Modeling of HD 180642 V 1449 Aql THE

Modeling of HD 180642 = V 1449 Aql (THE only Cephei star main target of Co. Ro. T). Anne Thoul + Maryline Briquet, Pieter Degroote, Andrea Miglio, Josefina Montalban, Conny Aerts, Thierry Morel, Ewa Niemczura, Kévin Belkacem, . . . + the Corot B star Team Corot 2009 - HD 180642 - A. Thoul

HD 180642 spectroscopy photometry Zobs=0. 0099+-0. 0016 Corot 2009 - HD 180642 - A. Thoul Data from T. Morel, E. Niemczura et

HD 180642 dominant radial (l=0) mode l=3 photometry 11 ground independent frequencies from Corot ground spectroscopy Corot 2009 - HD 180642 - A. Thoul Courtesy Pieter Degroote P 62

HD 180642 Degroote, Aerts et al Hipparcos 0. 7 m Swiss telescope 1. 2 m Mercator telescope COROT ASAS photometry df/dt=[7. 6; 14. 4]10 -11 Hz/y df/dt ~ 10 -10 Hz/y Corot 2009 - HD 180642 - A. Thoul

HD 180642 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 Corot 2009 - HD 180642 - A. Thoul

HD 180642 Modelling: using CLES and OSC with AGS 05 and OP opacities Fit the radial mode “Free parameters”: X, Z, ov, M Corot 2009 - HD 180642 - A. Thoul

HD 180642 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 Corot 2009 - HD 180642 - A. Thoul

HD 180642 A. Fit the main frequency with the fundamental radial mode on the main sequence n=2 n=3 n=1 X=0. 72, Z=0. 015, ov=0, M=12 Corot 2009 - HD 180642 - A. Thoul

HD 180642 modelling radial mode with fundamental on MS effect of M and ov (X=0. 72, Z=0. 010) =0. 4 =0. 2 =0. 0 M=12 Corot 2009 - HD 180642 - A. Thoul M=10

HD 180642 modelling radial mode with fundamental on MS effect of Z (X=0. 72, ov=0) Z=0. 010 Z=0. 015 Corot 2009 - HD 180642 - A. Thoul

HD 180642 modelling radial mode with fundamental on MS effect of X (Z=0. 010, ov=0) X=0. 72 X=0. 74 M=12 Corot 2009 - HD 180642 - A. Thoul M=10

HD 180642 radial = fundamental on MS log g fixed by radial mode M~9 M~13 Corot 2009 - HD 180642 - A. Thoul

HD 180642 B. Fit the main frequency with the first overtone of the radial mode on the main sequence n=2 n=3 n=1 X=0. 72, Z=0. 015, ov=0, M=12 Corot 2009 - HD 180642 - A. Thoul

HD 180642 radial mode = first overtone M~13 M~10 radial mode = fundamental Corot 2009 - HD 180642 - A. Thoul

HD 180642 C. Fit the main frequency with the second overtone of the radial mode on the main sequence n=2 n=3 n=1 X=0. 72, Z=0. 015, ov=0. 4, M=10 Corot 2009 - HD 180642 - A. Thoul

HD 180642 n=3 n=2 n=1 Corot 2009 - HD 180642 - A. Thoul

HD 180642 D. Fit the main frequency with a radial mode after the TAMS n=3 n=2 n=1 n=2 n=3 n=2 X=0. 72, Z=0. 010, ov=0. 2, M=10 log Corot 2009 - HD 180642 - A. Thoul

HD 180642 TAMS n=3 n=2 n=1 MS X=0. 72, Z=0. 010, ov=0. 2, M=10 Corot 2009 - HD 180642 - A. Thoul

HD 180642 n=3 n=2 n=1 Corot 2009 - HD 180642 - A. Thoul

HD 180642 TAMS MS df/dt on MS much too small Corot 2009 - HD 180642 - A. Thoul

HD 180642 TAMS MS Corot 2009 - HD 180642 - A. Thoul

HD 180642 TAMS MS Corot 2009 - HD 180642 - A. Thoul

HD 180642 Corot 2009 - HD 180642 - A. Thoul

HD 180642 spectroscopy photometry Corot 2009 - HD 180642 - A. Thoul

HD 180642 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=12 Corot 2009 - HD 180642 - A. Thoul

HD 180642 X=0. 72, Z=0. 015, ov=0, M=9 radial mode is n=1, MS MAD radial mode is n=1, after TAMS radial mode is n=2, after TAMS radial mode is n=3, after TAMS Corot 2009 - HD 180642 - A. Thoul

HD 180642 X=0. 72, Z=0. 015, ov=0. 4, M=12 MAD radial mode is n=1, MS radial mode is n=2, MS radial mode is n=3, MS Corot 2009 - HD 180642 - A. Thoul

HD 180642 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 Corot 2009 - HD 180642 - A. Thoul

HD 180642 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%) Corot 2009 - HD 180642 - A. Thoul

HD 180642 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! Corot 2009 - HD 180642 - A. Thoul