Circularization and Tidal Dissipation in Eclipsing Binary Stars
Results for early type binaries in the Magellanic Clouds from the MACHO project.
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This work studies orbital circularization of binarystars past the Main Sequence using two new samples ofeclipsing binary stars found in the Magellanic Cloudsby the MACHO Project, as well as samples introducedby the OGLE-II project and finds strong evidence oforbit circularization past the Main Sequence phase ofstellar evolution, by the almost complete absence ofsystems with eccentric orbits in the Red Giant partof the Color Magnitude Diagram whereas the MainSequence exhibits systems with a broad range ofeccentricities.This absence allows to robustly conclude that binarystarscircularize their o...
This work studies orbital circularization of binary
stars past the Main Sequence using two new samples of
eclipsing binary stars found in the Magellanic Clouds
by the MACHO Project, as well as samples introduced
by the OGLE-II project and finds strong evidence of
orbit circularization past the Main Sequence phase of
stellar evolution, by the almost complete absence of
systems with eccentric orbits in the Red Giant part
of the Color Magnitude Diagram whereas the Main
Sequence exhibits systems with a broad range of
eccentricities.
This absence allows to robustly conclude that binary
stars
circularize their orbits either on crossing the
Hertzsprung Gap or on ascending the Red Giant Branch
when they undergo a sudden and dramatic increase in
their dimensions resulting in strong tidal forces
that disrupt the orbit.
The work then quantifies the effects of tidal
interaction and distortions via a a thorough study of
the Specific Dissipation Function Q, which is
generally not well known for binary stars and finds
evidence of a low degree of tidal dissipation.
stars past the Main Sequence using two new samples of
eclipsing binary stars found in the Magellanic Clouds
by the MACHO Project, as well as samples introduced
by the OGLE-II project and finds strong evidence of
orbit circularization past the Main Sequence phase of
stellar evolution, by the almost complete absence of
systems with eccentric orbits in the Red Giant part
of the Color Magnitude Diagram whereas the Main
Sequence exhibits systems with a broad range of
eccentricities.
This absence allows to robustly conclude that binary
stars
circularize their orbits either on crossing the
Hertzsprung Gap or on ascending the Red Giant Branch
when they undergo a sudden and dramatic increase in
their dimensions resulting in strong tidal forces
that disrupt the orbit.
The work then quantifies the effects of tidal
interaction and distortions via a a thorough study of
the Specific Dissipation Function Q, which is
generally not well known for binary stars and finds
evidence of a low degree of tidal dissipation.
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