Gamma-ray bursts from unstable Poynting-dominated outflows

Lyutikov, Maxim; Blackman, Eric G.

doi:10.1046/j.1365-8711.2001.04190.x

Cited by 64 publications

(60 citation statements)

References 60 publications

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“…5.3 has important implications for the evolutionary origin of systems that produce longduration gamma-ray bursts (LGRBs). In both the collapsar model (Woosley 1993) and the millisecond-magnetar model (Lyutikov & Blackman 2001), the Wolf-Rayet progenitor system of a stellar explosion producing a long (at least two-second) burst of gamma rays is required to have a rapidly spinning core (see, e.g., Langer 2012). Most, perhaps all (Niino 2011), of such gamma-ray bursts occur in regions of their host galaxies that have a low-metal content (Fruchter et al 2006;Modjaz et al 2008;Gräfener & Hamann 2008).…”

Section: The Single and Binary Channels For Long-duration Gamma-ray Bmentioning

confidence: 99%

The VLT-FLAMES Tarantula Survey

Ramírez-Agudelo

Simón‐Díaz

Sana

et al. 2013

A&A

235

281

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Context. The 30 Doradus (30 Dor) region of the Large Magellanic Cloud, also known as the Tarantula nebula, is the nearest starburst region. It contains the richest population of massive stars in the Local Group, and it is thus the best possible laboratory to investigate open questions on the formation and evolution of massive stars. Aims. Using ground-based multi-object optical spectroscopy obtained in the framework of the VLT-FLAMES Tarantula Survey (VFTS), we aim to establish the (projected) rotational velocity distribution for a sample of 216 presumably single O-type stars in 30 Dor. The sample is large enough to obtain statistically significant information and to search for variations among subpopulations -in terms of spectral type, luminosity class, and spatial location -in the field of view. Methods. We measured projected rotational velocities, e sin i, by means of a Fourier transform method and a profile fitting method applied to a set of isolated spectral lines. We also used an iterative deconvolution procedure to infer the probability density, P( e ), of the equatorial rotational velocity, e . Results. The distribution of e sin i shows a two-component structure: a peak around 80 km s −1 and a high-velocity tail extending up to ∼600 km s −1 . This structure is also present in the inferred distribution P( e ) with around 80% of the sample having 0 < e ≤ 300 km s −1 and the other 20% distributed in the high-velocity region. The presence of the low-velocity peak is consistent with what has been found in other studies for late O-and early B-type stars. Conclusions. Most of the stars in our sample rotate with a rate less than 20% of their break-up velocity. For the bulk of the sample, mass loss in a stellar wind and/or envelope expansion is not efficient enough to significantly spin down these stars within the first few Myr of evolution. If massive-star formation results in stars rotating at birth with a large portion of their break-up velocities, an alternative braking mechanism, possibly magnetic fields, is thus required to explain the present-day rotational properties of the O-type stars in 30 Dor. The presence of a sizeable population of fast rotators is compatible with recent population synthesis computations that investigate the influence of binary evolution on the rotation rate of massive stars. Even though we have excluded stars that show significant radial velocity variations, our sample may have remained contaminated by post-interaction binary products. That the highvelocity tail may be populated primarily (and perhaps exclusively) by post-binary interaction products has important implications for the evolutionary origin of systems that produce gamma-ray bursts.

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Section: The Single and Binary Channels For Long-duration Gamma-ray Bmentioning

confidence: 99%

The VLT-FLAMES Tarantula Survey

Ramírez-Agudelo

Simón‐Díaz

Sana

et al. 2013

A&A

235

281

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“…Does it consist of hot baryons, thermally loaded with radiation and pairs greatly exceeding the rest mass (Piran, 1999;Mészáros, 2002), or is the "jet" characterized by large scale magnetic fields, dynamically dominant and present from start (at the central engine) to finish (in the afterglow) (Meszaros and Rees, 1997;Lyutikov and Blackman, 2001;Blandford, 2002;? In the latter case the baryons play little role and may as well be absent.…”

Section: Poynting Flux or Fireball?mentioning

confidence: 99%

The Supernova Gamma-Ray Burst Connection

Woosley

Bloom

2006

AIP Conference Proceedings

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ABSTRACT:Observations show that at least some gamma-ray bursts (GRBs) happen simultaneously with core-collapse supernovae (SNe), thus linking by a common thread nature's two grandest explosions. We review here the growing evidence for and theoretical implications of this association, and conclude that most long-duration soft-spectrum GRBs are accompanied by massive stellar explosions (GRB-SNe). The kinetic energy and luminosity of well-studied GRBSNe appear to be greater than those of ordinary SNe, but evidence exists, even in a limited sample, for considerable diversity. The existing sample also suggests that most of the energy in the explosion is contained in nonrelativistic ejecta (producing the supernova) rather than in the relativistic jets responsible for making the burst and its afterglow.

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“…Usov 1994;Thompson 1994;Smolsky & Usov 1996;Mészáros & Rees 1997;Lyutikov & Blackman 2001;Spruit et al 2001;Drenkhahn 2002;Drenkhahn & Spruit 2002). In this paper we turn to investigate the very early reverse shock emission powered by such a magnetized outflow, just as Sari & Piran (1999) and Mészáros & Rees (1999) have done for the baryon dominated fireball.…”

Section: Introductionmentioning

confidence: 99%

The very early afterglow powered by ultra-relativistic mildly magnetized outflows

Fan

Wei

Wang

2004

A&A

114

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Abstract. In the Poynting Flux-dominated outflow (the initial ratio of the electromagnetic energy flux to the particle energy flux σ 0 1) model for gamma-ray bursts, particularly the γ-ray emission phase, nearly half of the internally dissipated magnetic energy is converted into the γ-ray energy emission and the rest is converted into the kinetic energy of the outflow. Consequently, at the end of the γ-ray burst, σ decreases significantly (σ ∼ 1 or even smaller). We numerically investigate the very early reverse shock emission powered by such mildly magnetized outflows interacting with medium-uniform interstellar medium (ISM) or stellar wind (WIND). We show that for σ ∼ 0.05−1 and typical parameters of gamma-ray bursts, both the ISM-ejecta interaction and the WIND-ejecta interaction can power very strong optical emission (m R ∼ 10−12th mag or even brighter). Similar to the very early afterglow powered by the non-magnetized ejecta interacting with the external medium, the main difference between the ISM-ejecta interaction case and the WIND-ejecta interaction case is that, before the reverse shock crosses the ejecta, the R-band emission flux increases rapidly for the former, but for the latter it increases only slightly. At the very early stage, the ejecta are ultra-relativistic. Due to the beaming effect, the random magnetic field generated in shocks contained in the viewing area is axisymmetric, unless the line of sight is very near the edge of ejecta. The formula Π net ≈ 0.60b 2 /(1 + b 2 ) (where b is the ratio of the ordered magnetic field strength to that of random one) has been proposed to describe the net linear polarization of the synchrotron radiation coming from the viewing area. For σ ∼ 0.05−1, the ordered magnetic field dominates over the random one generated in the reverse shock (As usual, we assume that a fraction B ∼ 0.01 of the thermal energy of the reverse shock has been converted into the magnetic energy), the high linear polarization is expected. We suggest that the linear polarization detection of the early multi-wavelength afterglow is required to see whether the outflows powering GRBs are magnetized or not.

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Gamma-ray bursts from unstable Poynting-dominated outflows

Cited by 64 publications

References 60 publications

The VLT-FLAMES Tarantula Survey

The VLT-FLAMES Tarantula Survey

The Supernova Gamma-Ray Burst Connection

The very early afterglow powered by ultra-relativistic mildly magnetized outflows

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