The DOI matches its Crossref record; 159 of the 159 references it cites were found in a registry or an index.
Physical Processes Shaping Gamma‐Ray Burst X‐Ray Afterglow Light Curves: Theoretical Implications from the Swift X‐Ray Telescope Observations
Open accessAbstract
With the successful launch of the Swift Gamma-Ray Burst Explorer, a rich trove of early X-ray afterglow data has been collected by its onboard X-Ray Telescope (XRT). Some interesting features are emerging, including a distinct rapidly decaying component preceding the conventional afterglow component in many sources, a shallow decay component before the more "normal" decay component observed in a good fraction of GRBs, and X-ray flares in nearly half of the afterglows. In this paper we systematically analyze the possible physical processes that shape the properties of the early X-ray afterglow light curves and use the data to constrain various models. We suggest that the steep decay component is consistent with the tail emission of the prompt gamma-ray bursts and/or the X-ray flares. This provides strong evidence that the prompt emission and afterglow emission are likely two distinct components, supporting the internal origin of the GRB prompt emission. The shallow decay segment observed in a group of GRBs suggests that very likely the forward shock keeps being refreshed for some time. This might be caused by either a long-lived central engine, or a wide distribution of the shell Lorentz factors, or else possibly the deceleration of a Poynting flux-dominated flow. X-ray flares suggest that the GRB central engine is very likely still active after the prompt gamma-ray emission is over, but with a reduced activity at later times. In some cases, the central engine activity even extends to days after the burst triggers. Analyses of early X-ray afterglow data reveal that GRBs are indeed highly relativistic events and that early afterglow data of many bursts, starting from the beginning of the XRT observations, are consistent with the afterglow emission from an ISM environment.
Overview
The claims and statistics of this paper haven’t been checked yet.
Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.
Integrity signals
Registry
Cites
Statistics
Verification
Claims the paper makes
The claims and statistics of this paper haven’t been checked yet.
Run the check — free, no account needed. It reads the open-access text and checks the sources it cites.
Claims other papers make about this one
Each is checked against this paper’s own text: does it say what the citing paper says it does?
In the citing paper
“Detection and measurement of gamma-ray burst afterglows and transients ( e.g., Zhang & Mészáros 2004; Zhang et al. 2006; Kann et al. 2010 ) to high redshift ( ∼ 7.5 )”
From LSST: From Science Drivers to Reference Design and Anticipated Data Products (2019) · cites this paper as Zhang et al. 2006
Self-check
Percentages, sums and reported differences re-computed from the paper’s own numbers.
The self-check needs the paper’s full text.
Citations
Cites
Burrows, D. N., Hill, J. E., Nousek, J. A., Kennea, J. A., Wells, A., Osborne, J. P., Abbey, A. F., Beardmore, A. P., Mukerjee, K., Short, A. D. T., et al. (2005) · Space Science Reviews · doi:10.1007/s11214-005-5097-2 · Cited by 2,649
Self-citationSpectra and Light Curves of Gamma-Ray Burst Afterglows
Sari, R., Piran, T., & Narayan, R. (1998) · The Astrophysical Journal · doi:10.1086/311269 · Cited by 2,303 · cited 2×
“…the external shock (Mészáros & Rees 1993; Dermer & Mitman 1999) or do they come from different locations (i.e., prompt emission from the internal shocks [Rees & Mészáros 1994; Paczynski & Xu 1994], while the afterglow comes from the external shock [Mészáros & Rees 1997a; Sari et al. 1998])?”
BackgroundMethodBATSE observations of gamma-ray burst spectra. I - Spectral diversity
Band, D. L., Matteson, J. L., Ford, L., Schaefer, B. E., Palmer, D. M., Teegarden, B. J., Cline, T. L., Briggs, M. S., Pačiesas, W. S., Pendleton, G. N., et al. (1993) · The Astrophysical Journal · doi:10.1086/172995 · Cited by 2,298
Unsteady outflow models for cosmological gamma-ray bursts
Rees, M. J., & Meszaros, P. (1994) · The Astrophysical Journal · doi:10.1086/187446 · Cited by 1,275 · cited 2×
“…the external shock (Mészáros & Rees 1993; Dermer & Mitman 1999) or do they come from different locations (i.e., prompt emission from the internal shocks [Rees & Mészáros 1994; Paczynski & Xu 1994], while the afterglow comes from the external shock [Mészáros & Rees 1997a; Sari et al. 1998])?”
BackgroundSelf-citationOptical and Long‐Wavelength Afterglow from Gamma‐Ray Bursts
Mészáros, P., & Rees, M. J. (1997) · The Astrophysical Journal · doi:10.1086/303625 · Cited by 1,200 · cited 3×
“…the external shock (Mészáros & Rees 1993; Dermer & Mitman 1999) or do they come from different locations (i.e., prompt emission from the internal shocks [Rees & Mészáros 1994; Paczynski & Xu 1994], while the afterglow comes from the external shock [Mészáros & Rees 1997a; Sari et al. 1998])?”
BackgroundSpectra and Light Curves of Gamma-Ray Burst AfterglowsPreprint
Sari, R., Piran, T., & Narayan, R. (1997) · Cited by 1,195
Sari, R., Piran, T., & Halpern, J. P. (1999) · The Astrophysical Journal · doi:10.1086/312109 · Cited by 1,051
Millisecond pulsars with extremely strong magnetic fields as a cosmological source of γ-ray bursts
Усов, В. В. (1992) · Nature · doi:10.1038/357472a0 · Cited by 1,039 · cited 1×
“The energy injection is also brief, but the outflow has a significant fraction of Poynting flux (e.g., Usov 1992; Thompson 1994; Mészáros & Rees 1997b; Lyutikov & Blandford 2003).”
BackgroundRelativistic fireballs: energy conversion and time-scales
Rees, M. J., & Mészáros, P. (1992) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/258.1.41p · Cited by 912
Evidence for a Canonical Gamma‐Ray Burst Afterglow Light Curve in the Swift XRT Data
Nousek, J. A., Kouveliotou, C., Grupe, D., Page, K. L., Granot, J., Ramirez-Ruiz, E., Patel, S., Burrows, D. N., Mangano, V., Barthelmy, S. D., et al. (2006) · The Astrophysical Journal · doi:10.1086/500724 · Cited by 886 · cited 4×
“Limited by the quality of the data, the current analyses indicate that the spectral indices remain unchanged in segments II, III, and IV, with a typical value of X 1 (FX / X ; Nousek et al. 2006).”
BackgroundInfluentialSelf-citation
Flagged first, then by citations
Research works printed but not linked: 14
- Burenin R. A., 1999, A&A, 344, L53
- Burrows D. N., 2005, Rev., 120, 165
- Dai Z. G., 1998, A&A, 333, L87
- Dermer, C. & Mitman, K. E. 2004, in ASP Conf. Ser. 312, Third Rome Workshop on Gamma-Ray Bursts in the Afterglow Era, ed. M. Feroci et al. (San Francisco: ASP), 301
- Dyks, J., Zhang, B. & Fan, Y. Z. 2005, ApJ, submitted (astro-ph/0511699) · arXiv
- Goad, M. 2006, A&A, in press (astro-ph/0511751) · arXiv
- Kobayashi, S., Zhang, B., Meszaros, P. & Burrows, D. N. 2005, ApJ, submitted (astro-ph/0506157) · arXiv
- Lyutikov, M. & Blandford, R. D. 2003, MNRAS, submitted (astro-ph/0312347) · arXiv
- Panaitescu, A., Meszaros, P., Gehrels, N., Burrows, D. & Nousek, J. 2006, MNRAS, in press (astro-ph/0508340) · arXiv
- Piro L., 1998, A&A, 331, L41
- Proga, D. & Zhang, B. 2006, ApJ, submitted (astro-ph/0601272) · arXiv
- Romano, P., etal 2006, A&A, submitted (astro-ph/0602497) · arXiv
- Rossi, E., Beloborodov, A. M. & Rees, M. J. 2004, in AIP Conf. Proc. 727, Gamma-Ray Bursts: 30 Years of Discovery, ed. E. E. Fenimore & M. Galassi (New York: AIP), 198
- Woosley, S. E., Zhang, W. & Heger, A. 2003, in AIP Conf. Proc. 662, Gamma-Ray Burst and Afterglow Astronomy 2001, ed. G. R. Ricker & R. K. Vanderspek (New York: AIP), 185
Cited by
Sorted by citations
Items 501–600 of 1,000
Einstein Probe discovery of EP240408a: A peculiar X-ray transient with an intermediate timescale
Zhang, W., Yuan, W., Ling, Z., Chen, Y., Rea, N., Rau, A., Cai, Z., Cheng, H., Zelati, F. C., Dai, L., et al. (2024) · Science China Physics Mechanics and Astronomy · doi:10.1007/s11433-024-2524-4 · Cited by 22
Steep Decay of GRB X-Ray Flares: The Results of Anisotropic Synchrotron Radiation
Geng, J.-J., Huang, Y.-F., & Dai, Z.-G. (2017) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/aa725a · Cited by 22
Zhao, L., Liu, L.-D., Gao, H., Lan, L., Lei, W., & Xie, W. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab8f91 · Cited by 22
A Semianalytic Afterglow with Thermal Electrons and Synchrotron Self-Compton Emission
Warren, D. C., Dainotti, M. G., Barkov, M. V., Ahlgren, B., Ito, H., & Nagataki, S. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac2f43 · Cited by 22
“The afterglows modeled here correspond to Phase III of the canonical afterglow (Zhang et al. 2006; Racusin et al. 2009).”
BackgroundMethodInfluentialSalafia, O. S., Colombo, A., Gabrielli, F., & Mandel, I. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202243260 · Cited by 22
Dependence of Temporal Properties on Energy in Long-Lag, Wide-Pulse Gamma-Ray Bursts
Zhang, F.-W., Qin, Y.-P., & Zhang, B.-B. (2007) · Publications of the Astronomical Society of Japan · doi:10.1093/pasj/59.4.857 · Cited by 22
“…has been extensively studied (Link, Epstein, & Priedhorsky 1993; Cheng et al. 1995; Norris et al. 1996; Norris, Narani & Bonnell 2000; Wu & Fenimore 2000; Hakkila & Giblin 2004; Hakkila & Giblin 2006; Chen et al. 2005; Norris & Bonnell 2006; Yi et al. 2006; Zhang et al. 2006b; Zhang et al. 2006c).”
BackgroundSelf-citationThe afterglow and host galaxy of GRB 090205: evidence of a Ly-αemitter at z = 4.65
D’Avanzo, P., Perri, M., Fugazza, D. P., Salvaterra, R., Chincarini, G. L., Margutti, R., Wu, X.-F., Thöne, C. C., Fernández-Soto, A., Ukwatta, T. N., et al. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201014801 · Cited by 22
Self-citationLate Central-engine Activity in GRB 180205A
Becerra, R. L., Watson, A. M., Fraija, N., Butler, N., Lee, W. H., Troja, E., Román-Zúñiga, C. G., Kutyrev, A. S., Nuñez, L. C. Á., Ángeles, F., et al. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab0026 · Cited by 22
“…of the core associated to the progenitor during the collapse (King et al. 2005), rupture of the accretion disk due to gravitational instability at large radii in different time intervals (Proga & Zhang 2006; Perna et al. 2006) and a neutron star with differential rotation (Dai et al. 2006).”
BackgroundSelf-organized criticality in multi-pulse gamma-ray bursts
Lyu, F., Li, Y.-P., Hou, S.-J., Wei, J.-J., Geng, J.-J., & Wu, X.-F. (2020) · Frontiers of Physics · doi:10.1007/s11467-020-0989-x · Cited by 22
Gamma ray burst studies with THESEUS
Ghirlanda, G., Salvaterra, R., Toffano, M., Ronchini, S., Guidorzi, C., Oganesyan, G., Ascenzi, S., Bernardini, M. G., Camisasca, A. E., Mereghetti, S., et al. (2021) · Experimental Astronomy · doi:10.1007/s10686-021-09763-3 · Cited by 22
Gupta, R., Oates, S. R., Pandey, S. B., Castro-Tirado, A. J., Joshi, J. C., Hu, Y. D., Valeev, A. F., Zhang, B., Zhang, Z., Kumar, A., et al. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1573 · Cited by 22
Self-citationVery High Energy Observations of Gamma‐Ray Burst Locations with the Whipple Telescope
Horan, D., Atkins, R. W., Badran, H. M., Blaylock, G., Bradbury, S. M., Buckley, J. H., Byrum, K. L., Celik, O., Chow, Y. C. K., Cogan, P., et al. (2007) · The Astrophysical Journal · doi:10.1086/509567 · Cited by 22
Perri, M., Guetta, D., Antonelli, L. A., Cucchiara, A., Mangano, V., Reeves, J., Angelini, L., Beardmore, A. P., Boyd, P., Burrows, D. N., et al. (2007) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20066227 · Cited by 22
Self-citationGamma-ray bursts in the Swift era
O'Brien, P. T., & Willingale, R. (2007) · Astrophysics and Space Science · doi:10.1007/s10509-007-9551-3 · Cited by 22
GLASTProspects forSwift‐Era Afterglows
Gou, L. ‐., & Meszaros, P. (2007) · The Astrophysical Journal · doi:10.1086/521045 · Cited by 22
Self-citationTesting a new view of Gamma Ray Burst AfterglowsPreprint
Nardini, M., Ghisellini, G., Ghirl, G., & Celotti, A. (2009) · Cited by 21
Inferring the Redshift of More than 150 GRBs with a Machine-learning Ensemble Model
Dainotti, M. G., Taira, E., Wang, E., Lehman, E., Narendra, A., Pollo, A., Madejski, G. M., Petrosian, V., Bogdan, M., Dey, A., et al. (2024) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/ad1aaf · Cited by 21
“The afterglow sometimes contains the plateau emission feature where the flux during the plateau remains constant (Nousek et al. 2006; Rowlinson et al. 2014; Zhang et al. 2006; Dainotti et al. 2008; Sakamoto et al. 2007; O’Brien et al. 2006; Zaninoni et al. 2013; Liang et al. 2007).”
BackgroundOn the duration of gamma-ray bursts
Zhang, B. (2025) · Journal of High Energy Astrophysics · doi:10.1016/j.jheap.2024.12.013 · Cited by 21
Self-citationO’Connor, B., Pasham, D. R., Andreoni, I., Hare, J., Beniamini, P., Troja, E., Ricci, R., Dobie, D., Chakraborty, J., Ng, M., et al. (2025) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ada7f5 · Cited by 21
“For instance, many GRBs exhibit an extended plateau phase following the prompt emission, lasting from a few hundred seconds to several hours before rapidly declining in X-rays (e.g., Zhang et al. 2006; Troja et al. 2007; Rowlinson et al. 2010).”
InfluentialLenart, A. Ł., Dainotti, M. G., Khatiya, N. S., Bal, D., Hartmann, D. H., Fraija, N. I., & Zhang, B. (2025) · Journal of High Energy Astrophysics · doi:10.1016/j.jheap.2025.100384 · Cited by 21
“…light curves, such as the “plateau phase," where the luminosity of the afterglow remains nearly constant for a period before decaying more rapidly (Zhang et al., 2006; Nousek et al., 2006; Evans et al., 2007; O’Brien et al., 2006; Willingale et al., 2007; Zhang et al., 2007; Liang et al., 2007;…”
Self-citationZhang, B., Lü, H.-J., & Liang, E. (2016) · Space Science Reviews · doi:10.1007/s11214-016-0305-9 · Cited by 21
“These plateaus can be understood within the standard external shock model with continuous energy injection into the blastwave (Zhang et al. 2006; Nousek et al. 2006; Rees and Mészáros 1998; Dai and Lu 1998c,a; Zhang and Yan 2011; Yu and Dai 2007).”
BackgroundInfluentialSelf-citationGRB 140423A: A Case of Stellar Wind to Interstellar Medium Transition in the Afterglow
Li, L., Wang, X.-G., Zheng, W., Pozanenko, A. S., Filippenko, A. V., Qin, S., Wang, S.-Q., Jiang, L.-Y., Li, J., Lin, D.-B., et al. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/aba757 · Cited by 21
A blast from the infant Universe: The very high-zGRB 210905A
Rossi, A., Frederiks, D. D., Kann, D. A., de Pasquale, M., Pian, E., Lamb, G. P., D’Avanzo, P., Izzo, L., Levan, A. J., Malesani, D. B., et al. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202243225 · Cited by 21
Xin, L. P., Han, X. H., Li, H.-L., Zhang, B., Wang, J., Turpin, D., Yang, X., Qiu, Y., Liang, E., Dai, Z.-G., et al. (2023) · Nature Astronomy · doi:10.1038/s41550-023-01930-0 · Cited by 21
Self-citationSwiftObservations of GRB 050603: An Afterglow with a Steep Late‐Time Decay Slope
Grupe, D., Brown, P. J., Cummings, J., Zhang, B., Retter, A., Burrows, D. N., Boyd, P. T., Capalbi, M., Gehrels, N., Holland, S. T., et al. (2006) · The Astrophysical Journal · doi:10.1086/504315 · Cited by 21
Self-citationGao, H., & Mészáros, P. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/802/2/90 · Cited by 21
“…Tce, since Swift observations suggest that many GRBs have an extended central engine activity time, manifested through flares (Burrows et al. 2005a; Zhang et al. 2006; Margutti et al. 2011) and extended shallow plateaus (Liang et al. 2007; Troja et al. 2007) in the X-ray light curves following the…”
BackgroundThe plateau of gamma-ray burst: hint for the solidification of quark matter?
Dai, S., Li, L., & Xu, R. (2011) · Science China Physics Mechanics and Astronomy · doi:10.1007/s11433-011-4384-z · Cited by 21
THE ORIGIN OF THE PLATEAU AND LATE REBRIGHTENING IN THE AFTERGLOW OF GRB 120326A
Hou, S. J., Geng, J. J., Wang, K., Wu, X. F., Huang, Y. F., Dai, Z. G., & Lu, J. F. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/785/2/113 · Cited by 21
“To summarize the X-ray afterglow data, a canonical X-ray afterglow light curve includes five components (Zhang et al. 2006; Nousek et al. 2006): a steep decay phase (Zhang et al. 2007, 2009), a shallow decay phase (Liang et al. 2007), a normal decay phase (Willingale et al. 2007), a post-jet break…”
BackgroundInfluentialChallenging gamma-ray burst models through the broadband dataset of GRB 060908
Covino, S., Campana, S., Conciatore, M. L., D'Elia, V., Palazzi, E., Thöne, C. C., Vergani, S. D., Wiersema, K., Brusasca, M., Cucchiara, A., et al. (2010) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201014994/pdf · Cited by 21
Racusin, J. L., Oates, S. R., de Pasquale, M., & Kocevski, D. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/826/1/45 · Cited by 21
“We look at a >X,avg, 200 s and L200 s in the context of the closure relations (Panaitescu et al. 2006; Zhang et al. 2006; Racusin et al. 2009), adding the spectral energy index (bx) for the standard forward shock (Figure 15).”
BackgroundMethodInfluentialThe Late-time Afterglow Evolution of Long Gamma-Ray Bursts GRB 160625B and GRB 160509A
Kangas, T., Fruchter, A. S., Cenko, S. B., Corsi, A., Postigo, A. D. U., Pe’er, A., Vogel, S. N., Cucchiara, A., Gompertz, B. P., Graham, J. F., et al. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab8799 · Cited by 21
Rise and fall of the high-energy afterglow emission of GRB 180720B
Ronchi, M., Fumagalli, F., Ravasio, M. E., Oganesyan, G., Toffano, M., Salafia, O. S., Nava, L., Ascenzi, S., Ghirlanda, G., & Ghisellini, G. (2020) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201936765/pdf · Cited by 21
Gamma-Ray Burst/Supernova Associations: Energy Partition and the Case of a Magnetar Central Engine
Lü, H.-J., Lan, L., Zhang, B., Liang, E., Kann, D. A., Du, S.-S., & Shen, J. (2018) · Digital Scholarship - UNLV (University of Nevada Reno) · Cited by 21
Self-citationGRB 170817A as a Refreshed Shock Afterglow viewed off-axis
Lamb, G. P., Levan, A. J., & Tanvir, N. R. (2020) · Figshare · Cited by 21
The Rate of Short-Duration Gamma-Ray Bursts in the Local Universe
(7744511), S. M., (7660679), N. T., (7744514), G. L., (7660652), A. L., & (7744517), D. T. (2018) · Figshare · Cited by 21
X-ray flares of γ-ray bursts: Quakes of solid quark stars?
Xu, R., & Liang, E. (2009) · Science in China. Series G, Physics, mechanics & astronomy/Science in China. Series G, Physics, Mechanics & Astronomy · doi:10.1007/s11433-009-0045-x · Cited by 21
Early multi-wavelength emission from gamma-ray bursts: from gamma-ray to x-ray
O'Brien, P. T., Willingale, R., Osborne, J. P., & Goad, M. R. (2006) · New Journal of Physics · doi:10.1088/1367-2630/8/7/121 · Cited by 21
VegasAfterglow: A high-performance framework for gamma-ray burst afterglows
Wang, Y., Chen, C., & Zhang, B. T. (2025) · Journal of High Energy Astrophysics · doi:10.1016/j.jheap.2025.100490 · Cited by 20
“The energy injection mechanism was proposed for modeling the afterglow emission of some GRBs that showed plateau features (Dai and Lu, 1998a; Zhang and Mészáros, 2001a; Zhang et al., 2006; Nousek et al., 2006; Lü et al., 2015).”
Self-citationIS THE LATE NEAR-INFRARED BUMP IN SHORT-HARD GRB 130603B DUE TO THE LI-PACZYNSKI KILONOVA?
Jin, Z.-P., Xu, D., Fan, Y.-Z., Wu, X.-F., & Wei, D.-M. (2013) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/775/1/l19 · Cited by 20
“The code used here has been developed in Fan & Piran (2006) and Zhang et al. (2006).”
MethodSelf-citationSynchrotron Self-Compton Afterglow Closure Relations and Fermi-LAT-detected Gamma-Ray Bursts
Fraija, N. I., Dainotti, M. G., Ugale, S., Jyoti, D., & Warren, D. C. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac7a9c · Cited by 20
“A continuous luminosity of the central engine can be described by Linj(t)∝ L0 t − q where q is the energy injection index and Linj is the luminosity injected into the blast wave (e.g., Zhang et al. 2006).”
BackgroundA Short Gamma-Ray Burst from a Protomagnetar Remnant
Jordana-Mitjans, N., Mundell, C. G., Guidorzi, C., Smith, R. J., Ramirez-Ruiz, E., Metzger, B. D., Kobayashi, S., Gomboc, A., Steele, I. A., Shrestha, M., et al. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac972b · Cited by 20
“…and spectral evolution of the optical emission (Δαopt= 4.2, Δβopt= 3.3; see Figure 2) are hard to explain just in terms of the flaring activity (i.e., Δt/ t> 1; Zhang et al. 2006) or the external shock from the decelerating relativistic ejecta (i.e., the afterglow; Piran 1999; Kobayashi 2000).”
BackgroundInfluentialSelf-citationProbing gamma-ray burst environments with time variability: ULTRASPEC fast imaging of GRB 080210★
Cia, A. D., Jakobsson, P., Björnsson, G., Vreeswijk, P. M., Dhillon, V. S., Marsh, T. R., Chapman, R., Fynbo, J. P. U., Ledoux, C., Littlefair, S. P., et al. (2011) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2010.18046.x · Cited by 20
Li, X., Zhou, B., He, H.-N., Fan, Y.-Z., & Wei, D.-M. (2014) · The Astrophysical Journal · doi:10.1088/0004-637x/797/1/33 · Cited by 20
“…wind energy will be transferred into the kinetic energy of the outflow, as indicated by the shallow decay of some GRB afterglows (Dai & Lu 1998a, 1998b; Zhang et al. 2006) and the light curves of some superluminous SNe (Kasen & Bildsten 2010; Woosley 2010; Inserra et al. 2013; Nicholl et al. 2013).”
Self-citationA MAD model for gamma-ray burst variability
Lloyd-Ronning, N., Dolence, J. C., & Fryer, C. L. (2016) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stw1366 · Cited by 20
“…have attributed this to late time activity of the central engine, based on, for example, similarities between some of the spectral and timing properties of the flares and the prompt emission (Burrows et al 2005, Fan & Wei 2005, Zhang et al. 2006, Margutti, et al. 2011, Guidorzi et al. 2015).”
BackgroundZou, L., Zhou, Z.-M., Xie, L., Zhang, L.-L., Lü, H.-J., Zhong, S.-Q., Wang, Z.-J., & Liang, E.-W. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab17dc · Cited by 20
Is GRB 110715A the Progenitor of FRB 171209?
Wang, X.-G., Li, L., Yang, Y.-P., Luo, J.-W., Zhang, B., Lin, D.-B., Liang, E., & Qin, S. (2020) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ab8d1d · Cited by 20
“For the shallow decay phase closure relation α = q/2 + (2 + q)β/2 (Zhang et al. 2006), we obtained the energy injection parameter q = 0 for αX,I = 0.70 +0.04 −0.05 and αO,I = 0.70 +0.13 −0.12, which is consistent with the energy injection from the spin-down of a millisecond magnetar (Dai & Lu 1998;…”
MethodInfluentialSelf-citationMoin, A., Chandra, P., Miller-Jones, J. C. A., Tingay, S. J., Taylor, G. B., Frail, D. A., Wang, Z., Reynolds, C., & Phillips, C. J. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/779/2/105 · Cited by 20
“This energy is 100 times the initial isotropic energy (Ek,iso,i ∼10 51; Marshall et al. 2011) and is thought to be continuously injected into the forward shock, which then produced a long-term, slowly varying afterglow (Dai & Lu 1998; Zhang & Meszaros 2001; Zhang et al. 2006).”
BackgroundResultInfluentialAdiabatic expansion, early X-ray data and the central engine in GRBs
Duran, R. B., & Kumar, P. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.14584.x · Cited by 20
OFF-AXIS PROPERTIES OF SHORT GAMMA-RAY BURSTSPreprint
Janka, H. T., Aloy, M. Á., Mazzali, P. A., & Pian, E. (2005) · Cited by 20
GRB 180620A: Evidence for Late-time Energy Injection
Becerra, R. L., Colle, F. D., Watson, A. M., Fraija, N., Butler, N., Lee, W. H., Román-Zúñiga, C. G., Bloom, J. S., González, J. J., Kutyrev, A. S., et al. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab5859 · Cited by 19
Yu, Y.-W., Gao, H., Wang, F. Y., & Zhang, B. (2022) · Springer eBooks · doi:10.1007/978-981-16-4544-0_126-1 · Cited by 19
Self-citationSchroeder, G., Rhodes, L., Laskar, T., Nugent, A. E., Escorial, A. R., Rastinejad, J., Fong, W., van der Horst, A. J., Vereš, P., Alexander, K. D., et al. (2024) · The Astrophysical Journal · doi:10.3847/1538-4357/ad49ab · Cited by 19
“The flux evolution The afterglow of short GRB 210726A when ν obs < ν m should follow F ν ∝ t (3+5 m ) / 6 (see table 2 of Zhang et al. 2006).”
BackgroundThe swift x-ray telescope: status and performance
Burrows, D. N., Kennea, J. A., Abbey, A. F., Beardmore, A. P., Campana, S., Capalbi, M., Chincarini, G. L., Cusumano, G., Evans, P. A., Hill, J. E., et al. (2007) · Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE · doi:10.1117/12.735130 · Cited by 19
Self-citationSw 1644+57/GRB 110328A: THE PHYSICAL ORIGIN AND THE COMPOSITION OF THE RELATIVISTIC OUTFLOW
Shao, L., Zhang, F.-W., Fan, Y.-Z., & Wei, D.-M. (2011) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/734/2/l33 · Cited by 19
Self-citationHow Swift is redefining time domain astronomy
Gehrels, N. A., & Cannizzo, J. K. (2015) · Journal of High Energy Astrophysics · doi:10.1016/j.jheap.2015.03.003 · Cited by 19
“By the time Swift had discovered a handful of GRBs and their XRT X-ray light curves were studied in detail, several basic features became obvious (Zhang et al. 2006; Nousek et al. 2006; O’Brien et al. 2006).”
BackgroundSelf-citationDermer, C. D. (2008) · The Astrophysical Journal · doi:10.1086/589730 · Cited by 19
Linking extended and plateau emissions of short gamma-ray bursts
Matsumoto, T., Kimura, S. S., Murase, K., & Mészáros, P. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa305 · Cited by 19
Shallow Decay of X-ray Afterglows in Short GRBs: Energy Injection from a Millisecond Magnetar?
Yu, Y., & Huang, Y.-F. (2007) · 天文和天体物理学研究：英文版 · doi:10.1088/1009-9271/7/5/07 · Cited by 19
“…curve in the X-ray band, one at tc when the injected energy roughly equals to its initial kinetic energy and one at t f when the energy injection is turned off (Dai & Lu 1998a; Zhang & Mészáros 2001; Zhang et al. 2006), where tf is roughly equal to the spin-down time scale TM,0 of the magnetar.”
BackgroundOptical observations of GRB 050401 afterglow : a case for double-jet model
Kamble, A., Misra, K., Bhattacharya, D., & Sagar, R. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2008.13504.x · Cited by 19
“While there is no clear understanding of the early steep decays of GRB afterglows, a few plausible explanations have been put forward : see e.g. Zhang et al. (2006); Pe’er et al. (2006).”
BackgroundX-ray flares from dense shells formed in gamma-ray burst explosions
Hascoët, R., Beloborodov, A. M., Daigne, F., & Mochkovitch, R. (2017) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slx143 · Cited by 19
“…X-ray flares motivated several authors to invoke late activity of the central engine and associate the flares with the jet produced by this actvity — a scaled-down version of the prompt GRB emission (e.g. ⋆ E-mail: hascoet@astro.columbia.edu Burrows et al. 2005a; Fan & Wei 2005; Zhang et al. 2006).”
BackgroundX‐Ray Afterglow Light Curves: Toward A Standard Candle?
Gendre, B., Galli, A., & Boër, M. (2008) · The Astrophysical Journal · doi:10.1086/589805 · Cited by 19
The initial Lorentz factors of fireballs inferred from the early X-ray data of SWIFT GRBs
Xue, R. R., Fan, Y.-Z., & Wei, D.-M. (2009) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/200811361/pdf · Cited by 19
Self-citationAnatomy of a dark burst - the afterglow of GRB 060108
Oates, S. R., Mundell, C. G., Piranomonte, S., Page, K. L., de Pasquale, M., Monfardini, A., Melandri, A., Zane, S., Guidorzi, C., Malesani, D., et al. (2006) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2006.10866.x · Cited by 19
“Such X-ray flares are common features of Swift XRT light curves (Liang et al. 2006; Zhang et al. 2006), and are usually associated with collisions between ultrarelativistic shells emitted by the ‘inner engine’ after the main high-energy event.”
BackgroundMethodInfluentialSelf-citationGRB 070518: a gamma-ray burst with optically dim luminosity
Xin, L. P., Zheng, W., Wang, J., Deng, J. S., Urata, Y., Qiu, Y., Huang, K. Y., Hu, J. Y., & Wei, J. (2009) · Monthly Notices of the Royal Astronomical Society · doi:10.1111/j.1365-2966.2009.15788.x · Cited by 18
“Moreover, such dramatic flares are also related to refreshed shocks or the central engine activity (e.g. Zhang et al. 2006).”
BackgroundMethodInfluentialProbing Magnetic Fields of GRB X-Ray Flares with Polarization Observations
Geng, J.-J., Huang, Y.-F., Wu, X.-F., Song, L.-M., & Zong, H.-S. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aacd05 · Cited by 18
“Some flares show clear rapid rise and steep decay structures superposed on the underlying afterglow (Zhang et al. 2006) and their durations are typically ∼ 102 − 103 s.”
BackgroundThe ultra-long GRB 220627A at z = 3.08
de Wet, S., Izzo, L., Groot, P., Bisero, S., D'Elia, V., de Pasquale, M., Hartmann, D. H., Heintz, K. E., Jakobsson, P., Laskar, T., et al. (2023) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202347017 · Cited by 18
Gamma rays from a reverse shock with turbulent magnetic fields in GRB 180720B
Arimoto, M., Asano, K., Kawabata, K. S., Toma, K., Gill, R., Granot, J., Ohno, M., Takahashi, S., Ogino, N., Goto, H., et al. (2023) · Nature Astronomy · doi:10.1038/s41550-023-02119-1 · Cited by 18
“One of the possible origins is energy injection from a central engine[33, 34], which makes the forward shock emission decay more slowly.”
BackgroundInfluentialGRB 051008: a long, spectrally hard dust-obscured GRB in a Lyman-break galaxy at z ≈ 2.8★
Volnova, A. A., Pozanenko, A. S., Gorosabel, J., Perley, D. A., Frederiks, D. D., Kann, D. A., Rumyantsev, V., Biryukov, V. V., Burkhonov, O. A., Castro-Tirado, A. J., et al. (2014) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stu999 · Cited by 18
The Full Curvature Effect Expected in Early X‐Ray Afterglow Emission from Gamma‐Ray Bursts
Qin, Y. (2008) · The Astrophysical Journal · doi:10.1086/589277 · Cited by 18
“Generally, the steep decay phase was interpreted as a consequence of the so-called curvature effect (Fenimore et al. 1996; Kumar & Panaitescu 2000; Dermer 2004; Dyks et al. 2005; Butler & Kocevski 2007a; Liang et al. 2006; Panaitescu et al. 2006; Zhang et al. 2006; Zhang et al. 2007).”
BackgroundVERY HIGH ENERGY γ-RAY AFTERGLOW EMISSION OF NEARBY GAMMA-RAY BURSTS
Xue, R. R., Tam, P. H. T., Wagner, S. J., Behera, B., Fan, Y.-Z., & Wei, D. M. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/703/1/60 · Cited by 18
Self-citationX-ray afterglow light curves: toward a standard candle?
Gendre, B., Galli, A., Boër, M., Galassi, M., Palmer, D., & Fenimore, E. (2008) · AIP conference proceedings · doi:10.1063/1.2943553 · Cited by 18
Lei, W., Wang, D.-X., Zou, Y.-C., & Zhang, L. (2008) · 天文和天体物理学研究：英文版 · doi:10.1088/1009-9271/8/4/04 · Cited by 18
On the lack of a radio afterglow from some gamma-ray bursts – insight into their progenitors?
Lloyd-Ronning, N., & Fryer, C. L. (2017) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stx313 · Cited by 18
“…light curves of GRBs has also been studied extensively and used to help discern the nature of the GRB emission and connect it to the progenitor (e.g., Swenson & Roming 2014, Burrows et al. 2005, Fan & Wei 2005, Zhang et al. 2006, Margutti, et al. 2011, Guidorzi et al. 2015, Greiner et al. 2016).”
BackgroundA Large Catalog of Homogeneous Ultra-Violet/Optical GRB Afterglows: Temporal and Spectral Evolution
Roming, P. W. A., Koch, T. S., Oates, S. R., Porterfield, B. L., Bayless, A. J., Breeveld, A. A., Gronwall, C. A., Kuin, N. P. M., Page, M. J., de Pasquale, M., et al. (2017) · The Astrophysical Journal Supplement Series · doi:10.3847/1538-4365/228/2/13 · Cited by 18
“Time-dependent UV/optical and X-ray temporal and spectral slopes would also help validate and further constrain GRB afterglow models (cf. Zhang & Mészáros 2004; Zhang et al. 2006).”
BackgroundNew three-parameter correlation for gamma-ray bursts with a plateau phase in the afterglow
Xu, M., & Huang, Y.-F. (2012) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201117754/pdf · Cited by 18
GRB 081008: From Burst To Afterglow And The Transition Phase In Between
Yuan, F., Schady, P., Racusin, J. L., Willingale, R., Kruehler, T., O'Brien, P. T., Greiner, J., Oates, S. R., Rykoff, E. S., Aharonian, F., et al. (2010) · Sabanci University · doi:10.15781/t26f9t · Cited by 18
Self-citationGamma-ray burst high energy emission from internal shocks
Galli, A., & Guetta, D. (2008) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20078518 · Cited by 18
Constraints on the Cosmological Parameters with Three-Parameter Correlation of Gamma-Ray Bursts
Li, J.-L., Yang, Y., Yi, S.-X., Hu, J.-P., Wang, F. Y., & Qu, Y.-K. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/ace107 · Cited by 17
“…the observations of Swift (Gehrels et al. 2004), a significant fraction of GRBs show a plateau phase in the X-ray light curves that is followed by a decay phase in the afterglows (Nousek et al. 2006; O’Brien et al. 2006; Zhang et al. 2006; Liang et al. 2007; Yi et al. 2015, 2016; Li et al. 2023b).”
BackgroundQuirola-Vásquez, J., Bauer, F. E., Jonker, P. G., Brandt, W. N., Eappachen, D., Levan, A. J., López, E., Luo, B., Ravasio, M. E., Sun, H., et al. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202347629 · Cited by 17
Long-term Radio Monitoring of the Fast X-Ray Transient EP 240315a: Evidence for a Relativistic Jet
Ricci, R., Troja, E., Yang, Y.-H., Yadav, M., Liu, Y., Sun, H., Wu, X.-F., Gao, H., Zhang, B., & Yuan, W. (2025) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ad8b3f · Cited by 17
“…sudden rebrightenings of low-energy ( < 10 keV) radiation that follow many GRBs, suggested instead that the central engine could remain active on much longer timescales than the observed GRB duration (Fan & Wei 2005; Zhang et al. 2006; Liang et al. 2006; Lazzati & Perna 2007; Maxham & Zhang 2009).”
Self-citationReverse Shock Emission in Gamma-Ray Bursts Revisited
Gao, H., & Mészáros, P. (2015) · Advances in Astronomy · doi:10.1155/2015/192383 · Cited by 17
“It was found that a number of physical processes are needed to shape the observed lightcurves [30, 31], including, for example, the suggestion that the X-ray afterglow is a superposition of the conventional external shock component and a radiation component that is related to the late central engine activity [4, 29, 3…”
BackgroundORIGIN OF THE GeV EMISSION DURING THE X-RAY FLARING ACTIVITY IN GRB 100728A
He, H.-N., Zhang, B., Wang, X., Li, Z., & Mészáros, P. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/753/2/178 · Cited by 17
“One of the key discoveries by theSwift satellite is the presence of X-ray flares during the early afterglow phase in a large fraction of gamma-ray bursts (GRBs) (see, e.g., Burrows et al. 2005; Zhang et al. 2006; Nousek et al. 2006).”
BackgroundSelf-citationON THE RECENTLY DISCOVERED CORRELATIONS BETWEEN GAMMA-RAY AND X-RAY PROPERTIES OF GAMMA-RAY BURSTS
Dado, S., & Arnon Dar, A. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/775/1/16 · Cited by 17
“…20 θ2)2 t0, γ (t) and δ(t) change rather slowly with t, which generates the plateau phase of Fν(t) of canonical X-ray AGs that was predicted by the CB model (see, e.g., Dado et al. 2002, Figures 27–33) and later observed with Swift (Nousek et al. 2006; Panaitescu et al. 2006; Zhang et al. 2006).”
BackgroundGRB 071112C: A CASE STUDY OF DIFFERENT MECHANISMS IN X-RAY AND OPTICAL TEMPORAL EVOLUTION
Huang, K. Y., Urata, Y., Tung, Y. H., Lin, H., Xin, L. P., Yoshida, M., Zheng, W., Akerlof, C. W., Wang, S., Ip, W.-H., et al. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/748/1/44 · Cited by 17
“Although the rising part in the R band was not visible in our measurements, the short duration peak in GRB 071112C implies that it is unlikely an example of the long-lasting plateau feature of long-lived GRBs (Zhang et al. 2006; Panaitescu & Vestrand 2008).”
BackgroundInfluentialSimulation and physical model based gamma-ray burst afterglow analysis
van Eerten, H. (2015) · Journal of High Energy Astrophysics · doi:10.1016/j.jheap.2015.04.004 · Cited by 15
The optical rebrightening of GRB100814A: an interplay of forward and reverse shocks?
de Pasquale, M., Kuin, N. P. M., Oates, S. R., Schulze, S., Cano, Z., Guidorzi, C., Beardmore, A. P., Evans, P. A., Uhm, Z. L., Zhang, B., et al. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv267 · Cited by 17
“The energy of the blast wave increases with time as E ∝ t1 − q, where q is linked to the parameter s (Zhang et al. 2006).”
BackgroundInfluentialSelf-citationMAGIC observation of the GRB 080430 afterglow
Aleksić, J., Anderhub, H., Antonelli, L. A., Antoranz, P., Backes, M., Baixeras-Aiguabella, C., Balestra, S., Barrio, J. A., Bastieri, D., González, J. B., et al. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200913461 · Cited by 17
“A shallower afterglow decay showing a synchrotron spectrum can be explained with late-time energy injection in the outflow (Panaitescu 2006; Zhang et al. 2006).”
BackgroundGRB 120729A: External Shock Origin for Both the Prompt Gamma-Ray Emission and Afterglow
Huang, L.-Y., Wang, X.-G., Zheng, W., Liang, E.-W., Lin, D.-B., Zhong, S.-Q., Zhang, H.-M., Huang, X.-L., Filippenko, A. V., & Zhang, B. (2018) · The Astrophysical Journal · doi:10.3847/1538-4357/aaba6e · Cited by 17
“…observed light curves have an achromatic behavior, consistent with the predictions of the external forward shock models with energy injection in the thin-shell case (Zhang et al. 2006; Li et al. 2012), suggesting that both the prompt γ-ray emission and the afterglow have the same physical origin.”
BackgroundResultSelf-citationEnergy Injection Driven by Precessing Jets in Gamma-Ray Burst Afterglows
Huang, B.-Q., & Liu, T. (2021) · The Astrophysical Journal · doi:10.3847/1538-4357/ac07a0 · Cited by 17
Oates, S. R., Racusin, J. L., de Pasquale, M., Page, M. J., Castro-Tirado, A. J., Gorosabel, J., Smith, P. J., Breeveld, A. A., & Kuin, N. P. M. (2015) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stv1956 · Cited by 17
“This steep decay segment is likely the tail of the prompt emission (Zhang et al. 2006).”
BackgroundTHE INTERPRETATION OF THE MULTI-WAVELENGTH AFTERGLOW EMISSION OF SHORT GRB 140903A
Zhang, S., Jin, Z.-P., Wang, Y.-Z., & Wei, D.-M. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/835/1/73 · Cited by 17
“In this case, the X-ray flat plateau decline as α = (2p−4)+(p+2)q4 (Zhang et al. 2006).”
BackgroundInfluentialA Study of GRBs with Low-luminosity Afterglows
Dereli, H., Boër, M., Gendre, B., Amati, L., Dichiara, S., & Orange, N. B. (2017) · The Astrophysical Journal · doi:10.3847/1538-4357/aa947d · Cited by 17
“…their light curve can be described as a steep-flat-steep broken power law (Nousek et al. 2006), whose first part (the steep decay) has been associated with the prompt phase (Barthelmy et al. 2005; Tagliaferri et al. 2005; Zhang et al. 2006; Willingale et al. 2007), through high latitude emission.”
BackgroundEarly multi-wavelength emission from Gamma-ray Bursts: from Gamma-ray to X-ray
O'Brien, P. T., Willingale, R., Osborne, J. P., & Goad, M. R. (2006) · Figshare · Cited by 17
The Closure Relations in Optical Afterglow of Gamma-Ray Bursts
Dainotti, M. G., Levine, D., Fraija, N. I., Warren, D. C., & Sourav, S. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac9b11 · Cited by 16
“…the prompt emission and preceding the afterglow decay, has been found in all wavelengths of the GRB after-glow, including X-ray (O’Brien et al. 2006; Zhang et al. 2006b; Nousek et al. 2006; Sakamoto et al. 2007; Evans et al. 2009), optical (Dainotti et al. 2020b, 2022a), and radio (Levine et al.…”
BackgroundMethodInfluentialLong-duration Gamma-Ray Burst Progenitors and Magnetar Formation
Song, C.-Y., & Liu, T. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/acd6ee · Cited by 16
“The shallow decay phase (Dai 2004; Zhang et al. 2006; Dall’Osso et al. 2011; Li et al. 2016) and “internal plateau” (Troja et al. 2007; Lyons et al. 2010; Stratta et al. 2018) in some GRB afterglow light curves have been proposed as the magnetar signature, but the BH hyperaccretion model cannot be…”
BackgroundZhong, S.-Q., Li, L., Xiao, D., Sun, H., Zhang, B., & Dai, Z.-G. (2024) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ad2852 · Cited by 16
“External plateaus are interpreted as the decelerating external forward shock by introducing: continuous energy injection from the central engine (Dai & Lu 1998a,b; Zhang & M´esz´aros 2001; Rees & M´esz´aros 1998; Sari & M´esz´aros 2000; Zhang et al. 2006), a two-component jet (Racusin et al. 2008), a reverse shock (Uh…”
BackgroundSelf-citationGamma-ray burst redshift estimation using machine learning and the associated web app
Narendra, A., Dainotti, M. G., Sarkar, M., Lenart, A. Ł., Bogdan, M., Pollo, A., Zhang, B., Rabeda, A., Petrosian, V., & Iwasaki, K. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202452651 · Cited by 16
Self-citationInduced gravitational collapse at extreme cosmological distances: the case of GRB 090423
RUFFINI, R. J., Izzo, L., Muccino, M., Pisani, G. B., Rueda, J. A., Wang, Y., Barbarino, C., Bianco, C. L., Enderli, M., & Kovacevic, M. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201423457 · Cited by 16
“That in long GRBs the X-ray emission, observed by Swift-XRT in energy range 0.3–10 keV, presents a typical structure composed of a steep decay, a plateau phase and a late power-law decay, was clearly expressed by Nousek, Zhang and their collaborators (Nousek et al. 2006; Zhang et al. 2006).”
BackgroundInfluentialGRB 060206: hints of precession of the central engine?
Liu, X. W., Wu, X.-F., & Lu, T. (2008) · Astronomy and Astrophysics · doi:10.1051/0004-6361:20078783 · Cited by 16
Mao, Z., Yu, Y.-W., Dai, Z.-G., Pi, C., & Zheng, X. (2010) · Astronomy and Astrophysics · doi:10.1051/0004-6361/200913252 · Cited by 16
Metadata
- Authors
- Zhang, B., Fan, Y. Z., Dyks, J., Kobayashi, S., Meszaros, P., Burrows, D. N., Nousek, J. A., & Gehrels, N.
- Affiliations
- University of Nevada, Las Vegas (US)
- Pennsylvania State University (US)
- Goddard Space Flight Center (US)
- Venue
- The Astrophysical Journal
- Publisher
- American Astronomical Society
- Published
- 2006-05
- Volume
- 642
- Issue
- 1
- Pages
- 354-370
- ISSN
- 0004-637X (ISSN-L)
- 1538-4357
- OpenAlex
- W2078391322
- Cited by
- 1,079
- References
- 155
- Citations by year
- 2026: 46 · 2025: 67 · 2024: 52 · 2023: 48 · 2022: 51 · 2021: 35 · 2020: 47 · 2019: 40 · 2018: 36 · 2017: 38 · 2016: 52 · 2015: 51 · 2014: 50 · 2013: 52 · 2012: 47
- FWCI
- 51.93
- Type
- journal article
- Language
- en
- Open access
- bronze
- doi.org
- Locations
- The Astrophysical Journal (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- CERN Document Server (European Organization for Nuclear Research) (submittedVersion)
- arXiv (Cornell University)
- Funders
- National Science Foundation (0114375, 0307376)
- National Aeronautics and Space Administration (NAS5-00136)
- University of Pennsylvania
- Pennsylvania State University (NAS5-00136)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Gamma-ray bursts and supernovae
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Astrophysics and Cosmic Phenomena
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astrophysical Phenomena and Observations
- Keywords
- gamma-ray bursts, X-ray afterglow, afterglow light curves, Swift X-ray Telescope, X-ray flares, prompt gamma-ray emission, central engine, forward shock, relativistic outflows, Poynting flux, interstellar medium, afterglow decay
About these checks
Registry, retraction, Cites and statistics results are computed, not judged, with one exception: a printed reference that no index lists is read once by a model before it counts as a citation error. Claims are extracted by a model and kept only when their quote appears verbatim in the text; each cited source is then checked, with a model’s help, for whether it says what the claim relies on. Those verdicts can be wrong — read the claim’s quote and the cited source before relying on one.
Statistics and arithmetic are recomputed, not judged.
Confidence bands are shown only for fields calibrated on our annotated test set. None is calibrated yet, so no band is shown.
What counts as a claim ›How we measure confidence ›How we check this ›
Are you an author, or do you see a problem with this page? Request a review
