Power Density Spectra of Gamma-Ray Bursts in the Internal Shock Model

A. Panaitescu; M. Spada; P. Meszaros

doi:10.1086/312230

paper

Power Density Spectra of Gamma-Ray Bursts in the Internal Shock Model

arXiv:astro-ph/9905026 · doi:10.1086/312230

Abstract

We simulate Gamma-Ray Bursts arising from internal shocks in relativistic winds, calculate their power density spectrum (PDS), and identify the factors to which the PDS is most sensitive: the wind ejection features, which determine the wind dynamics and its optical thickness, and the energy release parameters, which give the pulse 50-300 keV radiative efficiency. For certain combinations of ejection features and wind parameters the resulting PDS exhibits the features observed in real bursts. We found that the upper limit on the efficiency of conversion of wind kinetic energy into 50-300 keV photons is $\sim$ 1%. Winds with a modulated Lorentz factor distribution of the ejecta yield PDSs in accord with current observations and have efficiencies closer to $1 0^{- 3}$ , while winds with a random, uniform Lorentz factor ejection must be optically thick to the short duration pulses to produce correct PDSs, and have an overall efficiency around $1 0^{- 4}$ .

6 pages, 4 figures, Latex, submitted to The Astrophysical Journal (05/04/99)

Power Density Spectra of Gamma-Ray Bursts in the Internal Shock Model

Abstract

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