Reverse Shock Emission in Gamma-Ray Bursts Revisited

Mészáros, P.

doi:10.1155/2015/192383

Cited by 13 publications

(10 citation statements)

References 160 publications

(226 reference statements)

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“…Notwithstanding the constraints on t 0 , our revised decay indices of the Xray fluxes are still too steep ( 2) with respect to the model predictions for the forward shock (1.2, assuming that the energy distribution of the accelerated particles has a power-law shape with an index p=2.2, Wang et al 2003). The scenario of a reverse shock that is dominant in X-rays has been considered to explain some GRBs' afterglows (see Gao & Mészáros 2015, for a review). Genet et al (2007) have shown that the X-ray emission from a reverse shock may be dominant during the early afterglow phase provided that: 1-the bulk motion of the material ejected during the last stages of the source activity is Γ bulk <10 and 2-a large part of the shock-dissipated energy is transferred to a small fraction of the electron population (see also Uhm & Beloborodov 2007).…”

Section: Constraints On the Particle Acceleration Process From The Brmentioning

confidence: 87%

Evolving morphology of the large-scale relativistic jets from XTE J1550−564

Migliori

Corbel

Tomsick

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present an in-depth study of the large-scale, western jet of the microquasar XTE J1550−564, based on X-ray and radio observations performed in [2002][2003]. The jet is spatially resolved in both observing windows. The X-ray jet is expanding in time along the axis of the jet's propagation: we observe the formation of a tail (∼2.25 ), which appears to extend backwards with an apparent velocity ∼ −0.10c. The origin of this feature is discussed in the framework of scenarios of energy dissipation. A single power-law adequately describes the broadband spectra, supporting a synchrotron origin of the X-ray emission. However, a spectral break at ≈10 15 Hz is necessary in coincidence with a re-flare at 8.64 GHz in September 2002. This finding may be indicative of emission from newly accelerated low-energy particles. The first detection of the jet is in February 2001 (F 8.64GHz =0.25±0.09 mJy) in the flux rising phase. A phase of stable emission is followed by a rapid decay (t decay =167±5 days). The decay at radio frequencies is significantly shorter than in X-rays (t decay =338±14 days). We detected a high fraction (up to ∼9%) of linearly polarized radiation at 4.8 GHz and 8.6 GHz. The orientation of the electric vector is consistent with the picture of a shock-compressed magnetic field, and there are hints of variations on month-timescales, possibly connected with the evolution of the jet structure.

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Section: Constraints On the Particle Acceleration Process From The Brmentioning

confidence: 87%

Evolving morphology of the large-scale relativistic jets from XTE J1550−564

Migliori

Corbel

Tomsick

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…For relativistic RS, one more additional parameter, T 90 , representing the width of the ejected shell, enters the picture. For a detailed review, see Gao & Mészáros (2015). Synchrotron spectrum from the reverse shocked ejecta can be calculated from the properties of the downstream the same way as described for the FS in section-4.2.…”

Section: Reverse Shock Emissionmentioning

confidence: 99%

Radio Afterglows of Gamma Ray Bursts

Resmi

2017

J Astrophys Astron

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Abstract. This review focuses on the physics of Gamma Ray Bursts probed through their radio afterglow emission. Even though radio band is the least explored of the afterglow spectrum, it has played an important role in the progress of GRB physics, specifically in confirming the hypothesized relativistic effects. Currently radio astronomy is in the beginning of a revolution. The high sensitive Square Kilometer Array (SKA) is being planned, its precursors and pathfinders are about to be operational, and several existing instruments are undergoing upgradation. Thus, the afterglow detection statistics and results from follow up programs are expected to improve in the coming years. We list a few avenues unique to radio band which if explored to full potential have the promise to greatly contribute to the future of GRB physics.

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“…Both the X-ray plateaus and the optical re-brightenings can not be explained in the framework of a simple FS scenario. Thus researchers have proposed several refined models to interpret these unexpected features in recent years (see [21,22] for a review). Stimulated by these refined models, it is urgent to answer whether X-ray plateaus and optical re-brightenings have a natural origin or they are special outcomes varying in different GRBs.…”

Section: Introductionmentioning

confidence: 99%

Diverse Features of the Multiwavelength Afterglows of Gamma-Ray Bursts: Natural or Special?

Geng

Huang

2016

Advances in Astronomy

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The detection of optical re-brightenings and X-ray plateaus in the afterglows of gamma-ray bursts (GRBs) challenges the generic external shock model. Recently, we have developed a numerical method to calculate the dynamic of the system consisting of a forward shock and a reverse shock. Here, we briefly review the applications of this method in the afterglow theory. By relating these diverse features to the central engines of GRBs, we find that the steep optical re-brightenings would be caused by the fall-back accretion of black holes, while the shallow optical re-brightenings are the consequence of the injection of the electron-positron-pair wind from the central magnetar. These studies provide useful ways to probe the characteristics of GRB central engines.

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Reverse Shock Emission in Gamma-Ray Bursts Revisited

Cited by 13 publications

References 160 publications

Evolving morphology of the large-scale relativistic jets from XTE J1550−564

Evolving morphology of the large-scale relativistic jets from XTE J1550−564

Radio Afterglows of Gamma Ray Bursts

Diverse Features of the Multiwavelength Afterglows of Gamma-Ray Bursts: Natural or Special?

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