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UHECRs from Black Hole Jets of Radio Galaxies

UHECRs from Black Hole Jets of Radio Galaxies. Chuck Dermer Naval Research Laboratory, Washington, DC. Soeb Razzaque (NRL), Justin Finke (NRL), and Armen Atoyan (Concordia U., Montreal). New Journal of Physics, 2009. Outline. UHECR Clustering Observations and GZK Horizon

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UHECRs from Black Hole Jets of Radio Galaxies

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  1. UHECRs from Black Hole Jets of Radio Galaxies Chuck Dermer Naval Research Laboratory, Washington, DC Soeb Razzaque (NRL), Justin Finke (NRL), and Armen Atoyan (Concordia U., Montreal) New Journal of Physics, 2009

  2. Outline • UHECR Clustering Observations and GZK Horizon • 2. UHECRs from Radio Galaxies/Blazars • 1.minimum apparent luminosity to accelerate UHECRs • 2. jet power from synchrotron theory • 3. Gamma Ray Emission from UHECRs accelerated in Radio Galaxies

  3. Pierre Auger Observatory Three major discoveries in 2007: 1. Anisotropy in the arrival directions of UHECRs (birth of charged particle astronomy) 2. GZK cutoff (also HiRes) 3. Mixed composition of UHECRs (Science Magazine, Nov. 2007)

  4. Stanev, Biermann, Lloyd-Evans, Rachen, and Watson 1995, PRL, 75, 3056 >56 EeV (27 events) AGN Catalog of Veron and Veron Cetty 694 AGNs z < 0.024 (< 75 Mpc) 1. Clustering in the arrival directions of UHECR

  5. GZK cutoff 2. GZK cutoff

  6. Extragalactic Background Light (see Finke X8 6)

  7. Horizon distance: Linear distance where proton with measured energy E had energy eE GZK Horizon CMBR only: GZK cutoff consistent with UHECR protons Thanks to Floyd Stecker For model-dependent definition: Harari, Mollerach, and Roulet 2006

  8. Neutral Beam Model for UHECRs: Radio Galaxies and GRBs Possible photon targets forp +: Internal:synchrotron radiation External:accretion disk radiation (UV) (i)direct accretion disk radiation: (ii) accretion disk radiation scattered in the broad-line region (Atoyan & Dermer 2001) quasi-isotropic,up toRBLR~ 0.1-1 pc Impact of the external accretion disk radiation component: high p-rates & lower threshold energies: protMeV/(1- cos) pg→p→n, g, n Neutrons escape to become UHECRs (Atoyan & Dermer 2003) =7 (solid) =10 (dashed) =15 (dot-dashed) (red - without ADR) (for 1996 flare of 3C 279)

  9. UHECRs from Radio Galaxies/AGNs UHECR arrival directions are associated with Cen A, Cen B, an FR II radio galaxy and a BL Lac object within 140 Mpc. IGR J21247+5058, an FR II broad-lined radio galaxy at z = 0.02 or d ≈ 80 Mpc (INTEGRAL), is 2.1 degrees away from a HiRes Stereo event with E > 56 EeV. Moskalenko et al. 2009 Zaw et al. 2009 > 8 of the 27 UHECRs with E > 56 EeV are within 3.5 of nearby radio galaxies. Seyfert 2, low ionization, radio-quiet galaxies closest to the UHECR arrival directions

  10. Centaurus A

  11. Maximum Particle Energy in Fermi Acceleration • need > 1046 erg s-1 apparent isotropic luminosity to accelerate UHECR protons by Fermi processes Cen A power: Bolometric radio luminosity: 4×1042 erg s-1 Fermi gamma-ray power: 5×1041 erg s-1 Hard X-ray/soft g-ray power: 5×1042 erg s-1 UHECR power: few ×1040 erg s-1

  12. What is Average Jet Power of Cen A? Total energy and lifetime: Cocoon dynamics (Begelman and Cioffi 1989 for Cyg A) New approach: Compton-synchrotron theory to infer minimum power magnetic field Jet/counter-jet asymmetry gives outflow speed Hardcastle et al. 2009 Pj(Cen A)  1044 erg s-1 

  13. 3. Composition of UHECRs • Astrophysical arguments: • MFPs • Galactic magnetic field/clustering • Protons Particle physics arguments: Shower properties Xmax, RMS of Xmax  Heavy (~Fe) nuclei

  14. Search for Enhancements near Radio Galaxies

  15. Cygnus A Atoyan and Dermer (2008) Gamma Ray Signatures of UHECRs in Radio Galaxies UHECR studies from Fermi Gamma ray Space Telescope and ground-based gamma-ray observatory data • Secondary nuclear production • Compton-scattered CMB in radio lobes • 3. Cascade g radiation from UHECRs in transit from source • 4. Accumulation and photohadronic production of UHECRs in lobes of Radio Galaxies

  16. Sources of the UHECRs Ruled out: Galactic sources young neutron stars or pulsars, black holes, GRBs in the Galaxy Particle physics sources superheavy dark matter particles in galactic halo top-down models, topological defects Clusters of galaxies Viable: Jets of AGNs: radio-loud or radio-quiet? Cen A!, M87? GRBs: Magnetars? Others? Requires nanoGauss intergalactic magnetic field (see Razzaque W8 3) UHECRs accelerated by black-hole jets

  17. Photon cascading in IGM

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