Corot 2009 - HD180642 - A.Thoul Modeling of HD180642 = V1449 Aql (THE only  Cephei star main target of CoRoT). Anne Thoul + Maryline Briquet, Pieter Degroote,

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Corot HD A.Thoul Modeling of HD = 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

Corot HD A.Thoul HD photometry spectroscopy Z obs = Data from T. Morel, E.Niemczura et al.

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

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

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

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

Corot HD A.Thoul HD 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

Corot HD A.Thoul HD 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

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

Corot HD A.Thoul HD 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

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

Corot HD A.Thoul HD 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

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

Corot HD A.Thoul HD 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

Corot HD A.Thoul HD n=3 n=2 n=1

Corot HD A.Thoul HD 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

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

Corot HD A.Thoul HD n=1 n=2 n=3

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

Corot HD A.Thoul HD TAMS MS

Corot HD A.Thoul HD TAMS MS

Corot HD A.Thoul HD180642

Corot HD A.Thoul HD photometry spectroscopy

Corot HD A.Thoul HD 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

Corot HD A.Thoul HD 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

Corot HD A.Thoul HD 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

Corot HD A.Thoul HD 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 HD A.Thoul HD 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 HD A.Thoul HD 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!