Observations of X-ray flares from GRBs

A. D. Falcone, D. Morris, J. Racusin, G. Chincarini, A. Moretti, P. Romano, D. N. Burrows, C. Pagani, M. Stroh, D. Grupe, S. Campana, S. Covino, G. Tagliaferri, N. Gehrels

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Abstract

Swift-XRT observations of the X-ray emission from gamma ray bursts (GRBs) and during the GRB afterglow have led to many new results during the past two years. One of these exciting results is that ∼1/3-1/2 of GRBs contain detectable X-ray flares. The mean fluence of the X-ray flares is ∼10× less than that of the initial prompt emission, but in some cases the flare is as energetic as the prompt emission itself. The flares display fast rises and decays, and they sometimes occur at very late times relative to the prompt emission (sometimes as late as 105s after T0) with very high peak fluxes relative to the underlying afterglow decay that has clearly begun prior to some flares. The temporal and spectral properties of the flares are found to favor models in which flares arise due to the same GRB internal engine processes that spawned the prompt GRB emission. Therefore, both long and short GRB internal engine models must be capable of producing high fluences in the X-ray band at very late times.

Original languageEnglish (US)
Title of host publicationGamma-Ray Bursts 2007 - Proceedings of the Santa Fe Conference
Pages91-96
Number of pages6
DOIs
StatePublished - Dec 1 2008
EventSanta Fe Conference on Gamma-Ray Bursts 2007, GRB 2007 - Santa Fe, NM, United States
Duration: Nov 5 2007Nov 9 2007

Publication series

NameAIP Conference Proceedings
Volume1000
ISSN (Print)0094-243X
ISSN (Electronic)1551-7616

Other

OtherSanta Fe Conference on Gamma-Ray Bursts 2007, GRB 2007
CountryUnited States
CitySanta Fe, NM
Period11/5/0711/9/07

Fingerprint

gamma ray bursts
flares
x rays
afterglows
engines
fluence
decay

All Science Journal Classification (ASJC) codes

  • Physics and Astronomy(all)

Cite this

Falcone, A. D., Morris, D., Racusin, J., Chincarini, G., Moretti, A., Romano, P., ... Gehrels, N. (2008). Observations of X-ray flares from GRBs. In Gamma-Ray Bursts 2007 - Proceedings of the Santa Fe Conference (pp. 91-96). (AIP Conference Proceedings; Vol. 1000). https://doi.org/10.1063/1.2943557
Falcone, A. D. ; Morris, D. ; Racusin, J. ; Chincarini, G. ; Moretti, A. ; Romano, P. ; Burrows, D. N. ; Pagani, C. ; Stroh, M. ; Grupe, D. ; Campana, S. ; Covino, S. ; Tagliaferri, G. ; Gehrels, N. / Observations of X-ray flares from GRBs. Gamma-Ray Bursts 2007 - Proceedings of the Santa Fe Conference. 2008. pp. 91-96 (AIP Conference Proceedings).
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abstract = "Swift-XRT observations of the X-ray emission from gamma ray bursts (GRBs) and during the GRB afterglow have led to many new results during the past two years. One of these exciting results is that ∼1/3-1/2 of GRBs contain detectable X-ray flares. The mean fluence of the X-ray flares is ∼10× less than that of the initial prompt emission, but in some cases the flare is as energetic as the prompt emission itself. The flares display fast rises and decays, and they sometimes occur at very late times relative to the prompt emission (sometimes as late as 105s after T0) with very high peak fluxes relative to the underlying afterglow decay that has clearly begun prior to some flares. The temporal and spectral properties of the flares are found to favor models in which flares arise due to the same GRB internal engine processes that spawned the prompt GRB emission. Therefore, both long and short GRB internal engine models must be capable of producing high fluences in the X-ray band at very late times.",
author = "Falcone, {A. D.} and D. Morris and J. Racusin and G. Chincarini and A. Moretti and P. Romano and Burrows, {D. N.} and C. Pagani and M. Stroh and D. Grupe and S. Campana and S. Covino and G. Tagliaferri and N. Gehrels",
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Falcone, AD, Morris, D, Racusin, J, Chincarini, G, Moretti, A, Romano, P, Burrows, DN, Pagani, C, Stroh, M, Grupe, D, Campana, S, Covino, S, Tagliaferri, G & Gehrels, N 2008, Observations of X-ray flares from GRBs. in Gamma-Ray Bursts 2007 - Proceedings of the Santa Fe Conference. AIP Conference Proceedings, vol. 1000, pp. 91-96, Santa Fe Conference on Gamma-Ray Bursts 2007, GRB 2007, Santa Fe, NM, United States, 11/5/07. https://doi.org/10.1063/1.2943557

Observations of X-ray flares from GRBs. / Falcone, A. D.; Morris, D.; Racusin, J.; Chincarini, G.; Moretti, A.; Romano, P.; Burrows, D. N.; Pagani, C.; Stroh, M.; Grupe, D.; Campana, S.; Covino, S.; Tagliaferri, G.; Gehrels, N.

Gamma-Ray Bursts 2007 - Proceedings of the Santa Fe Conference. 2008. p. 91-96 (AIP Conference Proceedings; Vol. 1000).

Research output: Chapter in Book/Report/Conference proceedingConference contribution

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AU - Burrows, D. N.

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AU - Grupe, D.

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N2 - Swift-XRT observations of the X-ray emission from gamma ray bursts (GRBs) and during the GRB afterglow have led to many new results during the past two years. One of these exciting results is that ∼1/3-1/2 of GRBs contain detectable X-ray flares. The mean fluence of the X-ray flares is ∼10× less than that of the initial prompt emission, but in some cases the flare is as energetic as the prompt emission itself. The flares display fast rises and decays, and they sometimes occur at very late times relative to the prompt emission (sometimes as late as 105s after T0) with very high peak fluxes relative to the underlying afterglow decay that has clearly begun prior to some flares. The temporal and spectral properties of the flares are found to favor models in which flares arise due to the same GRB internal engine processes that spawned the prompt GRB emission. Therefore, both long and short GRB internal engine models must be capable of producing high fluences in the X-ray band at very late times.

AB - Swift-XRT observations of the X-ray emission from gamma ray bursts (GRBs) and during the GRB afterglow have led to many new results during the past two years. One of these exciting results is that ∼1/3-1/2 of GRBs contain detectable X-ray flares. The mean fluence of the X-ray flares is ∼10× less than that of the initial prompt emission, but in some cases the flare is as energetic as the prompt emission itself. The flares display fast rises and decays, and they sometimes occur at very late times relative to the prompt emission (sometimes as late as 105s after T0) with very high peak fluxes relative to the underlying afterglow decay that has clearly begun prior to some flares. The temporal and spectral properties of the flares are found to favor models in which flares arise due to the same GRB internal engine processes that spawned the prompt GRB emission. Therefore, both long and short GRB internal engine models must be capable of producing high fluences in the X-ray band at very late times.

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Falcone AD, Morris D, Racusin J, Chincarini G, Moretti A, Romano P et al. Observations of X-ray flares from GRBs. In Gamma-Ray Bursts 2007 - Proceedings of the Santa Fe Conference. 2008. p. 91-96. (AIP Conference Proceedings). https://doi.org/10.1063/1.2943557