Computer Science – Numerical Analysis
Scientific paper
Sep 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aipc..784..665c&link_type=abstract
MAGNETIC FIELDS IN THE UNIVERSE: From Laboratory and Stars to Primordial Structures. AIP Conference Proceedings, Volume 784, pp
Computer Science
Numerical Analysis
Astrophysical Jets, Numerical Analysis, Pre-Main-Sequence Stars, Star Formation, Interstellar Matter, Jets, Outflows And Bipolar Flows, Pre-Main Sequence Objects, Young Stellar Objects And Protostars, Star Formation
Scientific paper
In this paper, we briefly review the role played by the magnetic field in protostellar (or Herbig-Haro) jets. Among its most important effects on the jet dynamics at the large (sub-parsec and parsec) scales, we may distinguish: i) deflection of the jet in the interstellar medium; ii) change of the rate at which the Rayleigh-Taylor and Kelvin-Helmholtz instabilities develop in the jet head and along the beam; and iii) change of the emission line structure behind the working surfaces. Magnetic fields also seem to play a key role in the jet launching mechanism from the protostar and accretion disk that surrounds it. We present here recent results from three-dimensional Smoothed Particle Hydrodynamical numerical simulations of rotating jets which are in good agreement with high resolution observations of the DG Tau microjet that have shown the presence of a pattern in the radial velocity that is consistent with a rotating jet launched from a Keplerian accretion disk by magneto-centrifugal forces. We have also found that a magnetic field of ~ 0.5 mG is sufficient to collimate the jet against the lateral expansion that is caused by the centrifugal forces. The simulations have been also able to provide minimum values for the ratio Bφ/Bp that can be compared with inferred values from the observations.
Cerqueira Adriano H.
de Gouveia dal Pino Elisabete M.
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