Cosmic rays from 100 TeV up to the EeV regime: a review J.C. Arteaga-Velázquez Instituto de Física y Matemáticas, Universidad Michoacana Morelia, Michoacan, Mexico Content 1. Very high-energy astroparticle physics 2. Introduction to cosmic rays 3. Review 4. Detection at very-high energies 5. Experimental update 6. Multi-messenger/Multi-wavelength studies 7. Future detectors 8. Summary J.C. Arteaga - Cosmic rays 1 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
1. Very-high energy astroparticle physics J.C. Arteaga - Cosmic rays 2 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
The astroparticle physics field Astrophysics SNR IC 443, WISE/FERMI-LAT Particle physics Cosmology Astroparticle physics PbP collision in ALICE (2012) Galaxy distribution in the universe, Millenium simulation J.C. Arteaga - Cosmic rays 3 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Areas of research High energy (> 10 6 eV) astroparticle physics: Windows to the most energetic phenomena in the universe Particle cosmology Cosmic rays Cosmic abundances Dark matter High-/low-energy neutrinos Dark energy Gamma-ray astronomy Gravitational waves Structure of the universe Nonthermal sources (Supernova, AGN, GRB,…) Beyond standard model J.C. Arteaga - Cosmic rays 4 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Very-high energy astroparticle physics • Cosmic rays • Neutrinos PDG (2018) F. Halzen et al., Front. Astro. Sp. Sci. (2019) • Gamma rays A. Abdo, PRL 104 (2010) • Spectra of high energy cosmic rays, gamma rays and neutrinos follow power- law functions. Spectra are not of thermal origin J.C. Arteaga - Cosmic rays 5 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Very-high energy astroparticle physics • Test hadronic interactions at • Search for HE • Constrain models of the galactic and energies and regions of phase counterparts. local magnetic field LIGO/VIRGO/FERMI-LAT Cabral&Leedom(1993) space not available to current particle accelerators All-sky view of the magnetic field and CERN total intensity of dust emission measured by Planck (ESA) p-p collision ( √ s cm = 7 TeV) in ALICE VHE astroparticle • Find and understand the high-energy • Put limits on physics beyond physics processes that occur in astrophysical the standard model environments Dark matter Dark Black hole in M87 Energy NASA/EHT Baryonic matter • P r o b e m a t t e r a n d radiation of the inter- stellar/-galactic medium. J.C. Arteaga - Cosmic rays 6 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
2. Introduction to cosmic rays J.C. Arteaga - Cosmic rays 7 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Brief historical background Discovery: 1911-1912 “a radiation of very high penetrating power enters our atmosphere from above” V. F . Hess V. F. Hess, Phys. Z. 13, (1912) 1084 J.C. Arteaga - Cosmic rays 8 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Brief historical background Nature of the radiation: 1927-1936 A. Compton CR’s are charged particles. J. Clay, A. Compton, R. Millikan, et al. observed dependence of CR intensity with latitude. J.C. Arteaga - Cosmic rays 9 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Brief historical background Composition: 1940-1941 M. Schein Direct measurements in non-tripulated balloons carried out by M. Schein et al. at altitudes up to 20 km. Cosmic rays are dominated by protons M. Schein et al., Phys. Rev. 59, (1941) 615 J.C. Arteaga - Cosmic rays 10 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Cosmic ray known properties • One of the most energetic and enigmatic form of radiation from outer space • Composed by atomic nuclei: - Atomic nuclei (99 %) : H (85%), He (3%), Z ≥ 3 (3%) - Electrons (1 %) - Traces of antiparticles • Energy ranges from 100 MeV to 10 20 eV • Spectrum follows roughly a power law F(E) = E - γ • Origin is galactic and extragalactic: - Sun (E < 10 GeV), - Supernova remnants (E~TeV), - Extragalactic sources (E > 1 EeV). • Diffusive propagation in space: Age ~ O (10 7 yr) at HE’s J.C. Arteaga - Cosmic rays 11 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Cosmic ray open questions • How are they accelerated? • What are the sources of cosmic rays? LHC (CERN) • What are they made of? Open questions • Where are they accelerated • How do they propagate in the space? NASA/Modelo JF GAIA’s star map of our galaxy (ESA) • What is the origin of the features in their energy spectrum? Propagation of 10 18 eV CR ’s in the galaxy J.C. Arteaga - Cosmic rays 12 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
What do we need? • Multi-wavelength observations (E < • Cosmic ray measurements on: - Composition, MeV’s): - radio, microwave, infrared, visible, - energy, - arrival direction. UV, X-rays. Chandra X-ray telescope Addressing the mystery KASCADE-Grande detector of cosmic rays • Multi-messenger measurements: - Gamma rays (E > MeV’s) - Neutrinos (E > GeV’s) ICECUBE ν observatory HAWC γ -ray observatory J.C. Arteaga - Cosmic rays 13 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
3. Review J.C. Arteaga - Cosmic rays 14 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Energy spectrum Galactic Transition? Extragalactic γ = 2.7 γ = 3.1 F(E) = E - γ γ = 2.9 Knee γ ~ 3.3 Low energy ankle γ = 2.6 2nd. Knee LHC(pp) Ankle GZK Cut? J.C. Arteaga - Cosmic rays 15 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Origin Spectrum: γ = 2.7 Particle density: Energy density: J.C. Arteaga - Cosmic rays 16 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Origin Galactic cosmic rays: ρ RC = 1 eV/cm 3 V DG = π (20 kpc) 2 (300 pc) = 10 66 cm 3 τ escape = 10 7 years 300 pc L RC = V DG ρ RC / T DG ∼ 10 41 erg/s 40 kpc Supernova remnants Tycho SNR K SNR = 10 51 erg L SNR = K SNR x 3 SN/Siglo ∼ 10 42 erg/s L RC ∼ 10% L SNR Chandra X-ray Observatory J.C. Arteaga - Cosmic rays 17 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Acceleration mechanism Diffusive magnetic acceleration in shock fronts: • Fermi’s 1 st order mechanism Δ E/E ~ (v 2 /c) = β Effects at source: • Non lineal • Late phase of SNR • Different kinds of SNR’s • Spectrum of shape dN/dE ∼ E –( γ o + ε ) where γ o = 2 y ε < 1 M. Cardillo, A. Amato, P . • Maximum energy B. Peters, Nuovo Cimento 22 (1961) 800 Blasi (2015) E Zcut ~ Ze x B x R All = Ze E Hcut H He CNO Prediction of cuts/knees in spectra Fe • With magnetic field amplification or in very young SNR’s, then E Hcut up to 10 15 eV! A.R. Bell, Astrop. Phys. 43 (2013) S. Gabici et al., ApJ 665 (2007) L131 J.C. Arteaga - Cosmic rays 18 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Acceleration mechanism Production in the laboratory of astrophysical shocks by using supersonic plasmas C. K. Li et al., PRL 123, 055002 (2019) Schocked region Laser Expanding shell plasma with compressed B and ρ (300 - 400 km/s) Gasbag (H) filled tube Jet (e’s, 1200 - 1400 km/s) Washer Jet Hemispherical target • Electromagnetic shockwave • Magnetic turbulence • Electron acceleration in shocked region and in Weibel’s turbulences: - Spectrum follows a power-law - Consistent with 1st order Fermi acceleration J.C. Arteaga - Cosmic rays 19 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Sources Hilla’s plot: Size (L) vs magnetic field (B) of potential cosmic ray accelerators: E max ~ Ze ⋅ B ⋅ R No e ffi ciency losses are considered 1 0 1 7 e 1 v 0 1 p 5 r e o v t o p n r o t o n P .M. Bauleo et al, Nature 458 (2009) J.C. Arteaga - Cosmic rays 20 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Sources Galactic center Magnetars Superbubbles Supernova remnants
Sources Hilla’s model - Knee’s are the result of loss of magnetic confinement at the source. - Four types of sources to describe all-particle energy spectrum Knee H Knee H - Population 1: SNR (E max ~ 100 TeV) - Population 2: Galactic Pevatron PWN, SNR (E max ~ 1 PeV), galactic center, etc. - Population 3: Galactic Eevatron past Hypernovae/GRB’s. - Population 4: Extragalactic. S. Tilav, ISVHECRI (2014) T.K.Gaisser et al., Frontiers of Phys. 8 (2013) J.C. Arteaga - Cosmic rays 22 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
Propagation S. Mollerach, E. Roulet, Prog. in Part. and Nuc. Phys. 98 (2018) 85 Spallation Fragmentation • These secondary nuclei: • At low energies (GeV’s) CR composition is similar to that of our solar system . - Li, Be, B, F , - Sc, Ti, V, Cr, Mn, • But abundances of some rare elements in can be used as cosmic clocks, solar system are larger in CR’s: using primary-to-secondary ratios - Effect of spallation/fragmentation of primaries in space. J.C. Arteaga - Cosmic rays 23 2019 Meeting of the Mexican Cosmic Ray Division , Puebla, Nov, 2019
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