Light Curves of Gamma-Ray Burst Optical Flashes

By S. Kobayashi. 2000

242 citations recorded by the source corpus.

The standard model of gamma-ray burst (GRB) afterglows assumes that relativistically expanding material is decelerating as a result of interaction with the surrounding medium. The afterglows are well described by the synchrotron radiation from a forward shock, while the strong optical flash associated with GRB 990123 can be attributed to the emission from a reverse shock. We give a detailed study on the reverse shock emission. The full light curves are calculated for long and short GRB cases. We discuss the lack of the prompt optical detections by ROTSE for GRB 981121 and GRB 981223.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/fee29beb57cb72304a4f01fc5c3c0bbe3ac28d3c

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In Astronomy and Astrophysics

1. Bing Zhang
2. Pawan Kumar
3. E. Liang
4. Binbin Zhang
5. E. Berger
6. Xuefeng Wu
7. W. Lei
8. D. Burrows

Citations in the corpus

• CONSTRAINING GAMMA-RAY BURST INITIAL LORENTZ FACTOR WITH THE AFTERGLOW ONSET FEATURE AND DISCOVERY OF A TIGHT Γ0–Eγ,iso CORRELATION (2009, background): “In the optical band, early emission may be contaminated by the emission from the reverse shock (Mészáros & Rees 1997; Sari & Piran 1999; Kobayashi 2000; Zhang et al. 2003).”
• Gamma-Ray Bursts in the Swift Era (2007, background): “Even without additional suppression effects, a non-relativistic shockwith σ = 0 would generally give a reverse shock peak flux below the forward shock peak level (Kobayashi 2000;Nakar & Piran 2004; Zhang & Kobayashi 2005).”
• A complete reference of the analytical synchrotron external shock models of gamma-ray bursts (2013, methodology): “For the ISM case (k = 0), one may adopt g ’ 2 (Kobayashi, 2000; Zou et al., 2005).”
• OBSERVATIONS OF THE NAKED-EYE GRB 080319B: IMPLICATIONS OF NATURE'S BRIGHTEST EXPLOSION (2008, background): “Alternatively, the reverse-shock model (Kobayashi 2000) also predicts a very steep early decay, although even this model cannot exactly reconcile the steep decay with the observed spectral index; given α = 2.2 this model predicts β = 0.8.”
• Gamma-ray burst afterglows (2006, background): “Even without additional suppression effects, a non-relativistic shock with σ = 0 would generally give a reverse shock peak flux below the forward shock peak level (Kobayashi 2000; Nakar & Piran 2004; Zhang & Kobayashi 2005).”
• Probing the cosmic reionization history and local environment of gamma‐ray bursts through radio dispersion (2003, background): “…the GRB surroundings may vary significantly from burst to burst, as the fluence of UV ionizing photons emitted from the reverse shock can depend strongly on the initial Lorentz factor, GRB duration and other parameters (Kobayashi 2000, Waxman & Draine 2000, Draine & Hao 2002, Perna & Lazzati 2002).”
• The physics of gamma-ray bursts & relativistic jets (2014, background): “A detailed study of the RS dynamics and emission signature can be found in Kobayashi (2000).”
• Physical Processes Shaping Gamma-Ray Burst X-Ray Afterglow Light Curves: Theoretical Implications from the Swift X-Ray Telescope Observations (2005, background): “…argument that the reverse shock emission component plays an important role in the optical band; e.g.,Mészáros& Rees 1997a, 1999; Sari & Piran 1999; Kobayashi 2000; Kobayashi & Zhang 2003a, 2003b; Zhang et al. 2003; Wei 2003; Wu et al. 2003; Li et al. 2003b; Fan et al. 2004a, 2005b, 2005c; Zhang…”