Peak Luminosity-Spectral Lag Relation Caused by the Viewing Angle of the Collimated Gamma-Ray Bursts

By K. Ioka, Takashi Nakamura. 2001

141 citations recorded by the source corpus.

We compute the kinematical dependence of the peak luminosity, the pulse width, and the spectral lag of the peak luminosity on the viewing angle θv of a jet. For appropriate model parameters we obtain a peak luminosity-spectral lag relation similar to the observed one including gamma-ray burst (GRB) 980425. A bright (dim) peak with short (long) spectral lag corresponds to a jet with small (large) viewing angle. This suggests that the viewing angle of the jet might cause various relations in GRBs such as the peak luminosity-variability relation and the luminosity-width relation. Our model also suggests that X-ray-rich GRBs (or X-ray flushes or fast X-ray transients) are typical GRBs observed from large θv with large spectral lag and low variability.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/9fe3298d58e18771ef2f2ef573a5b97034b60f65

How researchers see this paper

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In Astronomy and Astrophysics

1. Bing Zhang
2. E. Liang
3. B. Metzger
4. Pawan Kumar
5. E. Berger
6. E. Nakar
7. Binbin Zhang
8. Stephan Rosswog

In Instrumentation

1. Bing Zhang
2. Stephan Rosswog
3. E. Liang
4. Binbin Zhang
5. Z. Dai
6. P. Mészáros
7. E. Ramirez-Ruiz
8. D. Burrows

In Statistical and Nonlinear Physics

1. Bing Zhang
2. Jay Norris
3. E. Ramirez-Ruiz
4. K. Ioka
5. Stan Woosley
6. Chris L. Fryer
7. Stephan Rosswog
8. A. Inoue

Citations in the corpus

• Implications of the Lag-Luminosity Relationship for Unified Gamma-Ray Burst Paradigms (2002, background): “…and gamma-ray energy, and in some cases the gamma-ray pulse behavior (Frail et al. 2001; Panaitescu & Kumar 2002; Wang & Wheeler 1998; Höflich et al. 1999; Nakamura 1999; Woosley et al. 1999; Salmonson 2001; Ioka & Nakamura 2001; Salmonson & Galama 2002; Rossi et al. 2002; Zhang & Meszaros 2002).”
• X-Ray-rich Gamma-Ray Bursts, Photospheres, and Variability (2002, unknown): “(e.g., Ioka & Nakamura 2001; Plaga 2001).”
• Cosmological Aspects of Gamma-Ray Bursts: Luminosity Evolution and an Estimate of the Star Formation Rate at High Redshifts (2001, background): “…(in the 50–300 keV energy range3) and the light-curve ‘‘ variability ’’ for eight bursts with measured redshifts (models for the physical mechanism behind this correlation can be found in Plaga 2001, Ioka & Nakamura 2001, Kobayashi, Ryde, & MacFadyen 2001, and Ramirez-Ruiz & Lloyd-Ronning 2002).”
• High-resolution calculations of merging neutron stars - III. Gamma-ray bursts (2003, background): “Seen from one viewing angle a burst would appear as a X-ray rich burst (Heise et al. 2001) while from a different angle it would be interpreted as a standard GRB (Salmonson 2000; Ioka & Nakamura 2001; Kobayashi, Ryde & MacFadyen 2002; RamirezRuiz & Lloyd-Ronning 2002; Mészáros et al. 2002).”
• THE AFTERGLOWS OF SWIFT-ERA GAMMA-RAY BURSTS. II. TYPE I GRB VERSUS TYPE II GRB OPTICAL AFTERGLOWS (2008, background): “Salmonson (2000) and Ioka & Nakamura (2001) interpret the lagluminosity correlation (Norris et al. 2000) as a kinematic effect, dependent on the viewing angle from which we see the jet and on the Lorentz factor.”
• DISCERNING THE PHYSICAL ORIGINS OF COSMOLOGICAL GAMMA-RAY BURSTS BASED ON MULTIPLE OBSERVATIONAL CRITERIA: THE CASES OF z = 6.7 GRB 080913, z = 8.2 GRB 090423, AND SOME SHORT/HARD GRBs (2009, background): “None of the previous kinetic modelers (Salmonson 2000; Ioka & Nakamura 2001; Shen et al. 2005; Lu et al. 2006) have seriously confronted the flux predictions with the data (although the timing data have been well interpreted by the models).”
• The Cosmic Dispersion Measure from Gamma-Ray Burst Afterglows: Probing the Reionization History and the Burst Environment (2003, methodology): “High-z GRBs may have alreadyz 1 5 been detected by BATSE based on the empirical luminosity indicators (Fenimore & Ramirez-Ruiz 2000; Norris, Marani, & Bonnell 2000; Murakami et al. 2003; Yonetoku et al. 2003), for which some theoretical explanations exist (e.g., Ioka & Nakamura 2001a).”
• Variabilities of Gamma-Ray Burst Afterglows: Long-acting Engine, Anisotropic Jet, or Many Fluctuating Regions? (2004, background): “Such patchy shells may be realized in the sub-jet model (Yamazaki, Ioka, & Nakamura 2004; Ioka & Nakamura 2001a).”
• Gamma-Ray Bursts in the Swift Era (2007, background): “The origin of this relation may have something todo with the same kinetic effect to interpret theL− τ relation (Ioka & Nakamura 2001) or the screening effect of the pair photosphere (Kobayashi et al. 2002; Mészáros et al. 2002).”
• Relativistic Jets in Collapsars (2002, background): “These are not ordinary high Γ jets seen just beyond a sharp edge (Ioka & Nakamura 2001).”
• Low-Luminosity Gamma-Ray Bursts as a Unique Population: Luminosity Function, Local Rate, and Beaming Factor (2006, background): “Are these LL-GRBs from the same population as HL-GRBs (Nakamura 1999; Ioka & Nakamura 2001; Yamazaki et al. 2003; Guetta et al. 2004) or from a sub-energetic GRB population (Kulkarni et al. 1998; Soderber 2004b; Mazzali et al. 2006; Toma et al. 2006) with a much higher rate than that of the…”
• Gamma-Ray Burst Formation Rate Inferred from the Spectral Peak Energy-Peak Luminosity Relation (2003, background): “Then, a crude approximation of the luminosity L is given by L ¼ 2 L0 2 j for v < j; 2 L0( 6 j = 8 v ) for v > j: ( ð11Þ For the case of v > j, L is proportional to 4, where ¼ ½ (1 cos v) 1 / 2v , so that the luminosity has the dependence of 8v (Ioka & Nakamura 2001; Yamazaki et al. 2002, 2003).”