On the dynamic efficiency of internal shocks in magnetized relativistic outflows

• Published in: Monthly notices of the Royal Astronomical Society 2010-01, Vol.401 (1), p.525-532
• Main Authors: Mimica, P., Aloy, M. A.
• Format: Article
• Language: English
• Subjects: Astrophysics; BL Lacertae objects: general; Fluid mechanics; Gamma rays; gamma-rays: bursts; hydrodynamics; Kinetics; Magnetic fields; MHD; shock waves; Stars & galaxies; Velocity
• ISSN: 0035-8711; 1365-2966
• DOI: 10.1111/j.1365-2966.2009.15669.x

We study the dynamic efficiency of conversion of kinetic-to-thermal/magnetic energy of internal shocks in relativistic magnetized outflows. We model internal shocks as being caused by collisions of shells of plasma with the same energy flux and a non-zero relative velocity. The contact surface, where the interaction between the shells takes place, can break up either into two oppositely moving shocks (in the frame where the contact surface is at rest), or into a reverse shock and a forward rarefaction. We find that for moderately magnetized shocks (magnetization σ≃ 0.1), the dynamic efficiency in a single two-shell interaction can be as large as 40 per cent. Thus, the dynamic efficiency of moderately magnetized shocks is larger than in the corresponding unmagnetized two-shell interaction. If the slower shell propagates with a sufficiently large velocity, the efficiency is only weakly dependent on its Lorentz factor. Consequently, the dynamic efficiency of shell interactions in the magnetized flow of blazars and gamma-ray bursts is effectively the same. These results are quantitatively rather independent on the equation of state of the plasma. The radiative efficiency of the process is expected to be a fraction fr < 1 of the estimated dynamic one, the exact value of fr depending on the particularities of the emission processes which radiate away the thermal or magnetic energy of the shocked states.