Persistent Counterparts to Gamma‐Ray Bursts

Katz, J. I.; Piran, Tsvi

doi:10.1086/304913

Cited by 120 publications

(130 citation statements)

References 22 publications

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“…However, the very steep spectrum and the very weak radio afterglow rule out an external shock origin (both form synchrotron radiation and from inverse Compton emission). We suggest following the earlier suggestion of Katz & Piran [13] and Katz, Piran & Sari [21] that this emission arises due to continued activity of the central engine. This is the first time that a power-law decaying X-ray afterglow is attributed to the activity of the central engine, though it has been suggested by Fan & Wei [23] and Zhang et al [24] that the flare-rich X-ray afterglow that have been detected in a good fraction of Swift GRBs [22] also trace the long term activity of the central engine.…”

Section: Discussion and Summarysupporting

confidence: 72%

The interpretation and implication of the afterglow of GRB 060218

Fan

Piran²,

Xu³

2006

J. Cosmol. Astropart. Phys.

121

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Abstract. The nearby GRB 060216/SN 2006aj was an extremely long, weak and very soft GRB. It was peculiar in many aspects. We show here that the X-ray, ultraviolet/optical and radio afterglow of GRB 060218 have to be attributed to different physical processes arising from different emission regions. From the several components in this burst's afterglow only the radio afterglow can be interpreted in terms of the common external shock model. We infer from the radio that the blast wave's kinetic energy was ∼ 10 50 erg and the circumburst matter had a constant rather than a wind profile. The lack of a "jet break" up to 22 days implies that the outflow was wide θ j > 1. Even though the late X-ray afterglow decays normally it cannot result from an external shock because of its very steep spectrum. Furthermore, the implied kinetic energy would have produced far too much radio. We suggest that this X-ray afterglow could be attributed to a continued activity of the central engine that within the collapsar scenario could arise from fall-back accretion. "Central engine afterglow" may be common in under-luminous GRBs where the kinetic energy of the blast wave is small and the external shock does not dominate over this component. Such underluminous GRBs might be very common but they are rarely recorded because they can be detected only from short distances.

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Section: Discussion and Summarysupporting

confidence: 72%

The interpretation and implication of the afterglow of GRB 060218

Fan

Piran²,

Xu³

2006

J. Cosmol. Astropart. Phys.

121

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“…This can be at least of the order of Γ in the comoving frame (Mastichiadis & Kazanas 2009) but in the case where the electrons are in equipartition with protons it can be a factor of (m p /m e ) higher, i.e. γ min = (m p /m e )Γ (Katz & Piran 1997;Panaitescu & Mészáros 1998). Since the energetic electrons will emit synchrotron radiation, a prescription for the magnetic field is also required.…”

Section: Radiationmentioning

confidence: 99%

On the multiwavelength emission from gamma ray burst afterglows

Πετροπούλου

Mastichiadis

2009

A&A

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Aims. Drawing an analogy with active galactic nuclei, we investigate the one-zone synchrotron self-compton (SSC) model of gamma ray bursts (GRB) afterglows in the presence of electron injection and cooling both by synchrotron and SSC losses. Methods. We solve the spatially averaged kinetic equations which describe the simultaneous evolution of particles and photons, obtaining the multi-wavelength spectrum as a function of time. We back up our numerical calculations with analytical solutions of the equations using various profiles of the magnetic field evolution under certain simplifying assumptions. Results. We apply the model to the afterglow evolution of GRBs in a uniform density environment and examine the impact various parameters have on the multiwavelength spectra. We find that in cases where the electron injection and/or the ambient density is high, the losses are dominated by SSC and the solutions depart significantly from the ones derived in the synchrotron standard cases.

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“…We now derive the evolution for the blast wave more precisely and generally, following Huang et al (1999; see also Katz & Piran 1997). We assume that material passing through the shock quickly radiates a fraction of the post-shock thermal energy, and retains the rest as thermal energy.…”

Section: Dynamicsmentioning

confidence: 99%

Gamma-Ray Burst Afterglows

Paradijs

Kouveliotou

Wijers

2000

Annu. Rev. Astron. Astrophys.

322

248

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The discovery of counterparts in X-ray and optical to radio wavelengths has revolutionized the study of γ -ray bursts, until recently the most enigmatic of astrophysical phenomena. We now know that γ -ray bursts are the biggest explosions in nature, caused by the ejection of ultrarelativistic matter from a powerful energy source and its subsequent collision with its environment. We have just begun to uncover a connection between supernovae and γ -ray bursts, and are finally constraining the properties of the ultimate source of γ -ray burst energy. We review here the observations that have led to this breakthrough in the field; we describe the basic theory of the fireball model and discuss the theoretical understanding that has been gained from interpreting the new wealth of data on γ -ray bursts.

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Persistent Counterparts to Gamma‐Ray Bursts

Cited by 120 publications

References 22 publications

The interpretation and implication of the afterglow of GRB 060218

The interpretation and implication of the afterglow of GRB 060218

On the multiwavelength emission from gamma ray burst afterglows

Gamma-Ray Burst Afterglows

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