Gamma ray bursts flares detected and observed by the Swift satellite

Chincarini, G.; Moretti, A.; Romano, P.; Campana, S.; Covino, S.; Tagliaferri, G.; Falcone, A.; Burrows, D. N.; Gehrels, N.; Mangano, V.; Cusumano, G.; Perri, M.; Giommi, P.; Capalbi, M.

doi:10.1016/j.asr.2007.04.058

Cited by 3 publications

(3 citation statements)

References 32 publications

(33 reference statements)

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“…Ultra-long GRBs (including GRBs 121027A, 101225A and 111209A) last for T ∼ 10 3 − 10 4 s and have luminosity in the L γ obs ∼ 10 49 − 10 50 erg s −1 range. X-ray flares take place T delay ∼ 100 − 10 5 s after the GRB trigger and last for T f ∼ 0.1T delay ∼ 10 − 10 4 s (Chincarini et al 2007). Their fluence can approach that of GRBs but it is typically ∼10 times smaller: E iso flare 3 × 10 52 erg (Falcone et al 2007).…”

Section: Comparison With Observationsmentioning

confidence: 99%

“…Their fluence can approach that of GRBs but it is typically ∼10 times smaller: E iso flare 3 × 10 52 erg (Falcone et al 2007). The typical peak luminosity of the X-ray flares drops with time: L iso flare ∼ E iso flare /T flare (Chincarini et al 2007). To compare the jet power predicted by the model to the observed luminosity of GRBs, beaming and radiative efficiency corrections have to be taken into account.…”

Section: Comparison With Observationsmentioning

confidence: 99%

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Testing the neutrino annihilation model for launching GRB jets

Leng

Giannios

2014

Monthly Notices of the Royal Astronomical Society: Letters

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The mechanism behind the launching of gamma-ray-burst (GRB) jets remains debated resulting in large uncertainty over the jet composition. Both magnetohydrodynamical and neutrino annihilation models have been proposed for the energy extraction in a black hole/accretiondisc central engine. In particular, for the extreme accretion ratesṀ ∼ 0.1 − 1 M ⊙ s −1 expected for bursts of duration T 100 s, the disc can be an efficient neutrino emitter. Neutrinoantineutrino annihilation results in an energy deposition rate at the jet that can, in principle, account for the burst's energetics. Recent discoveries of X-ray flares hours after the burst and of ultra-long GRBs suggest that GRB activity can last for ∼ 10 4 s or longer. These longlived events have fluence similar to that of classical GRBs. In view of these findings, we re-evaluate the neutrino annihilation model. We derive the maximum possible energy of a neutrino-powered jet as a function of the burst duration and show that the available energy drops fast for longer bursts. For a standard choice of the parameters, the model falls short by three to four orders of magnitude in explaining the observed energetics of events that last longer than ∼ 10 3 s. (DG) 1 Note that a stellar tidal disruption at a galactic centre is another possibility for the origin of ultra-long GRBs.

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Section: Comparison With Observationsmentioning

confidence: 99%

Section: Comparison With Observationsmentioning

confidence: 99%

Testing the neutrino annihilation model for launching GRB jets

Leng

Giannios

2014

Monthly Notices of the Royal Astronomical Society: Letters

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“…GRB050607 and GRB050730, Pagani et al 2006;Perri et al 2007) while others have only one big flare (e.g. GRB060526, Chincarini et al 2007a).…”

Section: Introductionmentioning

confidence: 99%

Gamma-ray burst high energy emission from internal shocks

Galli

Guetta

2008

A&A

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Aims. In this paper we study synchrotron and synchrotron self Compton (SSC) emission from internal shocks (IS) during the prompt and X-ray flare phases of gamma-ray bursts (GRBs). The aim is to test the IS model for the flare emission and for whether GRBs can be GeV sources. Methods. We determine the parameters for which the IS model can account for the observed prompt and X-ray flares emission, and study the detectability of the high energy SSC emission by the AGILE and GLAST satellites. Results. We find that the detectability of the SSC emission during the prompt phase of GRBs improves for higher values of the fireball Lorentz factor Γ and of the temporal variability t v . If IS is the mechanism responsible for the flare emission, and the Lorentz factor of the shells producing the flare is Γ ∼ 100, the flare light curves are expected to present some substructures with temporal variability t v = 10−100 ms which are much smaller than the average duration of flares, and similar to those observed during the prompt phase of GRBs. If one assumes lower Lorentz factors, such as Γ ∼ 10 ÷ 25, then a larger temporal variability t v ∼ 40 s can also account for the observed flare properties. However in this case we predict that X-ray flares do not have a counterpart at very high energies (MeV-GeV).Conclusions. An investigation on the substructures of the X-ray flare light curves, and simultaneous X-ray and high energy observations, will allow us to corroborate the hypothesis that late IS are responsible for the X-ray flares.

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Flares in Long and Short Gamma-Ray Bursts

Dado

Dar

2010

ApJ

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Gamma ray bursts flares detected and observed by the Swift satellite

Cited by 3 publications

References 32 publications

Testing the neutrino annihilation model for launching GRB jets

Testing the neutrino annihilation model for launching GRB jets

Gamma-ray burst high energy emission from internal shocks

Flares in Long and Short Gamma-Ray Bursts

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