MHD simulations of the formation and propagation of protostellar jets to observational length scales

Abstract

We present 2.5-D global, ideal MHD simulations of magnetically and rotationally driven protostellar jets from Keplerian accretion discs, wherein only the initial magnetic field strength at the inner radius of the disc, $B_{\mathrm{i}}$, is varied. Using the AMR-MHD code AZEUS, we self-consistently follow the jet evolution into the observational regime ($>10^3\mathrm{AU}$) with a spatial dynamic range of $\sim 6.5\times 10^5$. The simulations reveal a three-component outflow: 1) A hot, dense, super-fast and highly magnetised 'jet core'; 2) a cold, rarefied, trans-fast and highly magnetised 'sheath' surrounding the jet core and extending to a tangential discontinuity; and 3) a warm, dense, trans-slow and weakly magnetised shocked ambient medium entrained by the advancing bow shock. The simulations reveal power-law relationships between $B_{\mathrm{i}}$ and the jet advance speed, $v_{\mathrm{jet}}$, the average jet rotation speed, $⟨v_{\phi }⟩$, as well as fluxes of mass, momentum, and kinetic energy. Quantities that do not depend on $B_{\mathrm{i}}$ include the plasma-$\beta$ of the transported material which, in all cases, seems to asymptote to order unity. Jets are launched by a combination of the 'magnetic tower' and 'bead-on-a-wire' mechanisms, with the former accounting for most of the jet acceleration---even for strong fields---and continuing well beyond the fast magnetosonic point. At no time does the leading bow shock leave the domain and, as such, these simulations generate large-scale jets that reproduce many of the observed properties of protostellar jets including their characteristic speeds and transported fluxes.

arXiv comment26 pages, 16 figures. Accepted for publication in MNRAS

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