Other
Scientific paper
May 2000
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000rmxac...9...83v&link_type=abstract
"Astrophysical Plasmas: Codes, Models, and Observations, Proceedings of the conference held in Mexico City, October 25-29, 1999,
Other
Scientific paper
Alfvén waves have been used to explain the heating of stellar coronae and the production of stellar winds in many regions of the Hertzsprung-Russell (HR) diagram. The waves were used as a major acceleration mechanism in the wind of protostars, late-type stars, early-type stars and in the solar wind. They are also very important in the creation of inhomogeneities in the wind of early-types stars via thermal instability. On the other hand, Alfvénic heating generated by nonlinear and turbulent damping can be an important source of energy for ionizing protostellar disks, enabling angular momentum transport to occur through the Balbus-Hawley instability (BHI). We analysed the role of the damping of Alfvén waves in the inner and intermediate regions of protostellar disks (0.1 < R(AU) < 1.4). We show that when viscous dissipation is insufficient to ensure the necessary degree of ionization for BHI to occur, the damping of Alfvén waves can be an alternative source of energy for ionization.
Jatenco-Pereira Vera
Opher Reuven
Vasconcelos Maria Jaqueline
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