Events in the life of a cocoon surrounding a light, collapsar jet

By E. Ramirez-Ruiz, A. Celotti, Martin J. Rees. 2002

217 citations recorded by the source corpus.

According to the collapsar model, γ-ray bursts are thought to be produced in shocks that occur after the relativistic jet has broken free from the stellar envelope. If the mass density of the collimated outflow is less than that of the stellar envelope, the jet will then be surrounded by a cocoon of relativistic plasma. This material would itself be able to escape along the direction of least resistance, which is likely to be the rotation axis of the stellar progenitor, and to accelerate in approximately the same way as an impulsive fireball. We discuss how the properties of the stellar envelope have a decisive effect on the appearance of a cocoon propagating through it. The relativistic material that accumulated in the cocoon would have enough kinetic energy to substantially alter the structure of the relativistic outflow, if not in fact provide much of the observed explosive power. Shock waves within this plasma can produce γ-ray and X-ray transients, in addition to the standard afterglow emission that would arise from the deceleration shock of the cocoon fireball.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/1030c5747682a9994344d297454c1e537085ddbb

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Citations in the corpus

Gamma-Ray Bursts in the Swift Era (2009, background): “Low-mass galaxies and galaxy outskirts have lower metallicity on average and thus may yield more (and/or more luminous) GRBs compared to high-mass galaxies (Ramirez-Ruiz et al. 2002b).”
THE OBSERVABLE SIGNATURES OF GRB COCOONS (2016, background): “Already in 2002, Ramirez-Ruiz et al. (2002) realized the importance of the cocoon component and discussed its possible signature.”
Magnetic acceleration of ultrarelativistic jets in gamma-ray burst sources (2008, background): “…suggested that matter-dominated GRB jets could remain confined by the expanding cocoon of relativistically hot shocked jet material after they break out through the stellar surface (e.g. Ramirez-Ruiz et al. 2002) and could continue to accelerate during that phase (e.g. Lazzati & Begelman 2005).”
The Proto-Magnetar Model for Gamma-Ray Bursts (2010, background): “By contrast, somewhat lower-field magnetars (middle-left diagram) have fth ∼> 0.1 (Eth ∼ 1048−50 ergs), consistent with measurements or upperlimits on quasi-thermal photospheric emission from GRBs (e.g. Mészáros & Rees 2000; Ramirez-Ruiz et al. 2002; Ryde 2005; Guiriec et al. 2010).”
Supernova hosts for gamma-ray burst jets: dynamical constraints (2002, background): “…( θ 3◦ )2 erg. (31) C© 2003 RAS, MNRAS 345, 575–589 Downloaded from https://academic.oup.com/mnras/article-abstract/345/2/575/1746988 by guest on 27 July 2018 Ramirez-Ruiz et al. (2002b) have considered observable implications of cocoon blowout under the hypothesis that no mixing occurs between…”
The physics of gamma-ray bursts & relativistic jets (2014, methodology): “The collapsar model of long-duration GRBs offers a natural mechanism for generating a two-component jet: a narrow, highly relativistic, jet emerging from a star is accompanied by a wider, less relativistic “cocoon” surrounding the jet (Ramirez-Ruiz et al., 2002; Zhang et al., 2004b).”
High-Energy Neutrinos and Cosmic Rays from Low-Luminosity Gamma-Ray Bursts? (2006, background): “This thermal component would be the shock break out from a stellar envelope or a dense wind, or from a hot cocoon surrounding the GRB ejecta (Ramirez-ruiz et al. 2002).”
An Ordinary Short Gamma-Ray Burst with Extraordinary Implications: Fermi-GBM Detection of GRB 170817A (2017, background): “In this picture, significant energy is deposited by the jet responsible for the GRB in the surrounding dense material (e.g. in the debris disk) (Ramirez-Ruiz et al. 2002).”
Off-axis emission of short γ-ray bursts and the detectability of electromagnetic counterparts of gravitational-wave-detected binary mergers (2016, background): “Upon release, it accelerates quasi-isotropically (Ramirez-Ruiz et al. 2002; Nakar & Piran 2017).”
The Propagation and Eruption of Relativistic Jets from the Stellar Progenitors of Gamma-Ray Bursts (2003, background): “The cocoon of the jet will also have different properties from the jet itself, and shocks within the cocoon or with external matter could lead to -ray and hard X-ray transients (Ramirez-Ruiz et al. 2002).”
Gamma-Ray Bursts in the Swift Era (2007, methodology): “Tentative evidence that metallicity isanother important factor to make a GRB has been collected (e.g., Ramirez-Ruiz et al. 2002b; Prochaska et al. 2004; Stanek et al. 2006; Modjaz et al. 2007, cf. Campana et al. 2007).”
Temporal and Angular Properties of Gamma-Ray Burst Jets Emerging from Massive Stars (2006, background): “This phase is due to the release of the turbulent shocked material that accumulates around the jet due to vortex shedding before it breaks out of the star (Ramirez-Ruiz et al. 2002; Zhang et al. MORSONY, LAZZATI, & BEGELMAN586 Vol. 665 2003).”
Physical Processes Shaping Gamma-Ray Burst X-Ray Afterglow Light Curves: Theoretical Implications from the Swift X-Ray Telescope Observations (2005, methodology): “In the collapsar progenitor models, it is expected that the ejecta generally has two components, one ultrarelativistic component powering the GRB, and another moderately relativistic cocoon component (e.g., Zhang. et al. 2004b; Mészáros & Rees 2001; Ramirez-Ruiz et al. 2002).”