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Eclipsing binaries with eccentric orbits Waldemar Ogłoza www.as.up.krakow.pl
4 source of information:
C = M O + P E M O – time of referenced eclipse P – period E - epoch
Period variations diven by: Mass transfer Mass ejection 3 body Apsidal motion Magnetic braking Emission of gravitational waves …
Orbital circularisation and synchronization * radiative
Pri: = /2 - Sec: =3 /2 - - True anomaly - Mean anomaly = 2 (t-t o ) /P
Case: i 90
Why d /dt ≠ 0
Links www.as.ap.krakow.pl/o-c www.as.ap.krakow.pl/ephem
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