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 :after a few days ~ after a month from the burst power law : afterglow time Explosion energy Mazzali et al. (2006) SN component appears Progenitor mass GRB λ(a)
Spectrum of GRB prompt emission Band function: Broken power-law α~ -1 E α+2 E 3 E β+2 Planckian GRB090902B Abdo+(20009) GeV component GRB990123 Briggs et al. (1999) 1 (T obs =T local Γ=const) Spectrum fitting function Band function (Band et al. 1993)
1 Planck GRB090902B
GRB090902B (Ryde + 2011) 1 Planck GRB
GRB090926B (Planck like) Planck MAXI Fermi/GBM Rayleigh-Jeans tail? Serino et al. (2011)
Photospheric + Monte Carlo simulation (photon transport) Pe'er (2008, 2011),Beloborodov(2010) τ Lazatti +(2009,2011) Nagakura + (2011) Mizuta+ (2011) Non-thermal Particle injection Beloborodov(2010) Pe'er (2011)
Lj=5.e50 erg/s [0:100s] Opening angle 10 degrees Γ 0 =5, ε 0 /c 2 =80 (h 0 ~106) Γ_max~h 0 Γ 0 (Bernoulli's principle) 2D (r x θ) axisymmetric, progenitor 14_sum,R*=4.e10cm (Woosley & Heger (2006)) + wind (r>r*) ρ r -2 2D-rela- hydro code(constant specific heat ratio=4/3) Mizuta et al. (2004,2006) + MPI
Lj=5.e50 erg/s [0:100s] Opening angle 10 degrees Γ 0 =5, ε 0 /c 2 =80 (h 0 ~106) Γ_max~h 0 Γ 0 (Bernoulli's principle) 2D (r x θ) axisymmetric, progenitor 14_sum,R*=4.e10cm (Woosley & Heger (2006)) + wind (r>r*) ρ r -2 2D-rela- hydro code(constant specific heat ratio=4/3) Mizuta et al. (2004,2006) + MPI
log10(ρ/cm^3) Backflow Shock-break Interaction between jet and progenitor envelopes. Γ internal shocks High pressure cocoon confinement and a bent backflow enhance the appearance of internal oblique shocks. The jet includes knotty structure. AM, Kino, Nagakura('10)
log10(ρ/cm^3) progenitor Expanding cocoon Expanding envelopes After shock-break I r~10^11cm 10 Γ jet
log10(ρ/cm^3) After shock-break II r~10^12 cm Free expanding region ~500 (=Γ0*h0=533) Γ Recollimation shock Bubble dissipated dissipated region // z Free expanding region // Cold Bullet free expansion no dissiparion
1/beaming factor ~ 1/Γ (for β // n: LOS) θ 0 θ 5 θ 10
Light curve Dissipated region Free expanding region Γ Bullet dissipated Duration of light curve ~ jet injection. A few seconds time variability in early phase caused by internal discontinuity in the jet.
Duration / initial half opening angle θ0=10degrees 100s injection θ0=10degrees 30s injection Γ Cold Bullet free expandion Γ θ0=5degrees 100s injection Θ0=5 degrees 30s injection Γ Cold Bullet free expansion Γ
OA10 [0:100s] Light curves OA10 [0:30s] 100s Off-axsi OA05 [0:100s] OA5 [0:30s]
Lj=5.e50 erg/s [0:100/30s] Opening angle 10/5 degrees Γ 0 =100, h 0 ~5.3@r min =10 9 cm Γ_max~h 0 Γ 0 (fixed) θ0=10degrees 100s injection θ0=10degrees 30s injection θ0=5degrees 100s injection θ0=5degrees 30s injection much narrower structure
Light curves OA10 [0:100s] OA5 [0:30s] OA05 [0:100s]
Spectrum by numerical hydrodynamics Index~1(a=-1) IC index~2.5 (a=-2.5) Rayleigh-Jeans tail? GRB090926B θ0=10degrees 100s injection
Numerical Amati Relation GRB z>1 E iso Ep 2 Amati (Amati 2002,2006)
Numerical Yonetoku Relation is also found!! L iso_p E p 2 Yonetoku et al. 2004
dissipated region ( x 10 ) // for on-axis observer Free expanding // for off-axis observer Summary Spectrum off axis Planck like Band like) Numerical Amati and Yonetoku relations (