Gamma-Ray Bursts : :sts GeV/TeV photon emission and
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1 Gamma-Ray Bursts : :sts GeV/TeV photon emission and UHECR/UHEν Peter Mészáros Pennsylvania State University
2 GRB: (via PNS?) short long
3 GRB paradigm 3 Mészáros
4 Fireball Model of GRBs Several shocks - - also possible cross-shock IC Internal Shock Collisions betw. diff. parts of the flow External Shock Flow decelerating into the surrounding medium Reverse shock Forward shock n,p decouple Photospheric th. radiation GRB Afterglow X O R cm Mészáros
5 Standard shock γ-ray components : shock Fermi acc. of e - synchrotron and inv.compton E 2 N(E) Or? GeV νf ν Ext.Sh. Sy (reverse) 0pt Sy (forward) TeV γ ν GRB bright (9 th mag) prompt opt. transient (Akerlof etal 99). 1st 10 min: decay steeper than forw.sh. Interpreted as reverse shock But is it? Mészáros
6 BAT: Energy Range: kev FoV: 2.0 sr Burst Detection Rate: 100 bursts/yr SWIFT Three instruments Gamma-ray, X-ray and optical/uv Slew time: s! >95% of triggers yield XRT det >50% triggers yield UVOT det. XRT: Energy Range: kev Mission Operations PSU (Bristol Res. Park) UVOT: Wavelength Range: nm Launched Nov 04 Mészáros, L Aqu05
7 z=0.937 GRB B A prompt naked eye optical GRB Racusin et al, 08 Nature 455:183 γ, opt prompt l.c. appear similar same emission region, e.g. internal shock; but rad. mechanism? Interpret prompt as: i) optical synchrotron ii) MeV IC (SSC) (and) iii) predict 2nd order ~100 GeV (there are also differing opinions) Mészáros
8 080319b O/UV XR GRB B Mészáros Hei08
9 GRB B WJ Afterglow Prompt NJ Mészáros
10 080319B X-Ray 2-jet fit FS-NJ FS-WJ Mészáros Hei08
11 080319B optical 2-jet fit RS-WJ FS-WJ Mészáros Hei08
12 A different prompt: GRB060218/SN2006aj There may be more to prompt emission than high Γ shocks! An unusually long, smooth burst, T90~2100±100 s Low luminosity, low energy : Eiso~6x10 49 erg z=0.033, 2nd nearest GRB (138 Mpc) GRB/XRF Campana et al. 2006
13 A prompt X-ray BB component :...? SN Shock breakout (!) kt~0.17kev BB comp. temp. & radius Contribution of a fitted black-body component (20%) to the KeV flux: BB Interpreted as break-out of an anisotropic, semi-relativistic, radiation-mediated shock from Thomson optically thick stellar wind (Campana et al 06, Nature 442:1006; Waxman, Mészáros & Campana, 07, ApJ 667:351)
14 UHE CRs &, from GRB pγ, pp UHE, If protons present in (baryonic) jet p + Fermi accelerated (as are e - ) p,γ π ± μ ±,ν μ e ±,,ν e,ν μ (Δ-res.: E p E γ ~ 0.3 GeV 2 in jet frame) Eν,br ~ ev for MeV γs (int. shock) Eν,br ~ ev for 100 ev γs (ext. rev. sh.) : ICECUBE π 0 2γ γγ cascade : GLAST, ACTs.. Test hadronic content of jets (are they pure MHD/e ±, or baryonic?) Also (if dense): p,γ π ± μ ±,ν μ e ±,,ν e,ν μ Test acceleration physics (injection effic., ε e, ε B..) Test scattering length (magnetic inhomog. scale?..or non-fermi?..) Test shock radius: γγ cascade cut-off: E γ ~ GeV (internal shock) ; E γ ~ TeV (ext shock/igm) photon cut-off: diagnostic for int. vs. ext-rev shock
15 Fermi Also on Fermi : GBM (~BATSE range) ; 12 NaI: 10keV-3 MeV; 2 BGO: 150 kev-30 MeV Launched June LAT: Pair-conv.modules + calorimeter 20 MeV-300 GeV, ΔE/E~10%@1 GeV FoV = 2.5 sr (2xEgret), ang.res. θ~30-5 (10GeV) Sensit. ~ ph/cm 2 /s (2 yr; > 50xEgret) GBM: FoV 4π, 10keV-30MeV 2.5 ton, 518 W expect det/loc ~60 GRB/yr; simult. w. Swift : 30/yr
16 LL GRB : GeV-TeV γs arising from leptonic sy-ic origin 2 sources of hot IC e - : shocks- a: Γ~2, b: Γ~10 a) rel. jet in SS stage b) semirelat. outflow and 2 sources of seed photons: a) synchrotron (SSC) b) SN UV (SN IC), incl. early th. & late RI He, Wang, Yu & Mészáros 09 Mészáros
17 Hadronic GRB: easier to look for secondary photons from p,γ interactions Asano, Inoue & Mészáros ApJ in press, arxiv: If GRB are UHECR sources, may need εp/εe 10 tends to give identifiable hadronic photon peak Diagnostic for : high εp/εp : high bulk Γ : high εb/εe Mészáros Hei08
18 A bright LONG burst : GRB c Abdo et al. (the Fermi collaboration), 2009 Science, 323:1688 1) All spectra approximate Band functions : same mechanism? Could be Synchrotron. No obvious cutoff or a softening Γ 100; expect also SSC, but this could be > TeV, not observed Since no statistically significant higher energy component above Band, the latter must have either E TeV or Y~εe/εB 0.1 2) GeV only in 2nd pulse or later, vs. MeV (1st pulse) - Why? Could originate in different region, e.g. a 2nd set of internal shocks, with parameters or physics (possible) Or radiation from one set of shells up-scattered by another set of shells? (but no expected delay between 2nd LAT & GBM) Mészáros
19 Counts/bin Counts/bin Counts/bin NaI 4 GBM NaI 3 (8 kev-260 kev) Time since trigger (s) GBM BGO 0 (260 kev-5 MeV) 54.7 Counts/bin a b c d e LAT (no selection) Counts/bin Counts/bin Time since trigger (s) Time since trigger (s) Counts/sec Counts/sec Counts/sec GRB c Abdo, A. and Fermi coll., 09, Sci. 323:1688 Light-curve E 0 0 Counts/bin Counts/bin LAT (> 100 MeV) Time since trigger (s) LAT (> 1 GeV) Time since trigger (s) Counts/bin Counts/bin Time since trigger (s) Counts/sec Counts/sec Notice : GeV photons lag behind MeV! Mészáros
20 GRB C Spectrum Band fits (joint GBM/LAT) for all the different time intervals Soft-to-hard, to sort-of-softpeak-but-hardslope afterglow No evidence for 2nd component Mészáros
21 GRB c (the Fermi collaboration, 2009) 3) GeV only in 2nd pulse or later, vs. MeV (1st pulse) - Why? Hadronic? (the burning question)... natural delay since extra time for cascade to develop - but : expect hard to soft time evolution & distinct sp. component - not seen) Upshot: more analysis needed to test hadronic model and/or constrain variant of leptonic model Future Fermi+Swift+ground observations will tell Mészáros
22 GRB Fermi LAT/GBM identified SHORT burst Shows (sim. to long bursts) time LAG between soft 1st pulse and hard 2nd pulse Shows an EXTRA spectral component, besides usual Band component (first clear!) Hadronic? Maybe... Mészáros
23 GRB Spectrum: clear 2nd comp (5σ) Abdo, et al. 09 (LAT/GBM coll.) Nature, subm. arxiv/ Mészáros
24 ε!"ε#$%&'()*+, ) C 34 5D Hadronic model: )0 γ <8=>$?:+@> 0 1 )0 γ 234 5A ε 53>B Asano, Guierec, Mészáros, 09 (ApJL, arxiv ) Secondaries from photomeson cascades (but: need Lp,iso~10 55 erg/s!) 34 5B ε ν & ν 'ε ν (!"#)*+,-. +/% 678*9':;':8 34 5E 34 C 34 D 34 B 34 E 34 F 34 G Secondary photons ε$%&/. Secondary neutrinos (not detectable, for this burst) >? 4A 869)!:6/,65# #, #,67 8)2;23!<73,=)2;)23 >? 4B >? 4C >? >@ >? >A >? >B >? >C >? >D ε ν!"#$% Mészáros
25 (Granot, Venice09) Mészáros
26 Mészáros
27 Fermi LAT/GBM results (10/9/09) Mészáros
28 UHE neutrinos from GRB p,γ π ± μ ±,ν μ e ±,,ν e,ν μ Need baryon-loaded relativistic outflow Need to accelerate protons (as well as e - ) Need target photons or nuclei with τ 1 (generally within GRB itself or environment) Need Erel,p Erel,e Might hope to detect individual GRB if nearby (z 0.15), or else cumul. background 28
29 1 e - capt p,n 2 UHE ν in GRB Various collapsar GRB ν-sites 1) at collapse, similarly to supernova core collapse, make GW + thermal ν (MeV) 3 pγ, pp pγ 2) If jet outflow is baryonic, have p,n p,n relative drift, pp/pn collisions inelastic nuclear collisions VHE ν (GeV) 3 Int. shocks while jet is inside star, accel. protons pγ, pp/pn collisions UHE ν (TeV) 4) internal shocks below jet photosphere, accel. protons pγ, pp/pn collisions UHE ν (TeV) 5) Internal shocks outside star accel. protons pγ collisions UHE ν (100 TeV) 6) External rev. shock: pγ EeV ν (10 18 ev)
30 Hadronic GRB Fireballs: Thermal p,n decoupling VHE ν, γ Bahcall & Meszaros 2000 Radiation pressure acts on e -, with p + coming along (charge neutrality) The n scatter inelastically with p + The p,n initially expand together, while tpn <texp (p,n inelastic) When tpn ~texp p,n decouple At same time, vrel 0.5c p,n becomes inelastic π + Decoupling important when Γ 400, resulting in Γp >Γn Decay ν, of Eν GeV Motivation for DEEP-CORE!
31 While jet is inside progenitor: Meszaros & Waxman 01 Mészáros pan05
32 GRB : precursor (& pre-sn shell?) with ICECUBE Burst of Lγ~10 51 erg/s, E SN ~ z~0.17, θ~68 o Flux of n Razzaque, Mészáros, Waxman 03 PRD 69, Mészáros pan05
33 Internal shock ν s, contemp. with γ s Detailed νµ diffuse flux incl. cooling, using GEANT4 sim., integrate up to z=7, Up/Uγ=10 (left) ; z=20, Up/Uγ=100 (right) Asano 05, ApJ 623:967; Murase & Nagataki 06, PRD 73:
34 GRB Photospheric Neutrinos GRB relativistic outflows have a Thomson scattering τt~1 photosphere, below which photons are quasi-thermal Shocks and dissipation can occur below photosphere. Acceleration of protons occurs, followed by pp and pγ interactions neutrinos Gas and photon target density higher than in shocks further out. Characteristics resemble precursor neutrino bursts, but contemporan. with prompt gamma-rays Wang, Dai Murase
35 A different magnetar signature : Magnetar birth ν-alert? Murase, Mészáros & Zhang, PRD 09 ; arxiv: Magnetars (B~ G) may result from turbulent dynamo when born with fast (ms) rotation A fraction 0.1 of CC SNe may result in magnetars In PNS wind, wake-field acceleration can lead to UHECR energies E(t) ev Z η-1 μ33-1 t4-1 Surrounding ejecta provides cold proton targets for pp π ± ν ν-fluence during time tint first increases (strong initial π/μ cooling), then decreases (with the proton flux) Mészáros
36 Magnetar birth ν-alert Murase, Mészáros & Zhang 09 Magnetar D=5 Mpc Light curve - Can signal birth of magnetar - Test UHECR acc. in magnetar -BUT: Not an explanation for Auger, because a) UHECR flux not sufficient, and b) UHECR spectrum not like Auger obs. Diffuse flux Mészáros
37 EHE ν s Neutrino fluxes; Asano et al, 09, arxiv: JEM-EUSO sens.: M. Teshima, MPI Crucial parameter for neutrino (and CR) flux is Up/Ee. Note that ν s from pion decay are good targets too (not just muon decay) For typical values Up/Ee ~ 30 needed to make GRB interesting UHECR sources, the neutrino flux might be detectable from individual GRB sources at z~0.1 with 37 JEM- EUSO (K. Asano et al, 2008, in prep.)
38 AUGER result: UHECR spatial correlations with AGN/LSS Science Nov 2007 Dashed line: supergalactic equator Circles (proton): Events E>4.5x10 19 ev Crosses: Veron-Cety catalog AGNs
39 Auger spatial correlation Found 3σ corr. with V.C. AGNs within 3.5 deg inside 75 Mpc, for 28 events E>4.5x10 19 ev The above correlation suggest protons Science, 07 But cannot say positively it is AGNs - could be correl. with underlying LSS Kashti-Waxman confirm correl. with LSS at >98% confidence level, via two-pt corr., ang. power spectr. and predicted-observed coincid. If heavy mix: many more gals. inside each event s larger angular spread. But: AGN significance now (09) weakened to 1.7 σ 39
40 CR Flux & spectrum - GRB [Waxman 95] Mészáros grb-glast06
41 GZK CR Sources Sources: GRB ; AGN... #? Rate: R GRB (z=0)~ 0.5 Gpc -3 yr -1 ~ (D/100 Mpc) -3 yr -1 But, arrival time dispersion: t dis ~ 10 7 yr (B/10-8 G) 2 (λ B /1 Mpc) (D/100MPC) 2 (E p /10 20 ev) -2 N GRB (E>E p, D<D GZK ) ~ R. t disp ~ 10 4 B 2-8 λ B,0 D E 2 p20 GZK event rate: ~ 1 /Km 2 /100 yr [Waxman 95, 2005] Mészáros grb-glast06
42 UHECR data vs. GRB model Waxman 06
43 What about Eν ev? 2 CR models same GZK CR fit from GZK CRs to GZK νs But lead to GZK ν flux Can infer GZK CR injection spectrum and/or source cosm. luminosity evolution via their GZK νs. Seckel & Stanev astroph/
44 GRB GZK cosmogenic neutrinos Yuksel & Kistler 07 PRD 75: If GRB make the GZK UHECR, then: ν flux dep. on GRB rate vs. z (from z>> RGZK ) 44 Yuksel et al, 2007
45 Potential of Cosmogenic νs for CR Composition If CRs have large fraction of heavies, depending on source distance, photodissociation opt. depth could be <1 only some of them break up into p,n Implies smaller fraction contributes to π + and cosmogenic ν production (Anchordoqui et al 06) Cosmogenic ν flux vs. CR flux may help resolve discrepancy between Auger Xmax data and apparent correlation with AGN suggesting protons 45
46 Conclusions Much new information about GRB in the VHE range from Fermi They are likely sources of UHECR and UHENU, but still unknown Will learn much about best UHECR/UHENU candidates (GRB, AGN, MGR?) from GeV and TeV photon observations with good statistics TeV gamma obs. Fermi: (a) Second spectral component found; (b) HE emission SGRB ~ LGRB, (c) MQG > MPlanck for n=1, need n 2 Will constrain particle acceleration / shock parameters, compactness of emission region (dimension, mag.field,.) UHECR : chemical composition, angular correl.: sources? UHE ν will allow test of proton content of jets, proton injection fraction, test shock acceleration physics, magn. field If UHE ν NOT detected in GRB jets are Poynting dominated! Probe ν interactions at ~ TeV CM energies Constraints on stellar birth & death high-z, first structures? Cosmogenic nus: probe CR origins, sources
47 Back-up slides
48 Origin of ev UHECR: may be GRB - but what about ev? Radio, x-ray & gamma-ray observations of SN1998bw/GRB sub-energetic GRB GRB980425: E~1e48 erg (d=38 Mpc) Radio afterglow modeling: E>1e49 erg, \Gamma~1-2 X-ray afterglow: E~5e49 erg, \beta=0.8 Mildly relativistic ejecta component E_SN=3-5e52 erg V=0.1c S N SN shock acceleration in the Envelope? Tan et al. 01 Woosley et al. 99 Other SN/GRB w. semi-relativistic ejecta: SN2003lw/GRB SN2006aj/GRB060218
49 The maximum energy of accelerated particles 1) Type Ib/c hypernovae expanding into the stellar wind of Wolf-Rayet star 2) equipartition magnetic field B, both upstream and downstream Maximum energy: Hillas 84, Bell & Lucek 2001 Protons can be accelerated to ~10 19 ev Heavy nuclei can be accelerated to ~Z*10 19 ev
50 Flux level--- energetics Kinetic energy generation rate: Compare w. normal GRBs The required rate : Rate (z=0) kinetice nergy Hypernova (v=0.1c) ~500 ~1 Normal Ib/c SN rate: Normal GRBs 3-5e52 erg 1e53-1e54erg sub-energetic GRB rate: Soderberg et al. 06
51 Energy distribution with velocity Data from Soderberg et al. 06 Normal SN Very steep distribution -> negligible contribution to high-energy CRs Berezhko & Volk 04 Semi-relativistic hypernova: high velocity ejecta with significant energy is essential Wang, Razzaque, Meszaros, Dai 07 CR spectrum:
52 Transition from GCRs to EGCRs
53 Semi-relat. ( slow ) jets in core-collapse SN? Maybe all core coll. (II or Ib/c) SN resemble (watered-down) GRB? Evidence for asymmetric expansion of c.c. (Ib/c) SNR: - asymmetric remnants - optical polarization - jets may help eject envelope slow jets Γ~ few? Mészáros TeV05
54 Core collapse SN : slow jets? Spectrum and diffuse flux Razzaque, Mészáros, Waxman, 2004, PRL 93, Ando & Beacom, 2005, PRL 95, 1103 Maybe all core coll. (or Ib/c) SN resemble (watered-down) GRB? Evidence for asymmetric expansion of c.c. (Ib/c) SNR: slow jets Γ~ few? If so, accel protons while jet inside star, pγ π,μ ν (TeV) Diffuse flux: negligible, but individual SN in nearby (2-3 Mpc) gals, e.g. M82, NGC253, detectable (if have slow jets), at a rate ~ 1 SN/5 yr, fluence ~2 up-muons/sn (hypernova: 1/50 yr, 20 up-μ), negligible background, in km 3 detectors - ICECUBE
55 LIV limits GRB C Fermi collaboration (Abdo et al), 2009, Sci.. 1st and 2nd order (n=1,2) energy dependent pulse time dispersion in effective field theory formulation of LIV effects, where leading order deviation is E 2 - p 2 - m 2 ± E 2 (E/EQG) n Conservative lower limit on EQG, taking Eh/t (Eh/t 1/2 ) with t=pulse time since trigger These are (almost) the most stringent limits to-date via dispersion Mészáros
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