31 research outputs found
Numerical Simulations of Gamma-Ray Burst Explosions
Gamma-ray bursts are a complex, non-linear system that evolves very rapidly
through stages of vastly different conditions. They evolve from scales of few
hundred kilometers where they are very dense and hot to cold and tenuous on
scales of parsecs. As such, our understanding of such a phenomenon can truly
increase by combining theoretical and numerical studies adopting different
numerical techniques to face different problems and deal with diverse
conditions. In this review, we will describe the tremendous advancement in our
comprehension of the bursts phenomenology through numerical modeling. Though we
will discuss studies mainly based on jet dynamics across the progenitor star
and the interstellar medium, we will also touch upon other problems such as the
jet launching, its acceleration, and the radiation mechanisms. Finally, we will
describe how combining numerical results with observations from Swift and other
instruments resulted in true understanding of the bursts phenomenon and the
challenges still lying ahead.Comment: 14 Pages, Journal of High Energy Astrophysics for the dedicated
issue: "Swift: Ten Years of Discovery", in pres
Temporal and Angular Properties of GRB Jets Emerging from Massive Stars
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. Our simulations allow us to 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 and would be visible far off axis. The shocked phase has a relatively
narrow opening angle that is constant in time. During the unshocked jet 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. We
finally discuss the observational implications of our results, emphasizing the
possible ways to test progenitor models through the effects of jet propagation
in the star. In an appendix, we present 1D and 2D tests of the FLASH
relativistic hydrodynamics module.Comment: 56 pages, 31 figures (47 postscript files). ApJ in press. Updated
simulation results and revised according to referee comments. Manuscript with
full resolution figures and movies at
http://rocinante.colorado.edu/~morsony/GRB
Gamma-Ray Burst jet dynamics and their interaction with the progenitor star
The association of at least some long gamma-ray bursts with type Ic supernova
explosions has been established beyond reasonable doubt. Theoretically, the
challenge is to explain the presence of a light hyper-relativistic flow
propagating through a massive stellar core without losing those properties. We
discuss the role of the jet-star interaction in shaping the properties of the
outflow emerging on the surface of the star. We show that the nature of the
inner engine is hidden from the observer for most of the evolution, well beyond
the time of the jet breakout on the stellar surface. The discussion is based on
analytical considerations as well as high resolution numerical simulations.
Finally, the observational consequences of the scenario are addressed in light
of the present capabilities.Comment: Proceedings of the Royal Society dscussion meeting "Recent
developments in the study of Gamma-ray bursts", Philosophical Trans. of the
Royal Soc.
High-efficiency photospheric emission of long-duration gamma-ray burst jets: the effect of the viewing angle
We present the results of a numerical investigation of the spectra and light
curves of the emission from the photospheres of long-duration gamma-ray burst
jets. We confirm that the photospheric emission has high efficiency and we show
that the efficiency increases slightly with the off-axis angle. We show that
the peak frequency of the observed spectrum is proportional to the square root
of the photosphere's luminosity, in agreement with the Amati relation. However,
a quantitative comparison reveals that the thermal peak frequency is too small
for the corresponding total luminosity. As a consequence, the radiation must be
out of thermal equilibrium with the baryons in order to reproduce the
observations. Finally, we show that the spectrum integrated over the emitting
surface is virtually indistinguishable from a Planck law, and therefore an
additional mechanism has to be identified to explain the non-thermal behavior
of the observed spectra at both high and low frequencies.Comment: 6 pages, 8 figures, ApJ in press (few changes to figures