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arXiv · 1005.0141

Relativistic Radiation Mediated Shocks

Ran Budnik·Boaz Katz·Amir Sagiv·Eli Waxman
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Abstract

The structure of relativistic radiation mediated shocks (RRMS) propagating into a cold electron-proton plasma is calculated and analyzed. A qualitative discussion of the physics of relativistic and non relativistic shocks, including order of magnitude estimates for the relevant temperature and length scales, is presented. Detailed numerical solutions are derived for shock Lorentz factors $Γ_u$ in the range $6\leΓ_u\le30$, using a novel iteration technique solving the hydrodynamics and radiation transport equations (the protons, electrons and positrons are argued to be coupled by collective plasma processes and are treated as a fluid). The shock transition (deceleration) region, where the Lorentz factor $ Γ$ drops from $ Γ_u $ to $ \sim 1 $, is characterized by high plasma temperatures $ T\sim Γm_ec^2 $ and highly anisotropic radiation, with characteristic shock-frame energy of upstream and downstream going photons of a few~$\times\, m_ec^2$ and $\sim Γ^2 m_ec^2$, respectively.Photon scattering is dominated by e$^\pm$ pairs, with pair to proton density ratio reaching $\approx10^2Γ_u$. The width of the deceleration region, in terms of Thomson optical depths for upstream going photons, is large, $Δτ\simΓ_u^2$ ($Δτ\sim1$ neglecting the contribution of pairs) due to Klein Nishina suppression of the scattering cross section. A high energy photon component, narrowly beamed in the downstream direction, with a nearly flat power-law like spectrum, $νI_ν\proptoν^0$, and an energy cutoff at $ \sim Γ_u^2 m_ec^2 $ carries a fair fraction of the energy flux at the end of the deceleration region. An approximate analytic model of RRMS, reproducing the main features of the numerical results, is provided.

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Ran Budnik, Boaz Katz, Amir Sagiv, Eli Waxman. 2010-05-02. Relativistic Radiation Mediated Shocks. https://doi.org/10.1088/0004-637x%2F725%2F1%2F63

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