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CTA and Cosmic-ray Physics

CTA and Cosmic-ray Physics. Toru Shibata Aoyama-Gakuin University (26/Sep/2012). (1). capability of CTA for CR-physics. open questions in. hadronic components (proton, . . . . , iron). ●. leptonic components (electron, positron). ●. (2). All-particle spectrum of cosmic-rays.

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CTA and Cosmic-ray Physics

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  1. CTA and Cosmic-ray Physics Toru Shibata Aoyama-Gakuin University (26/Sep/2012) (1)

  2. capability of CTA for CR-physics open questions in hadronic components (proton, . . . . , iron) ● leptonic components (electron, positron) ● (2)

  3. All-particle spectrum of cosmic-rays equivalent center of mass energy (GeV) summarized by R. Engel (KIT) 1-ry p, He, . . , Fe, . . . - 2-ry (+ 1-ry?) p, B, sub-Fe, 10Be, . . e-, e+, g 1-ry + 2-ry (+ 2’-ry?) direct obs. indirect obs. PROTON satellite particle energy (eV/particle) (3)

  4. Energy spectra for individual elements Derbina, V. A., et al., 2005, ApJ, 628, L41 (4)

  5. recent results on proton & helium spectra Adriani et al. - Science - 332 (2011) 6025 ~2.75 really getting harder ? ~2.6 ~2.75 (5)

  6. average mass of cosmic-rays vs. 1-ry energy iron Derbina, V. A., et al., 2005, ApJ, 628, L41 lithium proton (6)

  7. shower maximum Xmax vs. 1-ry energy Etot smoothly connecting to direct data ? (7)

  8. Possibility ofhadronic spectra with CTA separation between hadrons and e-g components established ● separation between p, He, . . . . , Fe difficult, but ● probably OK L(p-He), M(C-N-O), H(Ne-Mg-Si), VH(Ca-Fe) <xmax> (elongation rate) longitudinal profile; <r> (lateral spread) transversal profile; (8)

  9. proton spectrum HEGRA; Hemberger, Ahronian, et al. 26th ICRC(1999) DE/E ~ 50% (9)

  10. possible enough separation between Ne, Mg, . . . . , Fe ● direct cherenkov photons from 1-ry heavy nuclei (Sitte, ICRC1965) Wakely, Kieda, Swordy; ICRC2001 10TeV g 10TeV Mg (10)

  11. qDC ~ 0.1° H.E.S.S. 30th ICRC(2007) qEAS ~ 1° (11)

  12. iron spectrum H.E.S.S. 30th ICRC(2007) (12)

  13. Possibility ofleptonic spectra with CTA all-electron spectrum (e-+ e+) on-board observation ●　nearby source ●　maximum accelerable energy ●　new components ● . . . . . . . . . (13)

  14. 1994: Nishimura; possibility of 1-ry electron observation with atmospheric cherenkov telescope (Proc. of Towards a Major Atmospheric Cherenkov Detector III, 1, edited by T. Kifune) 2008: HESS (Ahronian et al.), Phys. Rev. Lett. 101 (Phys. Rev. Lett. 101) 2011: MAGIC (Tridon et al.) (Proc. of 32th ICRC, Beijing) (14)

  15. uncertainty in indirect observation z = 1 electron Hadronness=0 electron (Electronness=1) (Aharonian et al.; arXiv:0811.3894v2, 2009) (D. B. Tridon; PhD thesis, MPI, 2011 (15)

  16. CTA < 50GeV ~ < 300GeV ~ < 100GeV ~ How about e/g – separation ? DX~15 g/cm2 for e/g ! DX~150 g/cm2 for p/Fe (dX~5 g/cm2) we should regard the data as an upper limit ? (16)

  17. Possibility of e/g – separation in CTA assuming the separation between hadron and EG (e+g) is established, how about between e and g ? DJ (q, f)= Jeast- Jwest (e- +de++g) (e+ + e- + de-+g) g-components subtracted but, even if possible, the energy range of e+ will be limited within 50-100GeV _ Kamioka et al. Astrop. Phys. 6 (1997) 155 - (17)

  18. moon shadow with geomagnetic field Amenomori et al. arXiv:0707.332v (2007) ~ 20%up? remark: - p/p ~ 10-4 around 100GeV e+/e- ~ 0.2 - e+-e- separation: much more hopeful than p-p separation (18)

  19. positron fraction charge dependent solar modulation ? (preliminary) - (19)

  20. Conclusion: CTA will bring us also fruitful data on charged components, both hadronic and leptonic ones, in the very high energy region where direct on-board experiments can not cover. Multi- wavelength with various elements, g, e-, e+, p, He, . . . . , sub-Fe, Fe (20)

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