From the Knee to the toes: The challenge of cosmic-ray composition

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1 New Views of the Universe December 8 th 13 th, 2005, Chicago From the Knee to the toes: The challenge of cosmic-ray composition Jörg R. Hörandel University of Karlsruhe www-ik.fzk.de/~joerg

2 New Views of the Universe December 8 th 13 th, 2005, Chicago From the Knee to the toes: The challenge of cosmic-ray composition JRH, astro-ph/ Jörg R. Hörandel University of Karlsruhe www-ik.fzk.de/~joerg

3 New Views of the Universe December 8 th 13 th, 2005, Chicago From the Knee to the toes: The challenge of cosmic-ray composition knee 2 nd knee ankle toes 26x 92x galactic? JRH, astro-ph/ Jörg R. Hörandel University of Karlsruhe www-ik.fzk.de/~joerg

4

5 acceleration of CR in supernova remnants Fermi acceleration finite lifetime of shock front: E max ~ Z ev propagation through galaxy Leakage from Galaxy: escape probability ~ f(z) CNO rigidity dependent cut-off E k ~Z? mass dependent cut-off E k ~ A extensive air showers B = 3 µg JRH, Astrop. Phys. 21 (2004) 241 Interactions with background particles (photons, neutrinos) New particle physics in atmosphere

6 TRACER Experiment - Mc Murdo, Antarctica LDB flight: December 12 th 26 th, 2003 ~ 40 km (3-5 g/cm 2 ) Z = 8-26 E = 1 GeV/n - ~10 TeV/n

7 TRACER energy spectra for individual elements D. Müller et al., Proc. 29 th ICRC, Pune (2005)

8 Extensive air showers P. Auger Jungfraujoch P. Auger W. Kolhörster et al., Naturwiss. 26 (1938) 576 P. Auger et al., Comptes renduz 206 (1938) 1721

9 KArlsruhe Shower Core and Array DEtector eē+ e + e - γ γ π 0 p p π + n π - Simultaneous measurement of electromagnetic, muonic, hadronic shower components µ - γ γ γ e + e - e - e + γ π 0 µ - e - π - π 0 p p n p π - π - n n π + µ + T. Antoni et al, Nucl. Instr. & Meth. A 513 (2004) 490

10 acceleration of CR in supernova remnants Interactions propagation through galaxy extensive air showers B = 3 µg

11 QGSJET 01 KASCADE: Test of interaction models Number of hadrons vs. number of muons N e -N µ analysis χ 2 distribution J. Milke et al., 29 th ICRC, Pune (2005)

12 acceleration of CR in supernova remnants Sources propagation through galaxy extensive air showers B = 3 µg

13 Acceleration of particles in supernova remnant p, O, Fe p e - γ π 0 γ ~kev ~TeV γ γ ASCA SN R RX J H.E.S.S.: TeV-Gamma rays ASCA: X-rays (kev) H.E.S.S. Experiment Namibia F.A. Aharonian, Nature 432 (2004) 75

14 KASCADE: Small scale anisotropy point source search no indication for point sources visible sky +-3 around galactic plane T. Antoni et al., ApJ 608 (2004) 865

15 acceleration of CR in supernova remnants Propagation propagation through galaxy extensive air showers B = 3 µg

16 ACE/CRIS Ratio of secondary to primary nuclei Leaky box model λ esc = 26.7βg/cm ( ) 0.58 βr/1.0 GV + ( βr/1.4 GV) N. E. Yanasak, ApJ 563 (2001) 768

17 Propagation pathlength in Galaxy λ~e -0.2 diffusion model 8 kpc * 1 p/cm 3 leaky box model λ = 26.7βg/cm ( ) 0.58 βr/1.0 GV + ( βr/1.4 GV) 1.4 N. E. Yanasak, ApJ 563 (2001) residual pathlength model λ = 6.0* R 10GV g/cm S.P. Swordy, 24th ICRC, Rome 2 (1995) 697 2

18 Anisotropy amplitude vs energy T. Antoni et al, ApJ 604 (2004) cos 2 sin 2 + = = = n i i n i i n n R α α r Rayleigh vector V.S. Ptuskin, Adv. Space Res. 19 (1997) 697 J. Candia et al., J. Cosmol. Astropart. Phys. 5 (2003) 3

19 acceleration of CR in supernova remnants Energy spectra & Mass composition propagation through galaxy extensive air showers B = 3 µg

20 SPASE-2 / AMANDA-B10 (South Pole) N e 1500 m E µ ρ e (30 m) E µ > 300 GeV 1980 m 120 m Rawlins et al, Proc. 28th ICRC, Tsukuba 1 (2003) 173

21 p-air cross section Fe N e Average p-p depth cross of section shower maximum X max depth X p CORSIKA/QGSJET 01 lower σ p-air lg N Nucl. Phys. B (Proc. Suppl.) 151 (2006) 75 JRH, J. Phys. G 29 (2003) 2439

22 p-air cross section Fe N e Average depth of shower maximum X max depth X p CORSIKA/QGSJET 01 lower σ p-air lg N Nucl. Phys. B (Proc. Suppl.) 151 (2006) 75 JRH, J. Phys. G 29 (2003) 2439

23 Mean logarithmic mass X max e,µ,h < i lna >= ri * lna JRH astro-ph/

24 KASCADE: Primary proton spectrum reconstructed from unaccompanied hadrons primary flux Φ 0 CORSIKA/ QGSJET Φ hadr T. Antoni et al, ApJ 612 (2004) 914 M. Aglietta et al., Astrop. Phys. 19 (2003) 329

25 Two dimensional shower size spectrum lg N e vs. lg N µ KASCADE A E 0 derive E 0 and A from N e and N µ data Fredholm integral equations of 1 st kind: g i (lg Ne,lg N µ ) ti (lg Ne,lg N µ = E) p ( E) de 0 i M Roth et al, 28 th ICRC, Tsukuba 1 (2003) 139

26 All-particle energy spectrum two hadronic interaction models: CORSIKA 6.018/GHEISHA QGSJET 01 -SIBYLL 2.1 T. Antoni et al., Astropart. Phys. 24 (2005) 1

27 KASCADE: Energy spectra for elemental groups Knee caused by cut-off for light elements Astrophysical interpretation limited by description of interactions in the atmosphere T. Antoni et al., Astropart. Phys. 24 (2005) 1

28 Proton Helium JRH astro-ph/

29 CNO O CNO Iron JRH astro-ph/ D. Müller et al., Proc. 29 th ICRC, Pune (2005) D. Müller et al., Proc. 29 th ICRC, Pune (2005)

30 KASCADE GRANDE Array 37 detector stations 370 m 2 e/γ: Scintillation counter KASCADE 200 m x 200 m 700 m 700 m G. Navarra et al., Nucl Instr & Meth A 518 (2004) 207

31 KASCADE-Grande N e -N µ correlation measurements preliminary R. Glasstetter et al., Proc. 29 th ICRC, Pune (2005)

32 Radio emission from air showers - LOPES Coherent emission of synchroton radiation in geomagnetic field e + e - E 0 =10 17 ev T. Huege expect signals ~ µv/(m MHz)

33 LOPES 30 antennas operating at KASCADE-Grande

34 LOPES first signals Position of shower in sky Nature 435 (2005) 313

35 Radio signal dependence on angle with respect to geomagnetic field 60 number of muons (i.e. primary energy) 0 Geosynchroton emission Nature 435 (2005) 313 ~ 1017 ev ~ 6*1017 ev Radio signal increases with energy

36 Hadrons at high altitude surviving protons 500 g/cm 2 1 PeV: ~ 6.5 λ i 320 m 2 sr 0.5 m 2 sr effective ideal: combination with air Cerenkov detector for calibration

37 New Views of the Universe December 8 th 13 th, 2005, Chicago From the Knee to the toes: The challenge of cosmic-ray composition Status: Description of interactions in atmosphere improved Mean mass increases as function of energy (knee region) Knee is caused by subsequential cut-offs for individual elements Astrophysical interpretation of EAS measurements limited by understanding of interactions in the atmosphere Perspectives: KASCADE-Grande (2nd knee) LOPES (radio signals) Radio in AUGER Hadrons at large altitude Proton spectrum } } galactic extragalactic ev >10 20 ev direct indirect ev Jörg R. Hörandel University of Karlsruhe, Germany www-ik.fzk.de/~joerg

38 D. Pernik M. Ave-Pernas Thanks to my colleagues... TRACER Experiment tracer.uchicago.edu A. Romero J.R. Hörandel P. Boyle G. Kelderhouse D. Müller

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