Abstract
The rotation rates of single white dwarfs have been measured, via as teroseismology, to range from 5 hours to 2 days and more (Kawaler 2001, Koester et al. 1998). However, if the progenitor stars always rotate as solid bodies, the rotation period should be much longer. Considering another limit, conservation of specific angular momentum j(=J/M), AGB stars should develop steep angular velocity gradients between the core and the envelope. Such gradients could trigger dynamo magnetic field generation — and thereby provide a shaping mechanism to produce assymetric planetary nebulae at the end of AGB evolution (Blackman et al. 2001).
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References
Blackman, E.G. et al. 2001, Nature, 409, 485.
Kawaler, S. 2001, in IAU Colloq. 183: Small Telescope Astronomy on Global Scales, ed. B. Paczynski, W.-P. Chen, & C. Lemme (San Franciso: ASP Press), p. 3.
Koester, D. et al. 1998, A.& A., 338. 612.
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Kawaler, S.D., Hostler, S., Burkett, J. (2003). The Origin of White Dwarf Rotation Velocities. In: de Martino, D., Silvotti, R., Solheim, JE., Kalytis, R. (eds) White Dwarfs. NATO Science Series, vol 105. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-0215-8_8
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DOI: https://doi.org/10.1007/978-94-010-0215-8_8
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