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Alfvén waves damping in protostellar disks providing a way to expand the action of the magneto-rotational instability

Published online by Cambridge University Press:  01 August 2006

A. A. Vidotto  and
V. Jatenco-Pereira
A. A. Vidotto
Affiliation:
IAG, Univ. de São Paulo, Rua do Matão 1226, São Paulo, SP 05508-900, Brazil email: aline@astro.iag.usp.br
V. Jatenco-Pereira
Affiliation:
IAG, Univ. de São Paulo, Rua do Matão 1226, São Paulo, SP 05508-900, Brazil email: aline@astro.iag.usp.br
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Abstract

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In order for the magneto-rotational instability to take place, we need a sufficiently ionized disk. Here, we study, besides viscous dissipation, another heating mechanism for the disk that involves the damping of Alfvén waves due to its interaction with dust grains.

Keywords

stars: pre–main-sequenceaccretionaccretion disksMHDturbulencewaves
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Symposium S237: Triggered Star Formation in a Turbulent ISM , August 2006 , pp. 491
Copyright
Copyright © International Astronomical Union 2007

References

Shakura, N.I. & Sunyaev, R.A. 1973, A&A 24, 337Google Scholar
Vidotto, A.A. & Jatenco-Pereira, V. 2006, ApJ 639, 416CrossRefGoogle Scholar