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Giant X-ray and optical Bump in GRBs: evidence for fall-back accretion model
High Energy Astrophysical Phenomena · Submitted 19 Dec 2020
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim The fall-back accretion model could well interpret the X-ray and optical bump for all candidates within a reasonable parameter space.
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The abstract, sentence by sentence
The successful operation of dedicated detectors has brought us valuable information for understanding the central engine and the progenitor of gamma-ray bursts (GRBs). For instance, the giant X-ray and optical bumps found in some long-duration GRBs (e.g. GRBs 121027A and 111209A) imply that some extended central engine activities, such as the late X-ray flares, are likely due to the fall-back of progenitor envelope materials. Here we systemically search for long GRBs that consist of a giant X-ray or optical bump from the Swift GRB sample, and eventually we find 19 new possible candidates. The fall-back accretion model could well interpret the X-ray and optical bump for all candidates within a reasonable parameter space. Six candidates showing simultaneous bump signatures in both X-ray and optical observations, which could be well fitted at the same time when scaling down the X-ray flux into optical by one order of magnitude, are consistent with the standard $F_{\nu}\propto\nu^{1/3}$ synchrotron spectrum. The typical fall-back radius is distributed around $10^{10}\rm-10^{12}$ cm, which is consistent with the typical radius of a Wolf-Rayet star. The peak fall-back accretion rate is in the range of $\sim 10^{-11}-10^{-4}M_{\odot} \ \text{s} ^{-1}$ at time $\sim10^{2}- 10^{5}~\rm s$, which is relatively easy to fulfill as long as the progenitor's metallicity is not too high. Combined with the sample we found, future studies of the mass supply rate for the progenitors with different mass, metallicity, and angular momentum distribution would help us to better constrain the progenitor properties of long GRBs.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The successful operation of dedicated detectors has brought us valuable information for understanding the central engine and the progenitor of gamma-ray bursts (GRBs). | background 1.00 | 0.06 | 0.02 | asserted 1.00 |
| s1 | For instance, the giant X-ray and optical bumps found in some long-duration GRBs (e.g. GRBs 121027A and 111209A) imply that some extended central engine activities, such as the late X-ray flares, are likely due to the fall-back of progenitor envelope materials. | background 0.61 | 0.09 | 0.21 | hedged possibility 1.00 |
| s2 | Here we systemically search for long GRBs that consist of a giant X-ray or optical bump from the Swift GRB sample, and eventually we find 19 new possible candidates. | contribution 0.79 | 0.97 | 0.08 | asserted 0.92 |
| s3 | The fall-back accretion model could well interpret the X-ray and optical bump for all candidates within a reasonable parameter space. | interpretation 0.88 | 0.73 | 0.59 | hedged possibility 0.99 |
| s4 | Six candidates showing simultaneous bump signatures in both X-ray and optical observations, which could be well fitted at the same time when scaling down the X-ray flux into optical by one order of magnitude, are consistent with the standard $F_{\nu}\propto\nu^{1/3}$ synchrotron spectrum. | result 0.93 | 0.88 | 0.08 | hedged possibility 0.94 |
| s5 | The typical fall-back radius is distributed around $10^{10}\rm-10^{12}$ cm, which is consistent with the typical radius of a Wolf-Rayet star. | result 0.93 | 0.83 | 0.08 | asserted 0.81 |
| s6 | The peak fall-back accretion rate is in the range of $\sim 10^{-11}-10^{-4}M_{\odot} \ \text{s} ^{-1}$ at time $\sim10^{2}- 10^{5}~\rm s$, which is relatively easy to fulfill as long as the progenitor's metallicity is not too high. | result 0.92 | 0.76 | 0.09 | asserted 0.84 |
| s7 | Combined with the sample we found, future studies of the mass supply rate for the progenitors with different mass, metallicity, and angular momentum distribution would help us to better constrain the progenitor properties of long GRBs. | future work 1.00 | 0.32 | 0.08 | hedged possibility 0.90 |
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Original abstract
The successful operation of dedicated detectors has brought us valuable information for understanding the central engine and the progenitor of gamma-ray bursts (GRBs). For instance, the giant X-ray and optical bumps found in some long-duration GRBs (e.g. GRBs 121027A and 111209A) imply that some extended central engine activities, such as the late X-ray flares, are likely due to the fall-back of progenitor envelope materials. Here we systemically search for long GRBs that consist of a giant X-ray or optical bump from the Swift GRB sample, and eventually we find 19 new possible candidates. The fall-back accretion model could well interpret the X-ray and optical bump for all candidates within a reasonable parameter space. Six candidates showing simultaneous bump signatures in both X-ray and optical observations, which could be well fitted at the same time when scaling down the X-ray flux into optical by one order of magnitude, are consistent with the standard $F_{\nu}\propto\nu^{1/3}$ synchrotron spectrum. The typical fall-back radius is distributed around $10^{10}\rm-10^{12}$ cm, which is consistent with the typical radius of a Wolf-Rayet star. The peak fall-back accretion rate is in the range of $\sim 10^{-11}-10^{-4}M_{\odot} \ \text{s} ^{-1}$ at time $\sim10^{2}- 10^{5}~\rm s$, which is relatively easy to fulfill as long as the progenitor's metallicity is not too high. Combined with the sample we found, future studies of the mass supply rate for the progenitors with different mass, metallicity, and angular momentum distribution would help us to better constrain the progenitor properties of long GRBs.
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3 arXiv papers cite this in 3 sentences
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Extensive investigations have been conducted on multi-wavelength afterglows, including giant flares, that involve energy injection models [ref] .
Synchrotron self-Compton Reverse Shock in Energy-Injection and Radiative Scenarios · Introduction · 0.92
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