Eclipsing binaries with eccentric orbits Waldemar Ogłoza www.as.up.krakow.pl.

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Presentation transcript:

Eclipsing binaries with eccentric orbits Waldemar Ogłoza

4 source of information:

C = M O + P  E M O – time of referenced eclipse P – period E - epoch

O-C

Period variations diven by: Mass transfer Mass ejection 3 body Apsidal motion Magnetic braking Emission of gravitational waves …

Diagram O-C

e=0.5

Gravitational breaking

Magnietic breaking

Orbital circularisation and synchronization * radiative

* convective:

Pri:  =  /2 -  Sec:  =3  /2 -  - True anomaly - Mean anomaly  = 2  (t-t o ) /P

Case: i  90

Why d  /dt  ≠ 0

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