P-type pulsators on the main sequence of HR Diagram Gyöngyi Kerekes COROT-day Budapest March, 2007.

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Presentation transcript:

P-type pulsators on the main sequence of HR Diagram Gyöngyi Kerekes COROT-day Budapest March, 2007

HRD δ Scuti β Cephei SPB γ Doradus

Comparison TypePeriod Amplitude (in magnitude) Spectral type β Cephei3-8 hours B2-B5 δ Scuti1-3 hours A0-F5

δ Scuti HD V mag = 7.81 Spectral type: A2 Outside of the instability strip, blue edge Reopens the problem of variability

Whitening

Fitting

Frequencies of HD Frequency (cycle/day) Amplitude (magnitude) Phase Noise (S/N) Frequency (cycle/day) Amplitude (magnitude) Phase Noise (S/N)

β Cephei stars Known since solar masses Main pulsation modes  radial But non-radial pulsations also detected Large fraction is multiperiodic Frequency spectrum is not too dense  modelling becomes possible Very interesting from astroseismologic point of view

β Cephei HD Main target of the first COROT long run V mag = 8.3 Spectral type: B 1.5

Whitening

Fitting

Frequencies Frequency (cycle/day) Amplitude (magnitude) Phase Noise (S/N) Frequency (cycle/day) Amplitude (magnitude) Phase Noise (S/N)

Conclusions Main obtained frequencies: Trends in light curves ↓ Further cleanings are required HD belongs to small amplitude δ Scuti s → maybe more modes are excited → COROT’s task to investigate if there are more modes δ Scuti HD β Cephei HD

Thank you for your attention!