1 / 21

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.

keola
Download Presentation

CTA and Cosmic-ray Physics

An Image/Link below is provided (as is) to download presentation Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author. Content is provided to you AS IS for your information and personal use only. Download presentation by click this link. While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server. During download, if you can't get a presentation, the file might be deleted by the publisher.

E N D

Presentation Transcript

  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)

More Related