MG13 - Talk detail |
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Participant |
Bianco, Carlo Luciano | |||||||
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Institution |
ICRANet - c/o Dip. di Fisica - Univ. La Sapienza - Piazzale Aldo Moro 5 - Roma - RM - Italy | |||||||
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Session |
GRB4 |
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Talk |
Oral abstract |
Title |
The fireshell model for GRBs: toward a canonical GRB scenario | |||||
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Abstract |
Within the fireshell model, Gamma-Ray Burst (GRB) light curves are composed by two distinct phenomena: the Proper GRB (P-GRB), emitted when the fireshell becomes transparent, and the extended afterglow, emitted due to the interaction with the CircumBurst Medium (CBM) of the ultrarelativistic baryonic matter shell left over after the transparency point. The peak of the extended afterglow, together with the P-GRB, forms what is usually called the "prompt emission". Such a theoretical framework implies the existence of three GRB classes, as a function of the fireshell baryon loading and of the CBM average density: the "genuine" short GRBs, where the P-GRB is energetically predominant over the extended afterglow, the "long" GRBs, where the extended afterglow is energetically predominant over the P-GRB, and the "disguised" short GRBs, where the extended afterglow, although still energetically predominant, has a peak flux lower than the P-GRB one due to a peculiarly low value of the CBM density, typical of galactic halos. In the talk I will discuss the "canonical GRB" scenario implied by the fireshell model, with particular emphasis on the "disguised short" GRB class, together with the implications of this scenario for the empirical correlations found in GRBs. |
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Accepted |
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Oral abstract |
Title |
Cooling processes and URCA emission in young NSs | |||||
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Abstract |
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Session |
SN1 |
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Talk |
Oral abstract |
Title |
Cooling processes and URCA emission in young NSs | |||||
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Abstract |
The traditional study of neutron star cooling has been generally applied to quite old objects such as the Crab Pulsar (957 years) or the central compact object in Cassiopeia A (330 years) with an observed surface temperature ~106 K. However, recent observations of the late (t = 10^8-10^9 s) emission of the supernovae (SNe) associated to GRBs (GRB-SN) show a distinctive emission in the X-ray regime consistent with temperatures ~10^7-10^8 K, which we defined as URCA emission. Similar features have been also observed in two Type Ic SNe SN 2002ap and SN 1994I that are not associated to GRBs. We advance the possibility that the late X-ray emission observed in GRB-SN and in isolated SN is associated to a hot neutron star just formed in the SN event, which we defined as a neo-neutron star. |
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