Flares in Gamma Ray Bursts
The flare activity that is observed in GRBs soon after the prompt emission with the XRT (0.3-10 KeV) instrumenton Board of the Swift satellite is leading to important clues in relation to the physical characteristics of the mechanismgenerating the emission of energy in Gamma Ray Bursts. We will briefly refer to the results obtained with the recent analysis 1and2and discuss the preliminary results we obtained with a new larger sample of GRBslimited to early flaresbased on fitting of the flares using the Norris 2005 profile.We find,in agreement with previous results,that XRT flares follow the main characteristics observed in 3for the prompt emission spikes.The estimate of the flare energy for the subsample with redshift is rather robust and an attempt is made,using the redshisft sample,to estimate how the energy emitted in flares depends on time.We used a H0=70km/s/Mpc,ΩA=0.7Ωm=0.3 cosmology.
γ-ray sources γ-ray burst
G.Chincarini J.Mao F.Pasotti R.Margutti C.Guidorzi M.G.Bernardini Swfit Italian team
INAE Osservatorio Astronomico di Brera,Via E.Bianchi 46,I-23807,Merate (LC),Italy;Universita degli S INAE Osservatorio Astronomico di Brera,Via E.Bianchi 46,I-23807,Merate (LC),Italy INAE Osservatorio Astronomico di Brera,Via E.Bianchi 46,I-23807,Merate (LC),Italy;Universita degli S Universita diRoma La Sapienza,ICRA,ICRANet,Italy INAE Osservatorio Astronomico di Brera,Via E.Bianchi 46,I-23807,Merate (LC),Italy;Universita degli S
国际会议
2008 NanJing Gamma-Ray Burst Conference(2008年伽马暴国际研讨会)
南京
英文
19-24
2008-06-23（万方平台首次上网日期，不代表论文的发表时间）