Heating of T Tauri disk winds by magnetic reconnection

Details Heating of T Tauri disk winds by magnetic reconnection Heating of T Tauri disk winds by magnetic reconnection

Aug 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003basbr..23..228d&link_type=abstract

Boletim da Sociedade Astronômica Brasileira (ISSN 0101-3440), vol.23, no.1, p. 228-229

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Scientific paper

The origin of jets from young protostars such as T Tauri stars remains a mistery. Despite tremendous efforts in the observational and theoretical domains, it is still unknown whether jets are driven by the disk alone (in the so called disk-wind process), by the central protostar alone (stellar winds) or by the interaction zone between the disk inner edge and the protostellar magnetosphere (X-winds). Previous modeling of the thermal and ionizaton structure of self-similar magnetically-driven disk winds heated by ambipolar diffusion have predicted too low densities at the jet basis. Other models involving mechanical heating or J-shocks have also failed to provide the observed thermal strutucture. We here investigate the heating of magnetized disk-corona sytems by magnetic reconnection and find that this is quite effective in heating the gas at the jet basis and results densities which are n > > 104 cm-3, as required by line emission observations.

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