1. Astrophysical ZeV acceleration in the jets from an accreting blackhole
Toshi Tajima, T. Ebisuzaki, A. Mizuta
UC Irvine and RIKEN
American Physical Society, DPP
Milwaukee
Oct. 24, 2017

2. abstract
wakefield driven by large clump accreting from the MRI-disk disruption toward BH / jets
 ZeV ion acceleration and GeV/TeV electron acceleration (gamma emission) from Blazars
 gamma emissions that reflect the accretion episodes : rise time an order or 2 shorter than the interval, both proportional to the BH mass
Theory by Ebisuzaki + Tajima (2014);
Simulation (general relativistic MHD) by Mizuta (2017);
Observation by Abazajian et al. (2017):
in agreement with each other イク

3. Cosmic-rays up to ~1020eV Fermi mechanism : difficult
Hillas plot : Emax~ eBR
Cygnus A jet
(radio image)
System size > gyro radius
for Fermi
Cygnus A jet
(radio image)
1020eV
1021eV
Extra galactic origin?
GZK cutoff
Fermi mechanism :
difficult

4. Blazar Flares From its Accretion Disk
disk: MRI drives clumps, which accrete and cause large disturbances
jets : ideal theater for wakefield acceleration

5. Ebisuzaki + Tajima : Astropart. J. (2014)

6. AGN : UHECR accelarator
Intense EM pulse  Strong Alfven pulse  episodic disk disruption
( a wave along B-field line, vA  c)
>>1
nonlinear & relativistic Alfven mode
Standard-disk (Shakra & Sunyaev (1973) is assumed)
ωA>ωp
ωA<ωp
Ebisuzaki & Tajima 2014
Comprehensive understanding of accretionflows, properties of
B-field, and general relativistic effect necessary
Also GRMHD simulations of accretion flows onto BHs

7. Laser-driven Bow and Wake
(Bulanov, Esirkepov)

8. Theory of wakefield toward extreme energy
(when 1D theory applies)
In order to avoid wavebreak,
a0 < γph1/2 ,
where
γph = (ncr / ne )1/2
←theoretical
←experimental
ncr =1021
ne = 1016
dephasing length
pump depletion length

9. Luminosity and spectral index as a function of time of AOO235+164
They anti-correlate
Luminosity L
Strong accretion
 strong wakefield
Spec. Index p
strong episode for wakefield:
index p = 2,
Otherwise p > 2
(Mima et al. 1991)
 p=2

10. Magnetized jet launch (GR MHD)
~60Rg
DISK
・Stratified structure in
magnetic energy density
・Disk wind along the disk
edge
Along the polar axis
・Mass density is low
・intermittent outflow
・High Magnetic energy density

11. Outflow luminosity from GR MHD ( 0<θ<10°)
θ0=0
θ1=10
Short time variavilitry (Δt~a few tensGM/c3) in electromagnetic components
(green and pink) : Good agreement with Ebisuzaki & Tajima(2014)
=> possible origine for flares in blazars (on axis observer),
strong Alfven wave mode => Application to wake field acc. for UHECRs

12. Summary ・Cosmic rays – power law spectrum up to ~1020eV
– Astrophysical accelerator of UHECR : not Fermi (ion
synchrotron depletes ion energy); electrons( γ burst)
 wakefield (straight acceleration of ions and electrons)
(Ebisuzaki & Tajima: 2014)
・Active galactic jets (blazars) are strong candidate for above
episodic (due to MRI) variations of
luminosity L and power index p
anti-correlated time dep. of L(t) and p(t): agrees w/ theory
・ GRMHD simulations of rotating BH + accretion disk
　　 shows similar tendencies
・ gravitational emission this episodic fashion (predict)

13. Thank you!