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Blue Supergiant Model for Ultra-Long Gamma-Ray Burst with Superluminous-Supernova-Like Bump
High Energy Astrophysical Phenomena · Submitted 18 Jul 2013
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim In this paper, we examine u, g, r, i, and J-band light curves of three ULGRBs and demonstrate that they can be fitted quite well by our BSG model with the appropriate choices of the jet opening angle and the number density of the ambient gas.
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Long GRBs (LGRBs) have typical duration of ~ 30 s and some of them are associated with hypernovae, like Type Ic SN 1998bw. Wolf-Rayet stars are the most plausible LGRB progenitors, since the free-fall time of the envelope is consistent with the duration, and the natural outcome of the progenitor is a Type Ic SN. While a new population of ultra-long GRBs (ULGRBs), GRB 111209A, GRB 101225A, and GRB 121027A, has a duration of ~ 10^4 s, two of them are accompanied by superluminous-supernova (SLSN) like bumps, which are <~ 10 times brighter than typical hypernovae. Wolf-Rayet progenitors cannot explain ULGRBs because of too long duration and too bright SN-like bump. A blue supergiant (BSG) progenitor model, however, can explain the duration of ULGRBs. Moreover, SLSN-like bump can be attributed to the so-called cocoon-fireball photospheric emissions (CFPEs). Since a large cocoon is inevitably produced during the relativistic jet piercing though the BSG envelope, this component can be a smoking-gun evidence of BSG model for ULGRBs. In this paper, we examine u, g, r, i, and J-band light curves of three ULGRBs and demonstrate that they can be fitted quite well by our BSG model with the appropriate choices of the jet opening angle and the number density of the ambient gas. In addition, we predict that for 121027A, SLSN-like bump could have been observed for ~ 20 - 80 days after the burst. We also propose that some SLSNe might be CFPEs of off-axis ULGRBs without visible prompt emission.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Long GRBs (LGRBs) have typical duration of ~ 30 s and some of them are associated with hypernovae, like Type Ic SN 1998bw. | background 1.00 | 0.04 | 0.02 | asserted 0.99 |
| s1 | Wolf-Rayet stars are the most plausible LGRB progenitors, since the free-fall time of the envelope is consistent with the duration, and the natural outcome of the progenitor is a Type Ic SN. | background 1.00 | 0.06 | 0.02 | hedged possibility 0.61 |
| s2 | While a new population of ultra-long GRBs (ULGRBs), GRB 111209A, GRB 101225A, and GRB 121027A, has a duration of ~ 10^4 s, two of them are accompanied by superluminous-supernova (SLSN) like bumps, which are <~ 10 times brighter than typical hypernovae. | background 0.95 | 0.06 | 0.03 | asserted 1.00 |
| s3 | Wolf-Rayet progenitors cannot explain ULGRBs because of too long duration and too bright SN-like bump. | gap 0.59 | 0.13 | 0.04 | asserted 1.00 |
| s4 | A blue supergiant (BSG) progenitor model, however, can explain the duration of ULGRBs. | contribution 0.40 | 0.23 | 0.24 | asserted 0.76 |
| s5 | Moreover, SLSN-like bump can be attributed to the so-called cocoon-fireball photospheric emissions (CFPEs). | interpretation 0.80 | 0.25 | 0.12 | asserted 0.80 |
| s6 | Since a large cocoon is inevitably produced during the relativistic jet piercing though the BSG envelope, this component can be a smoking-gun evidence of BSG model for ULGRBs. | interpretation 1.00 | 0.20 | 0.24 | asserted 0.59 |
| s7 | In this paper, we examine u, g, r, i, and J-band light curves of three ULGRBs and demonstrate that they can be fitted quite well by our BSG model with the appropriate choices of the jet opening angle and the number density of the ambient gas. | contribution 0.71 | 0.97 | 0.49 | asserted 0.99 |
| s8 | In addition, we predict that for 121027A, SLSN-like bump could have been observed for ~ 20 - 80 days after the burst. | result 0.85 | 0.84 | 0.09 | hedged possibility 0.99 |
| s9 | We also propose that some SLSNe might be CFPEs of off-axis ULGRBs without visible prompt emission. | interpretation 0.84 | 0.44 | 0.12 | speculative 0.78 |
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The paper
Original abstract
Long GRBs (LGRBs) have typical duration of ~ 30 s and some of them are associated with hypernovae, like Type Ic SN 1998bw. Wolf-Rayet stars are the most plausible LGRB progenitors, since the free-fall time of the envelope is consistent with the duration, and the natural outcome of the progenitor is a Type Ic SN. While a new population of ultra-long GRBs (ULGRBs), GRB 111209A, GRB 101225A, and GRB 121027A, has a duration of ~ 10^4 s, two of them are accompanied by superluminous-supernova (SLSN) like bumps, which are <~ 10 times brighter than typical hypernovae. Wolf-Rayet progenitors cannot explain ULGRBs because of too long duration and too bright SN-like bump. A blue supergiant (BSG) progenitor model, however, can explain the duration of ULGRBs. Moreover, SLSN-like bump can be attributed to the so-called cocoon-fireball photospheric emissions (CFPEs). Since a large cocoon is inevitably produced during the relativistic jet piercing though the BSG envelope, this component can be a smoking-gun evidence of BSG model for ULGRBs. In this paper, we examine u, g, r, i, and J-band light curves of three ULGRBs and demonstrate that they can be fitted quite well by our BSG model with the appropriate choices of the jet opening angle and the number density of the ambient gas. In addition, we predict that for 121027A, SLSN-like bump could have been observed for ~ 20 - 80 days after the burst. We also propose that some SLSNe might be CFPEs of off-axis ULGRBs without visible prompt emission.
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References
How the literature uses it
3 arXiv papers cite this in 5 sentences
Papers citing it · 4 sentences without a confident label
Cites it as background 1 paper
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However it still remains an open question what is the dominate dynamics of GRB progenitors, and many efforts have been made to find answers [ref] .
Gravo-thermal catastrophe in gravitational collapse and energy progenitor of Gamma-Ray Bursts · Introduction · 0.98
What it cites · 16 sentences without a confident label
Uses data or values from 4 papers
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Especially in GRB 111209A afterglow, a J-band bump with AB mag $∼22$ has been confirmed around $1050$ days after the burst [ref] .
A new population of ultra-long duration gamma-ray bursts · Introduction · 0.89
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The HI column densities of the host galaxies are measured as $N_H^host = 1.2 ×10^21 cm^-2$ for GRB 101225 [ref] , $N_H^host = 1.9 ×10^21 cm^-2$ for GRB 111209 [ref] , and $N_H^host = 1.3 ×10^22 cm^-2$ for GRB 121027 [ref] , respectively.
GRB 121027A: long-lasting, energetic X-ray flares and clues to radiation mechanism and progenitor star · Afterglow Emission · 1.00
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From observation, the V-band extinction takes values of $A_V^host ∼0.1 3.0$ [ref] .
Dust extinction for an unbiased sample of GRB afterglows · Afterglow Emission · 0.99
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