Magnetar giant flares and afterglows as relativistic magnetized explosions

We propose that giant flares on soft γ‐ray repeaters produce relativistic, strongly magnetized, weakly baryon‐loaded magnetic clouds, somewhat analogous to solar coronal mass ejection (CME) events. The flares are driven by unwinding of the internal non‐potential magnetic field which leads to a slow build‐up of magnetic energy outside of the neutron star. For large magnetospheric currents, corresponding to a large twist of the external magnetic field, the magnetosphere becomes dynamically unstable on the Alfvén crossing time‐scale of the inner magnetosphere, t A ∼ R NS / c ∼ 30 μs . The dynamic instability leads to the formation of dissipative current sheets through the development of a tearing mode. The released magnetic energy results in the formation of a strongly magnetized, pair‐loaded, quasi‐spherically expanding flux rope, topologically connected by the magnetic field to the neutron star during the prompt flare emission. The expansion reaches large Lorentz factors, Γ∼ 10–20 , at distances r ∼ 1–2 × 10 7  cm , where a leptophotonic load is lost. Beyond this radius plasma is strongly dominated by the magnetic field, though some baryon loading, with M ≪ E / c 2 , by ablated neutron star material may occur. Magnetic stresses of the tied flux rope lead to a late collimation of the expansion, on time‐scales longer than the giant flare duration. Relativistic bulk motion of the expanding magnetic cloud, directed at an angle θ∼ 135° to the line of sight (away from the observer), results in a strongly non‐spherical forward shock with observed non‐relativistic apparent expansion and bulk motion velocities β app ∼ cot θ/2 ∼ 0.4 at times of the first radio observations, approximately one week after the burst. An interaction with a shell of wind‐shocked interstellar medium (ISM) and then with the unshocked ISM leads to a deceleration, to non‐relativistic velocities approximately one month after the flare.