Abstract
The resonant interaction between an orbiting low-mass secondary star and the pulsational modes of the primary in a common envelope binary system is studied. When the secondary is very close to the envelope, and especially if it is inside the envelope, i.e., the system is in a common envelope phase, a rich spectrum of both g- and p-modes can be excited. During the common envelope phase high-order and high harmonic p-modes become important. By means of a simple one-zone model, the amplitudes of the forced oscillations are approximately estimated. It is claimed that if several conditions are met, then a brown dwarf secondary can cause nonnegligible axisymmetrical mass loss through its resonant interaction with a red giant primary's envelope. One implication of this for elliptical planetary nebulae is discussed.
Original language | English |
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Pages (from-to) | 593-600 |
Number of pages | 8 |
Journal | Astrophysical Journal |
Volume | 367 |
Issue number | 2 |
DOIs | |
State | Published - 1 Feb 1991 |
Externally published | Yes |
Keywords
- Stars: binaries
- Stars: pulsation