1. Transit Timing Variations Szilárd CsizmadiaJena University Institut for Planetary Research, German Aerospace Center Berlin, Germany szilard.csizmadia@dlr.deszilard.csizmadia@dlr.de2011 Jan 11

2. Transits & Eclipses

3. Some real examples of light curves (1)‏ STARE from ground HST from space

4. Some real examples of light curves (2)‏ From ground From space

5. What is O-C? O: observed midtime of a transit, of an eclipse, of a light maxima of a pulsating star, of any kind of a signal... C: calculated time of this signal (linear, quadratic, periodic, etc. ephemeris)‏ Pronounce: “O minus C”

6. An example C 0 = T 0 C 1 = T 1 + P C 2 = T 2 + P + P = T 2 + 2P C N = T 0 + NP T 0 : epoch, P: period, N: cycle number

7. An other example (P=2 days)‏

8. What is the big advantage of O-C? It is accumulating that is why we can study very small effects (smaller than that of the precision of the individual measurements). Example 1: O = T 0 ' + NP' - C = T 0 + NP O – C = (T 0 ' – T 0 ) + N(P' – P)  Wrong period: linear O-C  Wrong epoch: zero-point shift For instance: P' – P = 1 second (  10 -5 days), and our precision is about 20 seconds, then you have to wait for 20 minima to find the period is wrong (but 60 better)‏

9. Example2 : the period increases with a small part in every cycle: P' = P 0 (1 + N  )‏ Then: O 0 = T 0 O 1 = T 0 + P 0 +  O 2 = T 0 + P 0 +  + P 0 + 2   arithmetical series for  O N = T 0 + NP 0 + P 0 N(N-1)  O N  T 0 + NP 0 + P 0 N 2  For large N: The period variation is half of the quadratic term!

10. Real example for O-C variations SZ Lyn (pulsating star in a non-eclipsing binary)‏ Derekas et al. A&A 402, 733 (2003)‏ The companion star was discovered from the O-C diagram!

12. Can we discover other objects around a star, like a planet, using the O-C diagram? The answer is definitely YES!

13. The uncertain case of CM Dra A&A 460, 583 (2008)‏

14. How it looks like... (G. Perez, SMM/IAC)‏

15. Another very "certain" case: V391 Peg Nature 449, 189 (2007)‏

16. At this moment we have only theoretical calculations: star + transiting planet + another planet For perturbation calculations, see: general case: Borkovits et al. (A&A 398, 1091, 2003) coplanar case in circular orbits: Agol et al. (MNRAS 359, 567, 2005)‏

17. A general configuration

18. Perturbation is stronger in case of conjuctions (because the mutual distance is smaller, forces are stronger!) The effect is not symmetric: before conjuction the planet is accelerated, after that it is decelerated.

19. The O-C diagram amplitude (and its shape!) can be calculated applying the equations of celestial mechanics – generally it means numerical integrations of the equations of motion. Third order analytic theory and code for analysis: Borkovits et al. (A&A 398, 1091, 2003) Simplified equations: Agol et al. (MNRAS 359, 567, 2005)‏

20. Kozai - mechanism It is an important mechanism, if the mutual inclination is greater than 40° between the two planets: eccentricity will grow up to the vicinity of 1 (!) periodically. (Inclination also changes.)‏ Perhaps this is the explanation of some of the observed very high eccentricities (up to 0.92) in some exoplanetary system?

21. Resonances are very important because the amplitude of the perturbation can became very high. (See your textbooks...)‏

22. The higher the libration the higher the O-C amplitude. If the mean motion are in p:q resonance (p, q are small integers) there is a resonance and the consequence is the libration. The p:q smaller the libration's amplitude higher. Trojans (p:q = 1:1): the librational amplitude can be as high as 350°!

23. A very important table Kirste, S. Bachelor thesis, 2008

24. Kepler-19b

25. Kepler-20 system

26. http://arxiv.org/abs/1112.216 5

27. Kepler-11 system Nature 470, 52, 2011

28. CoRoT-1b (A&A 510, A94, 2010)

29. A&A 528, A53 (2011)

33. Pal et al. MNRAS413, l42, 2011 HAT-P-13b

34. Nascimbeni et al. A&A 532, A24, 2011