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Heating mechanisms in accretion disks around young stellar objects

Published online by Cambridge University Press:  13 January 2020

Natália F.S. Andrade
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas (IAG), Universidade de São Paulo, Rua do Matão 1226, São Paulo, SP, Brazil email: [email protected]
Rafael Rechiche de Campos
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas (IAG), Universidade de São Paulo, Rua do Matão 1226, São Paulo, SP, Brazil email: [email protected]
Vera Jatenco-Pereira
Affiliation:
Instituto de Astronomia, Geofísica e Ciências Atmosféricas (IAG), Universidade de São Paulo, Rua do Matão 1226, São Paulo, SP, Brazil email: [email protected]
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Abstract

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Accretion disks are observed around young stellar objects such as T Tauri stars. In order to complete the star formation, particles in the disk need to loose angular momentum in order to be accreted into the central object. The magneto-rotational instability (MRI) is probably the mechanism responsible for a magneto-hydrodynamic (MHD) turbulence that leads to disk accretion, which implies the disk particles to be coupled with the magnetic filed lines. As the temperature in the disk is low, we considered, besides the viscous heating mechanism often included in the models by means of the α - prescription, the damping of Alfvén waves as an additional heating source. In particular, we show that the mechanism derived that couples the turbulent and non-linear damping mechanisms of Alfvén waves proved to be very efficient, generating temperatures almost one order of magnitude higher than those mechanisms considered independently.

Type
Contributed Papers
Copyright
© International Astronomical Union 2020 

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