Abstract
Using a survey of 16 dense cores, Myers et al. (1991) deduced that they posses apparent elongations that would indicate prolate, rather than oblate shapes, with relative elongations that correspond to axial ratios of 2:1, but if some of them are oblate, then their axial ratios would be 3:1 to 10:1 or even larger. Myers et al. (1991) concluded that elongated cores embedded in much longer filaments are likely to be prolate if their long axes are approximately aligned with that of the filament but if their long axes are perpendicular to that of the filament, they could well be oblate.
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References
Chen, H., & Tokunaga, A. T. 1994, ApJS, 90, 149.
Myers, P. C., Fuller, G. A., Goodman, A. A., & Benson, P. J. 1991, ApJ, 376, 561.
Strom, K. M., Strom, S. E., & Merrill, K. M. 1993, ApJ, 412, 23.
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© 1999 Springer Science+Business Media Dordrecht
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Klapp, J., Sigalotti, L.D.G. (1999). Numerical Simulations of the Formation of Small Protostellar Clusters Using an SPH Code. In: Miyama, S.M., Tomisaka, K., Hanawa, T. (eds) Numerical Astrophysics. Astrophysics and Space Science Library, vol 240. Springer, Dordrecht. https://doi.org/10.1007/978-94-011-4780-4_49
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DOI: https://doi.org/10.1007/978-94-011-4780-4_49
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