photospheric emission from structured jet hirotaka ito collaborators shigehiro nagataki yitp @...
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![Page 1: Photospheric emission from Structured Jet Hirotaka Ito Collaborators Shigehiro Nagataki YITP @ YITP Lunch Seminar 2012 5/30 Shoichi Yamada Waseda University](https://reader030.vdocuments.site/reader030/viewer/2022032702/56649f435503460f94c62cff/html5/thumbnails/1.jpg)
Photospheric emission from Structured Jet
Hirotaka Ito
Collaborators
Shigehiro Nagataki YITP
@ YITP Lunch Seminar 2012 5/30
Shoichi Yamada Waseda University
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Gamma-Ray Burst (GRB)
・ duration
T ~ 10ms ー 100s
・ rapid variability
δt ~ ms
Most luminous explosion in the universe
Lγ,iso ~ 1052 erg/s
Time (s)
Co
un
ts/s
・ event rate
~1000/yr
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Briggs + 1999
<α>~ -0.9
β~ -2.5
νν^(-0.5)
Band function
< Ep > ~ 160 keV
< Ep > ~ 490 keV
Long GRB
Short GRB
α~ -1
<α>~ -0.5
<β>~ -2.3Nava + 2011
Fν ν∝ -α ( hν< Ep )Fν ν∝ -β ( hν> Ep )
Prompt Emission Spectrum
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Model for Emission Mechanism Internal Shock Model
Photospheric Emission Model
photosphere Internal shockExternal shock
γ γ
・ Low efficiency for gamma-ray production
・ too hard spectrum in low energy band (α)
GRB090902B
(e.g., Rees & Meszaros 2005, Pe’er et al.2005, Thompson 2007)
flaw
![Page 5: Photospheric emission from Structured Jet Hirotaka Ito Collaborators Shigehiro Nagataki YITP @ YITP Lunch Seminar 2012 5/30 Shoichi Yamada Waseda University](https://reader030.vdocuments.site/reader030/viewer/2022032702/56649f435503460f94c62cff/html5/thumbnails/5.jpg)
photosphere Internal shockExternal shock
γ γ
低エネルギースペクトルを説明(e.g., Rees & Meszaros 2005, Pe’er et al.2005, Thompson 2007)
flaw: high energy non-thermal tail( β)
Model for Emission Mechanism Internal Shock Model
Photospheric Emission Model
・ Low efficiency for gamma-ray production
・ too hard spectrum in low energy band (α)flaw
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Spine-Sheath jet
Spine
τ~1
0 >> 1
1 >> 1
Present Study
Sheath
Photosphere
0 > 1
Photon acceleration in a structured jet as a mechanism for production of non-thermal tail
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Spine
τ~1
0 >> 1
1 >> 1
Photons gain energy by crossing the boundary layer
Sheath
PhotosphereAccleration region
We solve the propagation of photons within the spine sheath jet
0 > 1
Present StudyPhoton acceleration in a structured jet as a mechanism for
production of non-thermal tail
Spine-Sheath jet
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r
Spine (θ<θ0 ) Sheath (θ0<θ<θj )
Calculation Range
rin << Rph
rout = 500Rph(τ~2×10-3)
rin (τ>>1)
rout (τ<<1)
Model
:photospheric radius
VelocitySpine-Sheath
Electron number density
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r
Spine (θ<θ0 ) Sheath (θ0<θ<θj )
Initial Condition
Inject thermal photons at the inner boundary
rin (τ>>1)
rout (τ<<1)
Model
Lin = 5.4×1052 r82/3400
8/3 L531/3 (rin/1011cm)-2/3 erg/s
Tin = 0.9 r81/6400
8/3 L53-5/12 (rin/1011cm)-2/3 keV
Propagation of photons are solved by Monte=Carlo method
VelocitySpine-Sheath
Electron number density
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Emax = 0mec2
Klein-Nishina cut-off
Spine
Sheath
Thermal + non-thermal tail
Result0=400j =1°0=0.5°obs=0.3°
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Comparison with Band function
β= -2.3α= -1
Structured jet model can reproduce Band function
α
β
-2.3
-1
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Summary
Structured jet can natural produce a power-law non-thermal tail above the peak energy
-
- Band Spectrum can be reproduced
Futrure works
・ Evaluation of the polarization
・ Photon accelerations in various structures
・ Hydrodymical simulation of relativistic jet as a background fluid
multi-component, shocks, turbulence