Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 1992
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992pasp..104..923s&link_type=abstract
Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 104, no. 680, p. 923-930.
Astronomy and Astrophysics
Astronomy
56
Asymptotic Giant Branch Stars, Planetary Nebulae, Star Formation, Stellar Activity, Magnetoactivity, Stellar Envelopes, Stellar Evolution
Scientific paper
We apply a method, which is traditionally used for the solar magnetic field, to estimate the magnetic activity of AGB stars. We find that any magnetic-field model which tries to explain axisymmetrical mass loss from single AGB stars encounters severe difficulties. This order-of-magnitude calculation suggests that magnetic activity in AGB stars could be significant only if the envelope is spun up by a binary companion. We conduct a preliminary study of a possible mechanism by which a single star might lose mass axisymmetrically. The results suggest that as the envelope mass of an AGB star decreases to less than or approximately equal to 1 solar mass the nature of the fundamental mode excitation could damage. It is possible that, due to the same mechanism, higher-order radial modes and nonradial p modes could become significant to the mass-loss process when the envelope mass becomes very low. We argue, however, that even this mechanism, if it works, requires a binary companion to spin up the AGB envelope.
Harpaz Amos
Soker Noam
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