great bu ’ s grb 2004 / 11 2 grb grb. early mission history 1960s, the vela series burst and...
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GReat Bu’s GRBGReat Bu’s GRB
2004 / 112
GRBGRB
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Early Mission Early Mission HistoryHistory
1960s, the Vela series
Burst And Transient Source Experiment (on the CGRO, launched in 1991)
BeppoSAX (launched in 1996/4/30)– provide a much more accurate location
HETE– failed in 1996
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GRB910421
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1967/7/2 the first observation1973 publish“Model burst”Distance:1)galactic disc ~102pc2)halo ~104pc3)cosmological ~Mpc
For now1)isotropic distribution2)redshift determination(~30 now)3)Angular distrubution
strong suggest a cosmological origion!!
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Z-known GRBsZ-known GRBs
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So….So….Huge energy Eiso~1051-54 erg
Rapid temporal variability on time scales of ms compact object
However, due to γ+γ e+ + e-
optical depth should be >> 1,
non-thermal spectrum optical thin
Compactness problem
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The “fire ball”The “fire ball”Large concentration of electromagnetic radiation in small region of space with small fraction of baryonsSudden release of high intensity gamma-rays produces e+e- pairs which create an opaque photon-lepton “fireball”
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The solution??The solution??The relativistic motion ( with Γ≧100 ) of the emitting region
GRB are produced when an UR energy flow is converted to radiation in an optically thin region
1~ 1,for
:effect beaming
cos1
coscos
:light of aberration
'
'
v
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GRB all starGRB all starGRB970228 Afterglow, x-ray ,optical counterpart, XT RT (a breakthrough)
GRB970508 Redshift ,absorption lines (FeII MgII), radio counterpart
GRB971214 Host galaxy
GRB980425 SN association(SN1998bw) (z=0.0085, the “closet”)
GRB990123 most energetic ( Eiso~3 X 1054erg ) optical counterpart (by ROTSE)
GRB030325 polarzation
GRB030329 SN association(SN2003dh)
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mC
Emmmm )(
2212211
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Adopt from SCIENCE@NASA
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Summary of Summary of observationobservation
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Observation (I) --Observation (I) --GRBGRB
Eiso
Burst rate
in 1991-2000 (CGRO operation period) 1/day (~1/106-7yr/galaxy)
Duration
T90:5%~95% in the 50-300keV
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Observation (II) --Observation (II) --GRBGRB
Spectrum
Non-thermal
No clear observational evidence for the existence of spectral lines
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Observation (III) -Observation (III) -afterglowafterglow
Lightcurves Well fitted by power-laws~5 GRB has line features in the early X-ray afterglow Some of them “Break” (low energy poewer index ~2)Offset from the center of the hot galaxyHost galaxy (025~Z~4.5): are typically low mass, faint galaxies (R~25) with active star formation region
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several re-brightenings, varying power law indices
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Observation (IV) Observation (IV) --afterglowafterglow
GRB/SN connection
red excess ,”SN bump”:
GRB980326, GRB011121
GRB980425 / SN1998bw : within the error box
GRB030329 / SN2003dh: very similar spectrum with that in SN1998bw case
“super” Type Ic
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Types of SNeTypes of SNeaccording to the spectrum with H = SN II without H = SN I with Si = SN Ia without Si but with He = SN Ib
without Si and without He = SN Ic
The energy source for SN Ia is nuclear; for the others is gravitational
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The lack of a measured redsiftSNIc Best fit : Z~0.95
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Spectral evolution
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Observation (V) -Observation (V) -afterglowafterglow
Polarization
MNRAS 309,L7 1999
Consider a magnetic field completelytangled in the plane of the shock front, but with a high degree of coherence in the orthogonal direction
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Γ >>1, no polarization
Γ ~ 1/(θc+ θ0)
Γ <1/(θc- θ0) see only part of the circle centred on θ0
Γ 1 light aberration vanishes,The observe magnetic field is Completed tangled and Polarization disappears
Two maxima in the polarization light curve, the first forThe horizontial component and the second for the vertical one!!
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GRB030325
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Oh , Theory Oh , Theory
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Model forestModel forestSGRs as a hint ??Relativistic dust crash energetically into the solar wind Comets falling onto NSsPrecessing jets from pulsarsCanonballs from supernovaeJet-disk in a binary systemMagnetar bubble collapseNS collapse to a strange starCollapse to a BH caused by accretionSupermassive BH formationEvaporating BHs
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The “fireball” The “fireball” againagain
GRBs occur through the dissipation of the kinetic energy of a relativistic expanding fire ball
γ-ray emission mechanisms
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The shape of The shape of thingsthings
Time variability (~milliesecond)
R~ CΓ∆T compact object
Duration 10-2s ~ 103s
Energy Eiso~1051-54 (for z-known GRBs)
Beaming
Rates , R~1/106-7yr/galaxy
if beamed…..
j
j
ddR
EE
j
isojet
0
2
0
2
sin2 ,4
R'
angle opening-half:
~2
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The internal-external The internal-external modelmodel
Time-varying outflow makes different Γ(>100) shells
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When a faster shell catch up with a slower one:
Kinetic energy internal energy (internal shock ) radiation (accelerated electrons interact with the ambient magnetic field )
internal shock GRBexternal forward shock afterglow
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The “inner The “inner engine”engine”
Binary NS merge
WD-NS , NS-BH merge
failed supernova (Collapsar)
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Collapsar Collapsar – a BH is bor– a BH is bornn
1993, by Woosley et al.
“Failed supernova”
Iron core collapse BH
MHD jet
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ApJ 524:262 1999ApJ 524:262 1999
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The jet is erupting through the surface of the star. Blue represents regions of low mass concentration, red and yellow are denser . Note the blue and red striations behind the head of the jet. These are bounded by internal shocks.
Adopted from GSFC, NASA
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Make story complete —Make story complete — asymmetric asymmetric supernova supernova
2000, by wheeler et al.
The generation of jets
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Make story more complete —Make story more complete — Wolf-Reyet starWolf-Reyet star
Wolf-Rayet stars are hot (25-50,000+ degrees K), massive stars (20+ solar mass) with a high rate of mass loss. Strong, broad emission lines (with equivalent widths up to 1000Å!) arise from the winds of material being blown off the stars. Wolf-Rayets stars are divided into 3 classes based on their spectra,
WN stars (nitrogen dominant, some carbon), WC stars (carbon dominant, no nitrogen),
WO stars with C/O < 1.
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The whole story….The whole story….To make a collapsar need three essential components:
1)Wolf-Rayet star
2)A rotating stellar core
3)A core collapse that failed to produce a successful supernova
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Summary Summary
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Conclusion Conclusion Multi-origion
MHD
Gravitational wave
Polarization
TeV photon observation
GRB 970828 no OT, “dark burst”
be obscured by dust in their host galaxy
associated with massive sar formation??
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The unified model??The unified model??astro-ph/0410728
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Reference and Special Reference and Special ThanksThanks
Many of content are adopted from “Jochen Greiner Homepage” ( http://www.mpe.mpg.de/~jcg/ )Romanian Report in Phisics, Vol.56 No.2 P204, 2004 Valeriu Tudose et al.ASTRONOMY, October 2004Others….