Common Envelope Evolution |
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Common Envelopes (CE) are thought to form when unstable mass transfer from
an evolving primary onto a compact companion, results in the primary's
envelope engulfing both stars. During the ensuing spiral-down phase, energy is transfered
into the envelope, resulting in its ejection and in a much reduced
binary period (Paczynski 1976). The CE mechanism explains the existence
of evolved short-period binaries, such as novae, dwarf novae, the
progenitors of type Ia supernovae,
low-mass X-ray binaries, as well as scores of other binary systems containing
all combinations of white dwarfs, neutron stars and black holes.
In addition to these classes, a
large number of evolved and un-evolved, apparently single, stars are increasingly revealing close
faint companions including planets.
Now more than ever we need a complete and clear description
of the changes induced in stellar evolution by the CE interaction.
On the right we show a density slice from one of the CE simulations of Passy et al. (2012). |
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Below are some of the questions that I am currently tackling with my research. |
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Are most Planetary Nebulae the result of binary interactions? |
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Post-AGB H-deficiency & binary mergers |
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A theoretical approach to Common Envelope interactions |
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Mass-loss geometry and disks |
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Blue Straggler stars: stellar collisions & binary mergers |
Last Update: 22 March 2018