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GRB after-glow: Supporting the cosmological fireball model, constraining parameters, and making predictions
Astrophysics · Submitted 13 Apr 1997
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We present several new results regarding the model predictions, and show that X-ray to optical observations of GRB970228 and GRB970402 are naturally explained by the model: The scaling of flux with time and frequency agrees with model predictions and requires a power law distribution of shock accelerated electrons, dlog N/dlog E=2.3+-0.1 (implying, and consistent with the observed, 1/t decline of flux observed at a given frequency); The absolute flux value agrees with that inferred through the model from observed gamma-ray fluence.
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The abstract, sentence by sentence
Cosmological fireball models of gamma-ray bursts (GRBs) predict delayed emission, ``after-glow,'' at longer wavelengths. We present several new results regarding the model predictions, and show that X-ray to optical observations of GRB970228 and GRB970402 are naturally explained by the model: The scaling of flux with time and frequency agrees with model predictions and requires a power law distribution of shock accelerated electrons, dlog N/dlog E=2.3+-0.1 (implying, and consistent with the observed, 1/t decline of flux observed at a given frequency); The absolute flux value agrees with that inferred through the model from observed gamma-ray fluence. The future after-glow emission of these bursts is predicted. The observations indicate that the ratio of magnetic field to equipartition value and the fraction F of dissipated kinetic energy carried by electrons are not much smaller than 1. More frequent observations at a fixed wavelength, or a wide spectrum at a fixed time, would put strong constraints on these parameters. We show that inverse-Compton scattering suppresses X-ray/ optical emission at delays t<T=10(F/0.3)^4 hr. Observations therefore imply F<0.3. The strong dependence of T on F implies that T may vary widely from burst to burst, and that frequent X-ray/optical observations at t~T would determine F. For F~0.2, inverse-Compton emission dominates during the first 2hr, producing >1GeV photons and providing a natural explanation to the delayed GeV emission observed in several strong bursts.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | Cosmological fireball models of gamma-ray bursts (GRBs) predict delayed emission, ``after-glow,'' at longer wavelengths. | background 1.00 | 0.04 | 0.07 | asserted 0.95 |
| s1 | We present several new results regarding the model predictions, and show that X-ray to optical observations of GRB970228 and GRB970402 are naturally explained by the model: The scaling of flux with time and frequency agrees with model predictions and requires a power law distribution of shock accelerated electrons, dlog N/dlog E=2.3+-0.1 (implying, and consistent with the observed, 1/t decline of flux observed at a given frequency); The absolute flux value agrees with that inferred through the model from observed gamma-ray fluence. | result 0.59 | 0.92 | 0.62 | asserted 1.00 |
| s2 | The future after-glow emission of these bursts is predicted. | contribution 0.52 | 0.73 | 0.11 | asserted 1.00 |
| s3 | The observations indicate that the ratio of magnetic field to equipartition value and the fraction F of dissipated kinetic energy carried by electrons are not much smaller than 1. | result 0.80 | 0.84 | 0.14 | hedged possibility 0.83 |
| s4 | More frequent observations at a fixed wavelength, or a wide spectrum at a fixed time, would put strong constraints on these parameters. | future work 0.99 | 0.19 | 0.05 | hedged possibility 0.60 |
| s5 | We show that inverse-Compton scattering suppresses X-ray/ optical emission at delays t<T=10(F/0.3)^4 hr. | result 0.93 | 0.82 | 0.08 | asserted 1.00 |
| s6 | Observations therefore imply F<0.3. | result 0.65 | 0.81 | 0.17 | asserted 0.97 |
| s7 | The strong dependence of T on F implies that T may vary widely from burst to burst, and that frequent X-ray/optical observations at t~T would determine F. | interpretation 0.77 | 0.73 | 0.10 | hedged possibility 0.91 |
| s8 | For F~0.2, inverse-Compton emission dominates during the first 2hr, producing >1GeV photons and providing a natural explanation to the delayed GeV emission observed in several strong bursts. | interpretation 0.79 | 0.73 | 0.11 | asserted 0.89 |
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The paper
Original abstract
Cosmological fireball models of gamma-ray bursts (GRBs) predict delayed emission, ``after-glow,'' at longer wavelengths. We present several new results regarding the model predictions, and show that X-ray to optical observations of GRB970228 and GRB970402 are naturally explained by the model: The scaling of flux with time and frequency agrees with model predictions and requires a power law distribution of shock accelerated electrons, dlog N/dlog E=2.3+-0.1 (implying, and consistent with the observed, 1/t decline of flux observed at a given frequency); The absolute flux value agrees with that inferred through the model from observed gamma-ray fluence. The future after-glow emission of these bursts is predicted. The observations indicate that the ratio of magnetic field to equipartition value and the fraction F of dissipated kinetic energy carried by electrons are not much smaller than 1. More frequent observations at a fixed wavelength, or a wide spectrum at a fixed time, would put strong constraints on these parameters. We show that inverse-Compton scattering suppresses X-ray/ optical emission at delays t<T=10(F/0.3)^4 hr. Observations therefore imply F<0.3. The strong dependence of T on F implies that T may vary widely from burst to burst, and that frequent X-ray/optical observations at t~T would determine F. For F~0.2, inverse-Compton emission dominates during the first 2hr, producing >1GeV photons and providing a natural explanation to the delayed GeV emission observed in several strong bursts.
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References
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10 arXiv papers cite this in 10 sentences
Papers citing it · 5 sentences without a confident label
Cites it as background 5 papers
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Gamma-ray burst (GRB) afterglows are produced by synchrotron emission arising from the collision of ultra-relativistic ejecta with a circumburst medium [ref] .
Systematic Error in Approximate Models of the GRB Early Afterglow · Introduction · 1.00
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The physical mechanism responsible for the multi-wavelength observation is broadly believed to be synchrotron radiation from the relativistic electrons accelerated at the external shock, developing when the relativistic outflow expands in the CBM [ref] .
Multi-messenger detection prospects of gamma-ray burst afterglows with optical jumps · Introduction · 0.87
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Alternative models for the emission in internal shocks include synchrotron self-Compton [ref] and inverse Compton scattering of external light [ref] similarly to the emission mechanism for blazar jets.
Gamma-Ray Burst Observations at High Energy with the Fermi Large Area Telescope · $$-ray emission mechanisms · 0.80
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