Tidal spin-up and the asymmetry degree of planetary nebulae

Details Tidal spin-up and the asymmetry degree of planetary nebulae Tidal spin-up and the asymmetry degree of planetary nebulae

May 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.274..147s&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 274, Issue 1, pp. 147-152.

Astronomy and Astrophysics

Astronomy

16

Binaries: General, Stars: Low-Mass, Brown Dwarfs, Stars: Mass-Loss, Planetary Nebulae: General

Scientific paper

We calculate the rate of orbital angular momentum deposition into the primary's envelopes in binary star systems. The low-mass secondary stars spiral in towards the envelope and deposit their orbital angular momentum as a result of tidal forces. We find that the increase in the angular momentum of the envelopes with time is very steep. As a result, the degree of asymmetry of the wind from the primary's envelopes will also increase steeply with time. If the primary is an AGB star, then the descendent planetary nebulae will be more asymmetrical in the inner regions. The higher degree of asymmetry in their inner regions is a common feature of elliptical planetary nebulae. We conclude, therefore, that tidal interaction of progenitors of elliptical PNe with companion brown dwarfs and massive planets can explain this common feature.

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