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Cited by 254

The DOI matches its Crossref record; 49 of the 49 references it cites were found in a registry or an index.

The First Survey of X‐Ray Flares from Gamma‐Ray Bursts Observed by Swift: Temporal Properties and Morphology

Open access
Chincarini, G., Moretti, A., Romano, P., Falcone, A. D., Morris, D., Racusin, J., Campana, S., Covino, S., Guidorzi, C., Tagliaferri, G., Burrows, D. N., Pagani, C., Stroh, M., Grupe, D., Capalbi, M., Cusumano, G., Gehrels, N., Giommi, P., La Parola, V., Mangano, V., Mineo, T., Nousek, J. A., O’Brien, P. T., Page, K. L., Perri, M., Troja, E., Willingale, R., Zhang, B.·2007·The Astrophysical Journal

Abstract

We present the first systematic investigation of the morphological and timing properties of flares in GRBs observed by Swift XRT. We consider a large sample drawn from all GRBs detected by Swift , INTEGRAL , and HETE-2 prior to 2006 January 31, which had an XRT follow-up and which showed significant flaring. Our sample of 33 GRBs includes long and short, at low and high redshift, and a total of 69 flares. The strongest flares occur in the early phases, with a clear anticorrelation between the flare peak intensity and the flare time of occurrence. Fitting each X-ray flare with a Gaussian model, we find that the mean ratio of the width and peak time is ⟨ Δ t / t ⟩ = 0.13 ± 0.10, albeit with a large scatter. Late flares at times >2000 s have long durations, Δ t > 300 s, and can be very energetic compared to the underlying continuum. We further investigated whether there is a clear link between the number of pulses detected in the prompt phase by BAT and the number of X-ray flares detected by XRT, finding no correlation. However, we find that the distribution of intensity ratios between successive BAT prompt pulses and that between successive XRT flares is the same, an indication of a common origin for gamma-ray pulses and X-ray flares. All evidence indicates that flares are indeed related to the workings of the central engine and, in the standard fireball scenario, originate from internal shocks rather than external shocks. While all flares can be explained by long-lasting engine activity, 29/69 flares may also be explained by refreshed shocks. However, 10 can only be explained by prolonged activity of the central engine.

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Metadata

Authors
Chincarini, G., Moretti, A., Romano, P., Falcone, A. D., Morris, D., Racusin, J., Campana, S., Covino, S., Guidorzi, C., Tagliaferri, G., Burrows, D. N., Pagani, C., Stroh, M., Grupe, D., Capalbi, M., Cusumano, G., Gehrels, N., Giommi, P., La Parola, V., Mangano, V., Mineo, T., Nousek, J. A., O’Brien, P. T., Page, K. L., Perri, M., Troja, E., Willingale, R., & Zhang, B.
Venue
The Astrophysical Journal
Published
2007-12-20
Volume
671
Issue
2
Pages
1903-1920
ISSN
  • 0004-637X (ISSN-L)
  • 1538-4357
OpenAlex
W2027706131
Cited by
254
References
49
FWCI
16.10
Type
journal article
Language
en
Open access
bronze

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CoChat. (2026). Citation check: The First Survey of X‐Ray Flares from Gamma‐Ray Bursts Observed by Swift: Temporal Properties and Morphology. https://app.cochat.ai/papers/10.1086/521591
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Chincarini, G., Moretti, A., Romano, P., Falcone, A. D., Morris, D., Racusin, J., Campana, S., Covino, S., Guidorzi, C., Tagliaferri, G., Burrows, D. N., Pagani, C., Stroh, M., Grupe, D., Capalbi, M., Cusumano, G., Gehrels, N., Giommi, P., La Parola, V., . . . Zhang, B. (2007). The First Survey of X‐Ray Flares from Gamma‐Ray Bursts Observed by Swift: Temporal Properties and Morphology. The Astrophysical Journal. https://doi.org/10.1086/521591

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Contains information from the Semantic Scholar Academic Graph Datasets, made available under the ODC Attribution License (ODC-BY 1.0).

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