurin, R Taillet, and F Donato, Astron. Astrophys. 394, 1039 (2002)CrossRef ADS
  [3]D Maurin, R Taillet, F Donato, P Salati, A Barrau and G Boudoul, LAPTH-949, arXiv:astro-ph/​0212111 (unpublished)
  [4]A W Strong and I V Moskalenko, Astrophys. J. 509, 212 (1998)CrossRef ADS
  [5]GALPROP project web page: http://​galprop.​stanford.​edu
  [6]C Evoli, D Gaggero, D Grasso, and L Maccione, J. Cosmol. Astropart. Phys. 0810, 018 (2008)CrossRef ADS
  [7]G D Bernardo, C Evoli, D Gaggero, D Grasso, and L Maccione, Astropart. Phys. 34, 274 (2010)CrossRef ADS
  [8]CREAM Collaboration: H S Ahn et al, Astrophys. J. 714, L89 (2010)
  [9]CREAM Collaboration: Y S Yoon et al, Astrophys. J. 728, 122 (2011)
  [10]PAMELA Collaboration: O Adriani et al, Science 332, 69 (2011)
  [11]M Malkov, P Diamond, and R Sagdeev, Phys. Rev. Lett. 108, 081104 (2012)CrossRef ADS
  [12]Y Ohira and K Ioka, Astrophys. J. 729, L13 (2011)CrossRef ADS
  [13]T Stanev, P L Biermann, and T K Gaisser, Astron. Astrophys. 274, 902 (1993)ADS
  [14]V I Zatsepin and N V Sokolskaya, Astron. Astrophys. 458, 5 (2006)CrossRef ADS
  [15]P L Biermann, J K Becker, J Dreyer, A Meli, E S Seo, and T Stanev, Astrophys. J. 725, 15 (2010)CrossRef
  [16]Q Yuan, B Zhang and X-J Bi, in: Contribution to the 32nd ICRC, Beijing, #1355 (2011), arXiv:11090076
  [17]M Ave, P J Boyle, C Höppner, J Marshall, and D Müller, Astrophys. J. 697, 106 (2009)CrossRef ADS
  [18]P Blasi, E Amato, and P D Serpico, Phys. Rev. Lett. 109, 061101 (2012)CrossRef ADS
  [19]N Tomassetti, Astrophys. J. 752, L13 (2012)CrossRef ADS
  [20]J R Hörandel, N N Kalmykov, and A V Timokhin, Astropart. Phys. 27, 119 (2007)CrossRef ADS
  [21]P Blasi and E Amato, J. Cosmol. Astropart. Phys. 2012, 28 (2011)
  [22]A E Vladimirov, G Jóhannesson, I V Moskalenko, and T A Porter, Astrophys. J. 752, 68 (2012)CrossRef ADS
  [23]D A Green, arXiv:0905.​3699 (2009), URL http:​ /​/​www.​mrao.​cam.​ac.​uk/​surveys/​snrs
  [24]R N Machester, C B Hobbs, A Teoh, and M Hobbs, Astron. J. 129, 1993 (2005)CrossRef ADS
  [25]ATNF pulsar catalogue, http://​www.​atnf.​csiro.​au/​research/​pulsar/​psrcat/​
  [26]A D Erlykin and A W Wolfendale, Astropart. Phys. 35, 14 (2011)
  [27]S Thoudam and J R Hörandel, Mon. Not. R. Astron. Soc. 421, 1209 (2012)CrossRef ADS
  [28]G Bernard, T Delahaye, P Salati, and R Taillet, Astron. Astrophys. 544, A92 (2012)CrossRef ADS
  [29]A Putze, L Derome, and D Maurin, Astron. Astrophys. 516, 20 (2010)CrossRef
  [30]D Maurin, A Putze, and L Derome, Astron. Astrophys. 516, A67 (2010)CrossRef ADS
  [31]A W Strong, T A Porter, S W Digel, G Johannesson, P Martin, I V Moskalenko, and E J Murphy, Astrophys. J. 722, 7 (2010)CrossRef
  [32]T Bringmann, F Donato, and R A Lineros, J. Cosmol. Astropart. Phys. 2012, 049 (2012)CrossRef
  
• 作者单位：YONG-YEON KEUM (1)
  PIERRE SALATI (2)
  
  1. Institute of Basic Science, Seoul National University, 1 Kwan-Ak-Ro, Kwan-Ak-Gu, Seoul, Republic of Korea
  2. LAPTH, Université de Savoie, CNRS, 9 chemin de Bellevue, BP110, F-74941, Annecy-le-Vieux Cedex, France
  
• 刊物类别：Physics and Astronomy
• 刊物主题：Physics
  Physics
  Astronomy
  Astrophysics
  
• 出版者：Springer India
• ISSN：0973-7111

文摘

Recent measurements of cosmic ray proton and helium spectra show a hardening above a few hundreds of GeV. This excess is hard to understand in the framework of the conventional models of galactic cosmic ray production and propagation. Here, we propose to explain this anomaly by the presence of local sources. Cosmic ray propagation is described as a diffusion process taking place inside a two-zone magnetic halo. We calculate the proton and helium fluxes at the Earth between 50 GeV and 100 TeV. Improving over a similar analysis, we consistently derive these fluxes by taking into account both local and remote sources for which a unique injection rate is assumed. We find cosmic ray propagation parameters for which the proton and helium spectra remarkably agree with the PAMELA and CREAM measurements over four decades in energy. Keywords PAMELA–CREAM anomaly cosmic ray nuclei (proton–helium) spectrum diffusion and transport of cosmic ray.