Temporal and Angular Properties of Gamma-Ray Burst Jets Emerging from Massive Stars
By B. Morsony, D. Lazzati, M. Begelman. 2006
190 citations recorded by the source corpus.
We study the long-term evolution of relativistic jets in collapsars and examine the effects of viewing angle on the subsequent gamma-ray bursts. We carry out a series of high-resolution simulations of a jet propagating through a stellar envelope in 2D cylindrical coordinates using the FLASH relativistic hydrodynamics module. For the first time, simulations are carried out using an adaptive mesh that allows for a large dynamic range inside the star while still being efficient enough to follow the evolution of the jet long after it breaks out from the star. We single out three phases in the jet evolution: a precursor phase in which relativistic material turbulently shed from the head of the jet first emerges from the star, a shocked-jet phase where a fully shocked jet of material is emerging, and an unshocked-jet phase where the jet consists of a free-streaming, unshocked core surrounded by a thin boundary layer of shocked-jet material. The appearance of these phases will be different to observers at different angles. The precursor has a wide opening angle, the shocked phase has a relatively narrow opening angle, and in the unshocked phase the opening angle increases logarithmically with time. As a consequence, some observers see prolonged dead times of emission even for constant properties of the jet injected in the stellar core. We also present an analytic model that is able to reproduce the overall properties of the jet and its evolution. In an appendix, we present 1D and 2D tests of the FLASH relativistic hydrodynamics module.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/5891336aae31cb367c046e41836043a0c1f49002
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In Astronomy and Astrophysics
Citations in the corpus
- Relativistic MHD simulations of core-collapse GRB jets: 3D instabilities and magnetic dissipation (2015, background): “Note that this propagation velocity is somewhat slower than the propagation velocity of an equivalent hydrodynamic jet obtained analytically (Bromberg et al. 2011) and in 2D simulations (e.g. Morsony et al. 2007; Mizuta & Aloy 2009).”
- The physics of gamma-ray bursts & relativistic jets (2014, background): “This induces variability in a jet even when the central engine has little fluctuation [715].”
- The Proto-Magnetar Model for Gamma-Ray Bursts (2010, background): “…by accretion, or via the accretion-mediated extraction of the black hole’s spin (Blandford & Znajek 1977), then powers a relativistic jet, which burrows through the star and ultimately powers the GRB at larger radii (MacFadyen & Woosley 1999; Proga et al. 2003; Matzner 2003; Morsony et al. 2007).”
- A theory of photospheric emission from relativistic, collimated outflows (2012, background): “Hydrodynamic simulations of GRB jets after the launching phase (e.g., Zhang et al. 2003; Morsony et al. 2007; Mizuta et al. 2011) show the jet drilling through the stellar envelope, pushing material towards the sides, forming a hot cocoon (e.g. Aloy et al. 2000).”
- THE OBSERVABLE SIGNATURES OF GRB COCOONS (2016, background): “We focus, however, on the signatures resulting from partial mixing as suggested by previous numerical simulations (e.g., Morsony et al. 2007; Mizuta & Aloy 2009; Mizuta & Ioka 2013; López-Cámara et al. 2013, 2016) and by our preliminary numerical results (Harrison et al., in preparation).”