SUMMARY AND FUTURE WORK

Rotational instabilities in star-like objects are well-in-hand (quantitative agreement between linear and nonlinear simulations). We find for:
T/|W| > 0.09-0.14 -==> bar mode secularly unstable

T/|W| > 0.27 ===> bar mode dynamically unstable

Incompressible fluid results are a good predictor of the properties of compressible fluids

Gravitational self-interaction torques saturate the growth of the bar mode before binary formation occurs in protostars

Star/disk and disk-like systems form naturally in GMCs. Their properties are qualitatively different from more star-like objects. They warrant far more attention in the future.