The structure and evolution of thin viscous disks. 1: Non-steady accretion and excretion

Details The structure and evolution of thin viscous disks. 1: Non-steady accretion and excretion The structure and evolution of thin viscous disks. 1: Non-steady accretion and excretion

Dec 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasj...46..575n&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 46, no. 6, p. 575-587

Statistics

Computation

5

Accretion Disks, Astronomical Models, Protostars, Star Formation, Stellar Envelopes, Stellar Evolution, Stellar Mass Accretion, Stellar Rotation, Stellar Winds, Angular Momentum, Angular Velocity, Boundary Layers, Mathematical Models, Spin Dynamics, T Tauri Stars, Temperature Distribution

Scientific paper

The long-term evolution of solar nebula is a non-steady process. Using the alpha-viscosity model, we computed the long-term non-steady evolution of circumstellar disks isolated from neighboring stars. The inner boundary layer, where the pressure is important, was taken fully into account, while the temperature distribution of the disk was assumed to be constant in time. Computations were made for a variety of angular velocities of a central star. The results indicate that there are three critical angular velocities of the central star, which distinguish between the inward and outward directions of the flows of mass and angular momentum. We also found that if the angular velocity of the central star is sufficiently high, the disk evolves from accretion to excretion. From our results we can expect that a protostar continues to accrete most of the disk mass and reaches a very rapidly rotating state with a critical spin rate, if no efficient mechanism works to carry away angular momentum from the star. On the other hand, a large mass loss is observed for young stars, such as T Tauri stars, and they are rather slow rotators. We thus examine how stellar winds keep a protostar at a low spin rate.

Affiliated with

Also associated with

No associations

Rating

The structure and evolution of thin viscous disks. 1: Non-steady accretion and excretion does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with The structure and evolution of thin viscous disks. 1: Non-steady accretion and excretion, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The structure and evolution of thin viscous disks. 1: Non-steady accretion and excretion will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1414258