Astronomy and Astrophysics – Astrophysics
Scientific paper
Mar 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...283..858d&link_type=abstract
Astronomy and Astrophysics, Vol. 283, p. 858 (1994)
Astronomy and Astrophysics
Astrophysics
8
Hydrodynamics - Methods: Numerical - Stars: Formation
Scientific paper
A second-order accurate, three-dimensional hydrodynamic code has been used to model the gravitational collapse and fragmentation of a centrally condensed, differentially rotating protostellar core. The initial model is assumed to have a moderate amplitude (α = 0.3), m = 2 density perturbation with ratios of thermal and rotational to gravitational energy αi ≍ 0.15 and βi ≍ 0.17, respectively. Formation of a hierarchical multiple protostellar core is observed to occur during the isothermal collapse only if the initial conditions include small internal radial motions. Collapse from rest results only in the formation of a binary system. A linear perturbation analysis shows that internal radial motions if present initially can induce finite non-axisymmetry through hydrodynamical coupling which may then amplify inducing gravitation- or rotation-driven fragmentation. This provides an important mechanism to induce multiple (hierarchical) fragmentation in rapidly rotating cloud cores collapsing with significant initial non-rotational kinetic energy.
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