On the jet structure and magnetic field configuration   of
GRB 020813

Lazzati, Davide; Covino, S.; Gorosabel, J.; Rossi, Elena M.; Ghisellini, G.; Rol, E.; Cerón, J. M. Castro; Castro-Tirado, A. J.; Valle, M. Della; Alighieri, S. di Serego; Fruchter, A. S.; Fynbo, J. P. U.; Goldoni, P.; Hjorth, J.; Israel, G. L.; Kaper, L.; Kawai, N.; Floc’h, E. Le; Malesani, D.; Masetti, N.; Mazzali, P. A.; Mirabel, F.; Møller, P.; Ortolani, S.; Palazzi, E.; Pian, E.; Rhoads, James E.; Ricker, G.; Salmonson, J. D.; Stella, L.; Tagliaferri, G.; Tanvir, N. R.; Heuvel, E. van den; Wijers, R. A. M. J.; Zerbi, F. M.

doi:10.1051/0004-6361:20035951

Cited by 51 publications

(63 citation statements)

References 30 publications

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“…We refer to the companion paper by Lazzati et al (2004) for a detailed theoretical discussion and interpretation of the data reported in the present work.…”

Section: Resultsmentioning

confidence: 99%

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GRB 020813: Polarization in the case of a smooth optical decay

Gorosabel¹,

Rol²,

Covino³

et al. 2004

A&A

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Abstract. We present the results of a VLT polarimetric monitoring campaign of the GRB 020813 optical afterglow carried out in three nights, from 0.88 to 4.20 days after the gamma-ray event. The mean values of the degree of linear polarization (P) and its position angle (θ) resulting from our campaign are P = 1.18 ± 0.10% and θ = 148.7• ± 2.3 • , after correcting for Galactic interstellar polarization. Our VLT data set is most naturally described by a constant degree of linear polarization and position angle, nonetheless a slow θ evolution cannot be entirely ruled out by our data. The VLT monitoring campaign did not reveal either a significant θ rotation respect to the Keck spectropolarimetric observations performed ∼0.25 days after the GRB . However, P is a factor of two lower than the polarization degree measured from Keck. Additionally, the VLT polarization data allowed us to construct an accurate V-band light curve. The V-band photometric data revealed a smooth light curve with a break located between the last Keck and our first VLT polarimetric measurement, 0.33 < t break,V < 0.88 days after the GRB. The typical magnitude fluctuations of the VLT V-band lightcurve are 0.003 mag, 0.010 mag and 0.016 mag for our three observing nights, respectively. We speculate that the stability of θ might be related to the smoothness of the light curve.

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“…We refer to the companion paper by Lazzati et al (2004) for a detailed theoretical discussion and interpretation of the data reported in the present work.…”

Section: Resultsmentioning

confidence: 99%

“…In the present paper we report an intensive polarimetric follow up of the GRB 020813 OA. In a companion paper Lazzati et al (2004) report a physical interpretation of the polarization data published in this study. 1 See http://www.mpe.mpg.de/∼jcg/grbgen.html…”

Section: Introductionmentioning

confidence: 83%

GRB 020813: Polarization in the case of a smooth optical decay

Gorosabel¹,

Rol²,

Covino³

et al. 2004

A&A

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“…In the top panel the Lorentz factor of the ejecta is assumed to remain equal to that of the freshly shocked fluid just behind the forward shock (FS), while the middle panel is assumed to follow the Blandford & McKee (1976) self-similar solution (BM). The bottom panel is for a structured jet where the energy per solid angle drops as θ −2 outside of some small core angle (taken from Lazzati et al 2004). In this case P(t/t j ) is practically independent of θ obs .…”

Section: The Radio Flare and Its Polarisationmentioning

confidence: 99%

Gamma-Ray Burst Jets and their Radio Observations

Granot

Horst

2014

Publ. Astron. Soc. Aust.

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Radio observations play a key role in studying the jets that power GRBs, the most luminous cosmic explosions. They are crucial for determining the GRB jet energy, the external density, and the microphysical parameters of relativistic collisionless shocks, from afterglow broadband modeling. Radio image size measurements are rare, but provide extremely useful information. The "radio flare" peaking after ß1 day helps constrain the magnetisation and magnetic-field structure of GRB outflows. This review discusses the current observational and modeling status, focusing on the afterglow and outlining prompt radio emission searches, along with recent theoretical progress in GRB jet dynamics, focusing on magnetic acceleration, jet propagation inside a massive star progenitor (for long GRBs), the reverse shock, and the late afterglow. Great progress has been made in our understanding of magnetic acceleration, collimation and later sideways expansion of GRB jets, with interesting implications for the prompt, reverse shock, and afterglow emission. We outline how theory and observations were combined to study GRB jet physics and their immediate environment. Finally, potential paths are suggested for combining theory and observations to achieve greater progress, and some prospects for the future are discussed in light of the expected improvements in observational capabilities and theoretical advances.

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“…The observer line of sight must be within the beam (otherwise the GRB would be undetectable) but in general not perfectly aligned with the jet. This breaks the source-observer axi-symmetry, avoiding the cancellation of electric vectors created in different emitting regions (Lazzati et al 2004).…”

Section: Polarimetric Observations Of Grb Afterglows and Hypernovaementioning

confidence: 99%

Multiwavelength observations of GRB afterglows

Castro-Tirado

2011

Proc. IAU

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Abstract. Multiwavelength observations of gamma-ray burst afterglows are presented, in particular those in the optical and millimetre wavelengths. I will focus on the observations mostly carried out at Spanish ground-based observatories (mainly the 10.4m GTC) and at the Plateau de Bure Interferometer in the French Alps. The importance of global networks of robotic telescopes (like BOOTES, established worldwide) for early time observations in order to put constraints on the physical mechanisms of the GRB early time emission phase is also discussed. The overall observational efforts provide additional clues for a better understanding of the reverse and forward shock. Finally I will report on the Lomonosov/UFFO-p capabilities taking into account its launch in 2012.

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On the jet structure and magnetic field configuration of GRB 020813

Cited by 51 publications

References 30 publications

GRB 020813: Polarization in the case of a smooth optical decay

GRB 020813: Polarization in the case of a smooth optical decay

Gamma-Ray Burst Jets and their Radio Observations

Multiwavelength observations of GRB afterglows

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