Solar wind and stellar jets, from newtonian to relativistic ones

Details Solar wind and stellar jets, from newtonian to relativistic ones Solar wind and stellar jets, from newtonian to relativistic ones

Mar 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aipc..895...87s&link_type=abstract

FIFTY YEARS OF ROMANIAN ASTROPHYSICS. AIP Conference Proceedings, Volume 895, pp. 87-96 (2007).

Astronomy and Astrophysics

Astrophysics

Particle Emission, Solar Wind, Mass Loss And Stellar Winds, Jets, Outflows And Bipolar Flows, Pre-Main Sequence Objects, Young Stellar Objects And Protostars

Scientific paper

In parallel to the development of numerical simulations, analytical solutions for modelling the acceleration and the collimation of winds and jets have been proposed. We present here how meridionally self-similar solutions can be used to model the solar wind using Ulysses data at solar minimum. Such solutions may also be adapted to explain the formation core or spine jets in classical and weak TTauri stars (class II and III young stellar jets) as well as relativistic jet cores from AGN. The criterion for collimation explains how the jet evolves towards a wind as the star approaches the main sequence. A similar scenario could explain the winds from Seyfert galaxies by opposition to the powerful jets from Fanaroff Riley sources.

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