Linear polarization in gamma-ray burst prompt emission

Despite being hard to measure, GRB prompt $γ$-ray emission polarization is a valuable probe of the dominant emission mechanism and the outflow's composition and angular structure. During the prompt emission the outflow is ultra-relativistic with Lorentz factors $Γ\gg1$. We describe in detail the linear polarization properties of various emission mechanisms: synchrotron radiation from different magnetic field structures (ordered: toroidal $B_{\rm tor}$ or radial $B_\parallel$, and random: normal to the radial direction $B_\perp$), Compton drag, and photospheric emission. We calculate the polarization for different GRB jet angular structures (e.g. top-hat, Gaussian, power-law) and viewing angles $θ_{\rm obs}$. Synchrotron with $B_\perp$ can produce large polarizations, up to $25\%\lesssimΠ\lesssim45\%$, for a top-hat jet but only for lines of sight just outside the jet's sharp edge. The same also holds for Compton drag, albeit with a slightly higher overall $Π$. Moreover, we demonstrate how $Γ$-variations during the GRB or smoother jet edges would significantly reduce $Π$. We construct a semi-analytic model for non-dissipative photospheric emission from structured jets. Such emission can produce up to $Π\lesssim15\%$ with reasonably high fluences, but this requires steep gradients in $Γ(θ)$. A polarization of $50\%\lesssimΠ\lesssim65\%$ can robustly be produced only by synchrotron emission from a transverse magnetic field ordered on angles $\gtrsim\!1/Γ$ around our line of sight (like a global toroidal field). Therefore, such a model would be strongly favored even by a single secure measurement within this range. We find that such a model would also be favored if $Π\gtrsim20\%$ is measured in most GRBs within a large enough sample, by deriving the polarization distribution for our different emission and jet models.

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