Studies of Gamma-Ray Bursts in the Swift era D a∠lga0 Department of Astronomy, Nanjing University 物理年会,北京,09/162006
Studies of Gamma-Ray Bursts in the Swift Era Dai Zigao Department of Astronomy, Nanjing University 物理年会，北京，09/16/2006
30000 20000 10000 Ime in seconds
Gamma-Ray Bursts T 600FTTTVTTTTTTTTTT 3B910507 3B90523 910717-16386 0a7911 1000 00 0005 5001000 n03 002}910430461721 0591050325454 40 Tu 十 0.003 50010002000500010000 02904n 2000 0.007 0sE91081469275 0.1 20 30 002E⊥⊥⊥ 020050010020000001000 Time since GRB-Trigger (s) 张盘/ke Temporal features: diverse and ectral features: broken power laws iky light curves with e of a few tens to hundreds of ke v
Spectral features: broken power laws with Ep of a few tens to hundreds of keV Temporal features: diverse and spiky light curves. Gamma-Ray Bursts
Bimodal distribution in durations 100g ◇ BATSE ◇ ■SAX ◇ 8088 10 ◇◇ 象8 88 ◇ ◇ ◇◇ ◇◇ 0: 8◇ ◇ 8 ◇ ◇◇■ shor long 2 01 001 01 90%Width 100 1000
Bimodal distribution in durations shor t long 2 s
Outline Pre-Swift progress lI. Recent progress and implications GRB cosmology
Outline I. Pre-Swift progress II. Recent progress and implications III. GRB cosmology
Most important discoveries in the pre-Swift era >1967: Klebesadelet al 's discovery >1992: spatial distribution(BATSE) >1997: observations on multiwavelength the redshift of GRB970508(BeppoSAy'of afterglows of GRB970228 and detection >1998 association of grb980425 with SN1998bw(BeppoSAX >2003: association of grbo30329 with SN2003dh (HETE-2)
Most important discoveries in the pre-Swift era ➢ 1967: Klebesadel et al.’s discovery ➢ 1992: spatial distribution (BATSE) ➢ 1997: observations on multiwavelength afterglows of GRB970228 and detection of the redshift of GRB970508 (BeppoSAX) ➢ 1998: association of GRB980425 with SN1998bw(BeppoSAX) ➢ 2003: association of GRB030329 with SN2003dh(HETE-2)
Some important discoveries in the pre-Swiftera > 1993: sub-classes(Kouveliotou et al.) >1994: MeV-GeV emission from GRB 940217 (Hurley et al ) 200 MeVemission from GRB 941017(Gonzalezet al 2003) 1997: detection of the iron lines in the X-ray afterglow of GRB 970508( Piro et al.) > 1999: optical flash and broken ligh curve of the r-band afterglow of Grb 990123(Akerlofet al fruchter et al. Kulkarniet al > 2002: X-ray flashes(Heiseet al Kippen et al.) > 2005: X-ray flares of GRBs(Piro et al.)
Some important discoveries in the pre-Swift era ➢ 1993: sub-classes (Kouveliotou et al.) ➢ 1994: MeV-GeV emission from GRB 940217 (Hurley et al.)； 200 MeV emission from GRB 941017 (Gonzalez et al. 2003) ➢ 1997: detection of the iron lines in the X-ray afterglow of GRB 970508 (Piro et al.) ➢ 1999: optical flash and broken ligh curve of the R-band afterglow of GRB 990123 (Akerlof et al.; Fruchter et al.; Kulkarni et al.) ➢ 2002: X-ray flashes (Heise et al.; Kippen et al.) ➢ 2005: X-ray flares of GRBs (Piro et al.)
Theoretical progress in the pre-Swift era >1975: UsoV chibison proposed GRBs at cosmological distances Ruderman discussed an optical depth >>1 problem >1986: Paczynski& Goodman proposed the fireball model of cosmological Grbs 1989: Eichler et al. proposed the ns- ns merger model >1990: Shemi Piran proposed the relativistic fireball model to solve the optical depth problem Usov and duncan Thompson proposed the magnetar model RBs 1992: Rees Meszaros proposed the external shock model of grb >1993: Woosley proposed the collapsar model >1994: Paczynski& Xu and Rees Meszaros proposed the internal shock model of GRBs; Katz predicted afterglows from GRBs >1995: Sari Piran analyzed the dynamics of forward-reverse shocks; Waxman fo Vietri discussed high-E cosmicrays from GRBs 1997: Waxman bahcall discussed high-E neutrinos from GRbs
Theoretical progress in the pre-Swift era ➢ 1975: Usov & Chibison proposed GRBs at cosmological distances; Ruderman discussed an optical depth >> 1 problem ➢ 1986: Paczynski & Goodman proposed the fireball model of cosmological GRBs ➢ 1989: Eichler et al. proposed the NS-NS merger model ➢ 1990: Shemi & Piran proposed the relativistic fireball model to solve the optical depth problem ➢ 1992: Rees & Meszaros proposed the external shock model of GRBs; Usov and Duncan & Thompson proposed the magnetar model ➢ 1993: Woosley proposed the collapsar model ➢ 1994: Paczynski & Xu and Rees & Meszaros proposed the internal shock model of GRBs; Katz predicted afterglows from GRBs ➢ 1995: Sari & Piran analyzed the dynamics of forward-reverse shocks； Waxman和Vietri discussed high-E cosmic rays from GRBs ➢ 1997: Waxman & Bahcall discussed high-E neutrinos from GRBs
> 1997: Meszaros Rees predicted light curves of afterglows >1998: Sari, Piran narayan established standard afterglow model; Vietri& Stella proposed the supranova model; Paczynski proposed the hypernova model; Dai& Lu and rees meszaros proposed energy injection models Dai Lu and meszaroset al proposed the wind model Wei& Lu discussed the Ic scattering in afterglows > 1999: Rhoads and Sariet al proposed the jet model; Sari& Piran explained the optical flash from GRB 990123 Dai&Lupr。 posed dense environments—GMC; Huanget al. established the genericdynamic model Mac et al. numerically simulated the collapsar model; Derishevet al proposed the neutron effect in afterglows > 2000: some correlations were found, e. g, Fenimoreet al and norriset al; Kumar Panaitescu proposed the curvature effect in afterglows
➢ 1997: Meszaros & Rees predicted light curves of afterglows ➢ 1998: Sari,Piran & Narayan established standard afterglow model; Vietri & Stella proposed the supranova model; Paczynski proposed the hypernova model; Dai & Lu and Rees & Meszaros proposed energy injection models; Dai & Lu and Meszaros et al. proposed the wind model; Wei & Lu discussed the IC scattering in afterglows； ➢ 1999: Rhoads and Sari et al. proposed the jet model; Sari & Piran explained the optical flash from GRB 990123; Dai & Lu proposed dense environments —— GMC； Huang et al. established the generic dynamic model; MacFadyen et al. numerically simulated the collapsar model; Derishev et al. proposed the neutron effect in afterglows ➢ 2000: some correlations were found, e.g., Fenimore et al. and Norris et al. ；Kumar & Panaitescu proposed the curvature effect in afterglows
2001: Frailet al found a cluster of the jet-collimated energies; Panaitescu Kumar fitted the afterglow data and obtained the model parameters >2002 the Amati correlation was found Zhang meszaros analyzed spectral break models of GRBS: Rossiet al and zhang meszaros discussed the structured jet models Fanet al found the magnetized reverse shock in GrB 990123 2003: Schaefer discussed the cosmological use of Grbs; 2004: the Ghirlanda correlation was found Daiet al used this relation to constrain the cosmological parameters
➢ 2001: Frail et al. found a cluster of the jet-collimated energies; Panaitescu & Kumar fitted the afterglow data and obtained the model parameters ➢ 2002: the Amati correlation was found; Zhang & Meszaros analyzed spectral break models of GRBs; Rossi et al. and Zhang & Meszaros discussed the structured jet models; Fan et al. found the magnetized reverse shock in GRB 990123 ➢ 2003: Schaefer discussed the cosmological use of GRBs; ➢ 2004: the Ghirlanda correlation was found; Dai et al. used this relation to constrain the cosmological parameters