Optical depth against CMB Fairbairn Rashba Troitsky 2009

Optical depth against CMB Fairbairn, Rashba, Troitsky 2009; Roncadelli, de Angelis, Mansutti 2009

GZK効果 Lorentz不変性の破れ？ GZK limit = 5£ 1010 Ge. V p + CMB ! N + GZK限界を超える宇宙線 陽子は 100 Mpc以上の距 離を飛べない． GZK=Greisen-Zatsepin. Kuzmin(1966) From http: //pdg. lbl. gov/

Axion • Originally, a psued-Goldstone boson for the Peccei-Quinn chiral symmetry to resolve the strong CP problem. • Basic features of the invisible QCD axion – Weak coupling (chiral) : gaq ¼ mq/fa ; fa &108 Ge. V – Small mass by the QCD instaton effect: ma ¼ 10 -3 e. V (1010 Ge. V/ fa) a – Dark matter candidate q g 5 a. 0. 01 (fa/1010 Ge. V)1. 175 – Coupling to gauge fields via anomaly: g a F Æ F • General Definition (ALP) – A pseudo scalar with shift symmetry and P/CP violation g g

Axions in Astrophysics • Key point Axions are converted to and from photos by mixing: q a g 5 • Solar axions due to the Primakov effect: – CAST experiment at CERN(2007, 2008) Cast Collaboration (2008) ar. Xiv: 0810. 4482 g B, E

Primakoff Effect • Conversion rate where s is the screening scale given by • Total axion number flux at the Earth • Estimation – Axion flux: a=g 102 3. 75£ 1011 cm-2 s-1 – Axion luminosity: La= g 102 1. 85£ 10 -3 L⊙ – Average energy: h Ei =4. 2 ke. V, h E 2 i=22. 7 ke. V 2 Raffelt GG: Plasmon decay into low mass bosons in stars, PRD 37: 1356 (1988)

CAST Bounds CAST Collaboration (2008) ar. Xiv: 0810. 4482

Experimetal Constrants: summary S. J. Asztalos, L. J. Rosenberg, K. van Bibber, P. Sikivie, and K. Zioutas, “Searches for astrophysical and cosmological axions, ” Ann. Rev. Nucl. Part. Sci. 56 (2006) 293 -326.

J. Jaeckel, A. Ringwald: ar. Xiv: 1002. 0329 The Low-Energy Frontier of Particle Physics

-a Conversion by Magnetic Fields • Propagation equation where with pl 2=4 ne/me being the plasma frequency, and R and CM represents the Faraday rotation effect and the vacuum Cotton-Mouton effect, respectively. • Non-resonant conversion For homogeneous magnetic fields, where For a random sequence of N coherent domains [Grossman Y, Roy S, Zupan J: PLB 543: 23(2002)] • Resonant conversion

Spectral Deformation of Cosmic -rays by Galactic and Intergalactic Magnetic Fields • Photon-ALP conversion rate where • Estimations Can be observed by GLAST(10% deformation) and E*=102 Ge. V » 1 Te. V if ma ¼ 10 -6» 10 -8 e. V at the CAST bound on ga and – Intergalactic fields: Ldom» 1 Mpc, B=(1 -5)¢ 10 -9 G for D=200» 500 Mpc – Intracluster fields: Ldom» 10 kpc, B=10 -6 G, ne' 10 -3 cm-3 for D= 1 Mpc – Galactic fields: Ldom» 10 kpc, B=(2 -4)¢ 10 -6 G, ne' 10 -3 cm-3 for D= 1 Mpc De Angelis A, Mansutti O, Roncadelli M: ar. Xiv: 0707. 2695 [astro-ph]

• Strong mixing can occur between cosmic g-ray and axions by cosmic magnetic fields Fairbairn, Rashba, Troitsky 2009 ar. Xiv 0910. 4085

– UHE gammas from QSOs and Blazers can penetrate the CMB/CIRB barrier to explain the observed flux. Expected flux from 3 C 279 Optical depth against CMB Fairbairn, Rashba, Troitsky 2009; Roncadelli, de Angelis, Mansutti 2009

中性子星，ブラックホール Crab Nebula (HST + Chandra) [Hubble. Site]

銀河中心にある巨大ブラックホール 1 kpc scale jet from M 87 [Hubble. Site]

Observatories of Extreme Physics • Gravitational Waves – – • Radio – – • Hakucho, Tenma, Ginga, Aska, Suzaku, Chandra ⇒ ? Gamma-rays – – • Ground-base telescope: Subaru(8 m) ⇒ JELT(30 m), TLT, Euro 50, … X-rays – • Ground-base VLBI/VLBA: CJF, RRFID, 2 cm Survey/MOJAVE Space VLBI : HALCA(VSOP) ⇒ VSOP-2/ASTRO-G(磁場の測定可）, RADIO Astron Optical/IR – • Ground-base Laser Interferometers: Stellar systems TAMA, LIGO, GEO, Virgo ⇒ LGCT, Adv-LIGO, LIGOII Space Laser Interferometers: ⇒ BBO: LISA, DECIGO Ground-base: CANGAROO, HESS, MAGIC ⇒ CTA Space: EGRET⇒ GLAST Cosmic Rays – – Neutrinos (Super-)KAMIOKANDE, Cascade Grande, AMANDA ⇒ CAROT, ICECube UHE CRs HALCA observations of AGASA, Hi. Resand ⇒ NGC 4261 Pierre Auger. NGC 1052

Massless Scalar Field around BH • Klein-Gordon product From the field equation the KG product defined by is independent of the choice of the Cauchy surface in DOC. • Scattering problem No incoming wave from the black hole

• Asymptotic behaviour – At infinity – At horizon where *= – m h , .

Superradiance • Flux conservation • Superradiance condition This condition is equivalent to Cf. Penrose process in the ergo region [Penrose 1969]

Black Hole Bombs • Black hole in a mirror box [Zel’dovich 1971; Press, Teukolsky 1972; Cardoso, Dias, Lemos, Yoshida 2004] • Massive bosonic fields around a black hole [Damour, Deruelle, Ruffini 1976; ] For light axions around an astrophysical black hole, an instability occurs. Its growth rate is [Zouros, Eardley 1979; Detweiler 1980] Numerical calculations show that the maximum instability is : [Furuhashi, Nambu 2004; Dolan 2007], Here note that Cf. Ad. S-Kerr black holes [Hawking, Reall 1999; Cardoso, Dias 2004; Cardoso, Dias, Yoshida 2006] Magnetic Penrose process and relativistic cosmic jets in GRB [van Putten 2000; Aguirre 2000; Nagataki, Takahashi, Mizuta, Tachiwaki 2007]

Axionic Instability of BHs • Due to the superradiance instability, black holes with a specific mass lose angular momentum resonantly.

Axionic Siren • If the angular-momentum supply by accretion is rapid enough, the system becomes a strong source of GW above the LISA bound as well as radiation if there exist strong magnetic fields. Here ² appears due to the GW emission loss and is of order 10 -7.