Protostellar formation in rotating interstellar clouds. VIII - Inner core formation

Details Protostellar formation in rotating interstellar clouds. VIII - Inner core formation Protostellar formation in rotating interstellar clouds. VIII - Inner core formation

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...346..336b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 346, Nov. 1, 1989, p. 336-349.

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38

Interstellar Matter, Molecular Clouds, Protostars, Rotating Matter, Star Formation, Stellar Cores, Angular Momentum, Computational Astrophysics, Ejection, Gravitational Collapse

Scientific paper

The results are presented of a variety of spherically symmetric one-dimensional (1D) calculations intended to determine the robustness of the dynamical hiccup phenomenon in protostellar cores. The 1D models show that the phenomenon is relatively insensitive to changes in the equations of state, numerical resolution, initial density and temperature, and the radiative transfer approximation. In 1D, the hiccup results in an explosive destruction of the entire inner protostellar core. Inner core formation is studied with a sequence of three-dimensional models which show that rapid inner core rotation stabilizes the hiccup instability. Instead, the inner core becomes quite flat and undergoes a cycle of binary fragmentation, binary decay into a single object surrounded by a bar, breakup of the bar into a binary, etc. When lesser amounts of rotation are involved, the inner core does hiccup somewhat, but mass is ejected in only a few directions, leading to several broad streams of ejecta.

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