1. Corot 2009 - HD180642 - A.Thoul Modeling of HD180642 = V1449 Aql (THE only  Cephei star main target of CoRoT). Anne Thoul + Maryline Briquet, Pieter Degroote, Andrea Miglio, Josefina Montalban, Conny Aerts, Thierry Morel, Ewa Niemczura, Kévin Belkacem,... + the Corot B star Team

2. Corot 2009 - HD180642 - A.Thoul HD180642 photometry spectroscopy Z obs =0.0099+-0.0016 Data from T. Morel, E.Niemczura et al.

3. Corot 2009 - HD180642 - A.Thoul dominant radial (l=0) mode l=3 ground photometry ground spectroscopy HD180642 11 independent frequencies from Corot Courtesy Pieter Degroote P62

4. Corot 2009 - HD180642 - A.Thoul HD180642 df/dt=[7.6;14.4]10 -11 Hz/ydf/dt ~ 10 -10 Hz/y Hipparcos 0.7m Swiss telescope 1.2m Mercator telescope ASAS photometry COROT Degroote, Aerts et al

5. Corot 2009 - HD180642 - A.Thoul HD180642 11 independent frequencies determined from Corot light curve Only one high frequency mode identified : the high amplitude radial mode One low frequency mode identified No clear multiplet Main radial mode shows a frequency decrease Photometric and spectroscopic error boxes do not overlap

6. Corot 2009 - HD180642 - A.Thoul HD180642 Modelling: using CLES and OSC with AGS05 and OP opacities Fit the radial mode “Free parameters”: X, Z,  ov, M

7. Corot 2009 - HD180642 - A.Thoul HD180642 Range of parameters explored: X = 0.72 – 0.74 Z = 0.010 – 0.015  ov and M: all possible values which give solutions close to the error box in HR diagram

8. Corot 2009 - HD180642 - A.Thoul HD180642 A. Fit the main frequency with the fundamental radial mode on the main sequence n=1 n=2 n=3 X=0.72, Z=0.015,  ov =0, M=12

9. Corot 2009 - HD180642 - A.Thoul HD180642 modelling radial mode with fundamental on MS effect of M and  ov (X=0.72, Z=0.010) M=10M=12  =0.4  =0.2  =0.0

10. Corot 2009 - HD180642 - A.Thoul HD180642 modelling radial mode with fundamental on MS effect of Z (X=0.72,  ov =0) Z=0.010 Z=0.015

11. Corot 2009 - HD180642 - A.Thoul HD180642 modelling radial mode with fundamental on MS effect of X (Z=0.010,  ov =0) X=0.72 X=0.74 M=10 M=12

12. Corot 2009 - HD180642 - A.Thoul HD180642 radial = fundamental on MS  log g fixed by radial mode M~9 M~13

13. Corot 2009 - HD180642 - A.Thoul HD180642 B. Fit the main frequency with the first overtone of the radial mode on the main sequence n=1 n=2 n=3 X=0.72, Z=0.015,  ov =0, M=12

14. Corot 2009 - HD180642 - A.Thoul HD180642 radial mode = fundamental radial mode = first overtone M~13 M~10

15. Corot 2009 - HD180642 - A.Thoul HD180642 C. Fit the main frequency with the second overtone of the radial mode on the main sequence n=1 n=2 n=3 X=0.72, Z=0.015,  ov =0.4, M=10

16. Corot 2009 - HD180642 - A.Thoul HD180642 n=3 n=2 n=1

17. Corot 2009 - HD180642 - A.Thoul HD180642 D. Fit the main frequency with a radial mode after the TAMS n=1 n=2 n=3 log X=0.72, Z=0.010,  ov =0.2, M=10 n=1 n=2 n=3 n=2 n=3

18. Corot 2009 - HD180642 - A.Thoul HD180642 TAMS MS X=0.72,Z=0.010,  ov =0.2,M=10 n=1 n=2 n=3

19. Corot 2009 - HD180642 - A.Thoul HD180642 n=1 n=2 n=3

20. Corot 2009 - HD180642 - A.Thoul HD180642 TAMS MS df/dt on MS much too small

21. Corot 2009 - HD180642 - A.Thoul HD180642 TAMS MS

22. Corot 2009 - HD180642 - A.Thoul HD180642 TAMS MS

23. Corot 2009 - HD180642 - A.Thoul HD180642

24. Corot 2009 - HD180642 - A.Thoul HD180642 photometry spectroscopy

25. Corot 2009 - HD180642 - A.Thoul HD180642 X=0.72, Z=0.010,  ov =0, M=10 X=0.72, Z=0.010,  ov =0.5, M=10 X=0.72, Z=0.015,  ov =0, M=10 X=0.72, Z=0.015,  ov =0, M=12

26. Corot 2009 - HD180642 - A.Thoul HD180642 radial mode is n=1, MS radial mode is n=1, after TAMS X=0.72, Z=0.015,  ov =0, M=9 radial mode is n=1, after TAMS radial mode is n=2, after TAMS radial mode is n=3, after TAMS MAD

27. Corot 2009 - HD180642 - A.Thoul HD180642 X=0.72, Z=0.015,  ov =0.4, M=12 radial mode is n=1, MS radial mode is n=2, MS radial mode is n=3, MS MAD

28. Corot 2009 - HD180642 - A.Thoul HD180642 CONCLUSIONS We’ve got a problem! Modelling of the star using main high amplitude radial mode: l=0, n=1  out of 2  error box in HR diagram (log g too high) range of excited frequencies more or less OK l=0, n=2  in 2  error box but range of excited frequencies too low l=0, n=3  in 1  error box but range of excited frequencies much too low df/dt cannot be explained by evolution

29. Corot 2009 - HD180642 - A.Thoul HD180642 We’ve got a problem! Is log g correct? If yes, how can we have such high amplitude oscillations with high order radial modes? What about the excitation of the modes? What is the explanation for df/dt? Evolution? Resonant coupling? Is the star on MS or after TAMS? (1%)

30. Corot 2009 - HD180642 - A.Thoul HD180642 A “CHIMERA” STAR Hybrid  Cephei / SPB star + solar-like oscillations (Kévin Belkacem et al.)  next step: try modelling the star using all stable and unstable modes NOTE: PROBLEM ==> We will learn something!