7-1yamazaki.pptx
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- なごみ えいさか
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1
2 Suzaku/ASTRO-H Suzaku/ASTRO-H
3 1. Vela ( Watchman ) ( ): GRB (1969) 2. GINGA ( ): X-ray counterpart GRB (galactic) X-ray burst? 3. BATSE ( ): Galactic origin models!!! 4. BeppoSAX ( ): X-ray (optical) afterglow cosmological distance!!! 5. HETE-2 (2000 ): long GRB/SN association 6. Swift (2004 ) high-z GRB (z > 6) => 7. Fermi (2008~) : GeV GRB
4 (=>calorimetry) VLA (redshift, localization, jet structure) (localization, jet structure) Swift/XRT available. *10keV-MeV GeV (jet speed, radiation mechanism, CR) Fermi 7events/yr TeV (radiation mechanism, CR) CTA events/yr.
5 GRB research in the Fermi era GRB GeV (1) Γ (2) GRB (~MeV ) (synchrotron or SSC?) (3) GRB Γ=300 Γ=1000 2ndary e ± (pγ π ± e ± ) Γ=100 Asano, Inoue primary e -
6 GRB research in the Fermi era GRB GeV (1) Γ (2) GRB (~MeV ) (synchrotron or SSC?) (3) GRB Γ=300 Γ=1000 2ndary e ± (pγ π ± e ± ) Γ=100 Asano, Inoue primary e -
7 GRB research in the Fermi era GRB GeV (1) Γ (2) GRB (~MeV ) (synchrotron or SSC?) (3) GRB Γ=300 Γ=1000 2ndary e ± (pγ π ± e ± ) Γ=100 Swift WAM LAT Swift WAM primary e - LAT
8 Fermi LAT detection of GRB C First GeV γ detection of a GRB with known redshift. * High-z, bright event: z = 4.35±0.15 E iso (10keV-10GeV) = 8.8x10 55 erg ~ 5 M sun c 2 => Jet collimation * GeV photons avoiding pair-creation annihilation => Relativistic motion: Γ > 890±20 (bin b ) Fermi LAT collaboration (2009)
9 Fermi GeV GRBs GeV delay (delay ) (leptonic model) IC emission? (Hadronic model) proton acceleration time? GeV lepton proton proton
10
11 Ahlers UHECRs in internal shocks of GRBs In internal shock, P 10^ γ GRB => π 0, π +, n UHECRs γ, e +/- : => GeV gamma s (1) Hires Fermi diffuse gamma IcuCube (γ, E max ) N(E) E γ exp ( E / E max ) β n => p + e - + ν e UHECRs UHE-Nu s CMB => GeV gamma s (2), UHE-Nu s(gzk-nu)
12 (GRB rate) SFR (GRB rate) SFR x (1+z) 1.4 GeV Gamma s (1),(2) GeV Gamma s (2) GeV Gamma UHECRs Fermi diffuse gamma
13 (GRB rate) SFR (GRB rate) SFR x (1+z) 1.4 GeV Gamma s (1),(2) GeV Gamma s (2) GeV Gamma UHECRs Fermi diffuse gamma
14 Ahlers GRB Internal shock UHECRs UHECR flux UHECR (γ<2.1) ev UHECR ev Fermi Diffuse gamma
15 Neutrino upper limit from IceCube GRB IceCube: Abbasi+2011
16 Neutrino upper limit from IceCube GRB Waxman GRB photon spectrum Guetta IceCube: Abbasi+2011
17 Neutrino upper limit from IceCube GRB AMANDA IceCube (40strings) IceCube (22strings) Waxman GRB photon spectrum Guetta IceCube: Abbasi+2011
18 Waxman Bahcall (upper) bound CR proton ν µ p+p or p+γ => π + or π - => ν µ or ν µ CR proton ( GeV/cm 2 /s/sr ) energy production rate (n p CR E p -2 ) factor 0.25 = 0.5 ( = loss via π 0 production) x 0.5 ( = E ν /E π ) t H : Hubble time (CR proton ) ξ Z ~1 : redshift evolution & energy loss
19 Waxman Bahcall (upper) bound CR proton WB bound τ (source size) / (CR proton m.f.p.) τ 1 WB bound τ < 1 WB bound (e.g. : τ << 1 for GRB external shocks, Galactic SNRs ) τ > 1 CR proton WB bound => IceCube
20 GRB? Short GRB = Soft gamma-ray repeater giant flare? NS-NS merger UV and localized region
21 Fermi(Ext.Gal.Diffuse GeV), Icecube( ), LIGO( )
22 GRB is a relativistic version of SNR (Piran99) particle acceleration *internal-external shock model, *models of jet dynamics, jet emission, polarization, external compton, *<V/Vmax> of QSOs, * particle acceleration
23
24 2000 X-ray flash γ (Heise et al. 2001) (in t Zand et al. 1999)
25 Spectral properties of XRFs and GRBs Ep=19 kev Ep=126 kev Kippen et al. 02 Barraud et al. 03 Photon indices α, β ( ) GRB XRF XRF Ep (peak energy) GRB
26 Motivation : AGN X- ray flash GRB
27 X-ray flash 1 XRF/XRR classical GRB by HETE-2 XRF/XRR GRB GRB viewing angle, gamma factor, Lamb et al. (2003)
28 Theoretical Models of the X-ray flash
29 X-ray flash X-ray flash Amati relation low-energy (by HETE-2) Amati relation Yonetoku, Ghirlanda,Tsutsui relations Ep Sakamoto, RY+08 X-ray flash
30 Relativistic beaming and Doppler effects 1/γ v = 0 (matter comoving frame) v (observer frame) γ (1 β ) v/c
31 ff-axis Jet Model of XRFs
32 Off-axis model Ep E iso : detected by HETE (on-axis) : detected by HETE (off-axis) : not detected by HETE
33 Off-axis afterglow Granot On-axis Off-axis Observed light curves have a rising part at days.
34 2004 Swift Swift ( ~)
35 X-ray/Optical Ghisellini+
36 2005 Swift X-ray flash/x-ray rich GRB off-axis model Sakamoto, RY+ (08) XRF: Ep < 100 kev XRR: Ep = keV GRB: Ep > 300keV
37 Off- axis model rising part Guidorzi+09 XRF XRF XRF Kruhler+07 de Ugarte Pos<go+07
38 GRB Kruhler et al T90(15-350keV) = 120s, Gamma= (BAT) (Ep = kev) S(25-50keV)/S(50-100keV) = / classical GRB z = => Ep (1+z) 200keV log(eiso) =
39 GRB = on-axis prompt & off-axis afterglow? (a) (b) (c) prompt prompt prompt prompt: GRB(on-axis), AG: on-axis prompt: XRF(off-axis), AG: on-axis Prompt: XRF(off-axis), AG: off-axis (a) GRB (a) (b), (c) (c) 1 (b) Prompt
40 GRB off-axis emission Fermi AGN( ) Cygnus A (700 )
41 Prompt 1 1. Jets-in-a-jet: magnetic reconnection in prompt Blazer TeV prompt
42
43 Prompt 2 2. Bent jet, (like AGN; Fermi/KANATA 2010): * collision with stars or MCs? prompt * current driven kink, KH insta. prompt
44 Prompt 3 3. Inhomogeneous prompt efficiency of mini-jets. -high efficiency jets: little energy after prompt -low efficiency jets: little dissipative in prompt
45 Summary GRB GRB X-ray flash off-axis jet model Off-axis jet *prompt jets-in-a-jet, bent jet, inhomogeneous efficiency
Akira MIZUTA(KEK) AM, Nagataki, Aoi (ApJ, , 2011) AM + (in prep)
Akira MIZUTA(KEK) AM, Nagataki, Aoi (ApJ, 732 26, 2011) AM + (in prep) 2011.12.28 GRB GRB. ex. GRB980425/SN1998bw, GRB030329/SN2003dh XRF060218/SN2006aj. GRB091127/SN2009nz XRF100316D/SN2010bh Spectrum
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TKK の物理的可能性 an extension of the TK neutrino oscillation experiment with a far detector in Korea 岡村直利 ( 京大 基研 ) 関西セミナーハウス (007/03/7( 007/03/7) based on hep-ph/050406 [Phys.Lett.B637,66 (006)] hep-ph/060755
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Based on N. Nagata, S. Shirai, JHEP 1403 (2014) 049. Ø Ø Y. Okada, M. Yamaguchi, T. Yanagida (1991), H. E. Haber, R. Hempfling (1991) J. R. Ellis, G. Ridolfi, F. Zwirner (1991) Scalar Par cles Gravi no
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![(Compton Scattering) Beaming 1 exp [i (k x ωt)] k λ k = 2π/λ ω = 2πν k = ω/c k x ωt ( ω ) k α c, k k x ωt η αβ k α x β diag( + ++) x β = (ct, x) O O x](/thumbs/104/162595168.jpg "(Compton Scattering) Beaming 1 exp [i (k x ωt)] k λ k = 2π/λ ω = 2πν k = ω/c k x ωt ( ω ) k α c, k k x ωt η αβ k α x β diag( + ++) x β = (ct, x) O O x")
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