Astronomy and Astrophysics – Astronomy
Scientific paper
Mar 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003mnras.340...91c&link_type=abstract
Monthly Notice of the Royal Astronomical Society, Volume 340, Issue 1, pp. 91-104.
Astronomy and Astrophysics
Astronomy
26
Methods: Numerical, Binaries: General, Stars: Formation
Scientific paper
Numerical simulations of the collapse of a slowly rotating cloud have been performed, assuming either isothermality, or a barotropic equation of state that reproduces the expected thermal behaviour of protostellar gas. A ring appears in the late stages of the collapse of a rotating cloud, and we have investigated the effect of differential rotation on the formation and fragmentation of this ring. In the simulations presented here, we have used Godunov-type particle hydrodynamics to avoid the side effects of artificial viscosity in a differentially rotating cloud. The initial state of a cloud is characterized by and , where , Ω and are the thermal, gravitational and rotational energies, respectively.
If the initial angular velocity, ω, of a cloud is proportional to r-P, then in the isothermal simulations, a ring forms if P is larger than 0.5, provided βo<~ 0.035.
In the simulations using a barotropic equation of state, with αo= 0.6 and βo<~ 0.035, a ring is always formed, irrespective of whether P<= 0.5 or P > 0.5. However, the mechanism and time of ring formation are different in the two extremes, as are the final configurations. Strong differential rotation (P > 0.5) is more effective in inducing fragmentation than solid-body rotation (P= 0), in the sense that fragmentation tends to occur earlier and to produce more fragments when P is larger.
Cha Seung-Hoon
Whitworth Anthony P.
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