1. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group A Hare and Hound in a Bag… Why are they seismologically interesting ?  Cephei Stars

2. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group

3. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group Structure of  Cephei Stars Simple structure : no convective envelope Massive stars : M ~ 9 – 12 M  Solar metallicity : if Z < Z   too few excited modes Convective core : m c  0.20 « Middle» main sequence stars : X c  0.3,  c /   150  Parameters : M,X,Z,  ov,  c / 

4. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group Oscillations of  Cephei Stars f, g- and p-modesbut… low degree l and low order n excited modes  Sparse structure spectrum Excitation :  mechanism in the Fe opacity bump at ~ 2 10 5 K Avoided crossings : frequencies parameter dependent rare enough to take it easy…

5. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group BAG ground-based observations  16 Lac  3 frequencies to appear in A&A – see Bag poster 1  HD129929  5 frequencies Science Express, May 29, 2003  M,Z,  ov,rotation law – see Bag poster 2  Eri  ? frequencies work in progress

6. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group BAG Hare & Hound Exercise  KU-Leuven  Ulg  ROB Site 1 : - Compute model HH1 and frequencies - Find Model HH2  Light curve  Site 2 : - Compute model HH2 and frequencies - Find Model HH1

7. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group Time Sampling - Total time span: 150 days - Orbital period: 6092 s (= 1h42m) - Exposure time: 0.8 s - CCD frame transfer time: 0.2 s - Rebinning in time domain: 1 data point every 32 s - Data loss due to moon: none (if launch before 2007) - Data loss due to SAA: 6-8 orbits/day pass through SAA no data loss for seismo channel, but increased noise level - Data loss due to solar panel rotation + flat field calibration: 1 orbit per 10 days - Data loss due to SEUs: 0.15 % of (rebinned) dataset - Data loss due to eclipse entries/exits: 20 s per orbit - Data loss due to technical failures: the longer the more rare, longest: +/- 6 days, about once a year - Barycentric time correction applied

8. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group

9. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group

10. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group

11. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group

12. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group Mode Identification Five high amplitude peaks  l = 0,1,2  One isolated peak at f 2 = 82.963  Hz  l = 0  One quintuplet containing f 3 and f 5  f 3 = 80.013  Hz is l = 2, m = 0  One quintuplet containing f 4  f 4 = 43.704  Hz is l = 2, m = 0

13. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group Method  Given : the error box in [log Te, log g] diagram log Te = [4.34,4.36] log g = [3.70,3.90]  On each sequence of evolution, i.e. for each (M,  ov,Z,X), find the model which fits f 2  fixes the age of the model  Among these, find models which also fit f 3 and f 4  Constraints on M,  ov,Z,X  Finally, check that all peaks in the spectrum can be explained by unstable modes

14. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group

15. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group

16. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group

17. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group

18. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group

19. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group

20. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group

21. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group Conclusions Frequencies given at a precision of 2 x 10 –4  Error bars on parameters More precision on frequencies  smaller errors bars Frequency analysis  output frequencies identical to input frequencies except where crowded Even there, most frequencies are recovered exactly down to very low amplitudes Modes of high degree (example shown : l = 5)  discriminate between several solutions if in a crowded region  NOT detectable with ground-based telescopes  COROT

22. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group BAG HH1-Frequency analysis 31 frequencies

23. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group BAG HH1-Mode identification l=0l=1 l=2 5 or more multiplets

24. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group June 3-7 2003 Corot Week 4 Belgian Asteroseismology Group HH1 - Seismic analysis

25. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group June 3-7 2003 Corot Week 4 Belgian Asteroseismology Group

26. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group June 3-7 2003 Corot Week 4 Belgian Asteroseismology Group

27. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group June 3-7 2003 Corot Week 4 Belgian Asteroseismology Group

28. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group June 3-7 2003 Corot Week 4 Belgian Asteroseismology Group

29. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group Conclusions  Ground-based observations : l = 0,1,2  Observations from space : l >>>  More frequencies  more constraints on stellar parameters  COROT should observe B stars

30. June 3-7 2003Corot Week 4 Belgian Asteroseismology Group Screenplay : Belgian Asteroseismology Group Starring : Aerts Conny – KU-Leuven Ausseloos Mario – Ulg Barban Caroline – KU-Leuven Briquet Maryline – KU-Leuven Bourge Pierre-Olivier – Ulg Cuypers Jan – ROB Daszynska Jadwiga – KU-Leuven De Cat Peter – KU-Leuven De Ridder Joris – KU-Leuven Dupret Marc-Antoine – Ulg Montalban Josefina – ULg Noels Arlette – Ulg Scuflaire Richard – Ulg Thoul Anne – Ulg Uytterhoeven Katrien – KU-Leuven