D. Douchin, O. De Marco, D. J. Frew, G. H. Jacoby, J. -C. Passy, T. Hillwig, S. B. Howell, H. Bond, A. Peyaud, A. Zijlstra, R. Napiwotzki, G. Jasniewicz, Q. Parker
During the past 20 years, the idea that non-spherical planetary nebulae might
need a binary or planetary interaction to be shaped was discussed by various
authors. It is now generally agreed that the varied morphologies of planetary
nebulae cannot be fully explained solely by single star evolution.
Observationally, more binary central stars of planetary nebulae have been
discovered, opening new possibilities to understand the connections between
binarity and morphology. So far, \simeq45 binary central stars of planetary
nebulae have been detected, most being close systems detected via flux
variability. In order to determine the PN binary fraction, one needs a method
that can detect wider binaries. We present here recent results concentrating on
binary infrared excess observations aimed at detecting binaries of any
separation.
View original:
http://arxiv.org/abs/1110.4192
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