AP summary

1
AP summary Corot Be star group
GEPI, Meudon Hubert, Floquet, Martayan, Frémat,
Neiner Univ. Valencia Fabregat, Gutiérrez-Soto,
Suso Brazil Janot-Pacheco, Andrade, Daflon in
collaboration with the B stars group (Aerts et
al.)
2
Search for faint Be stars in the exoplanet fields

• Spectroscopy with the VLT/Giraffe
• Ha and R photometry with the WFI/INT Stromgren
  photometry
• IR photometry with IRAC/Spitzer
• ? Program accepted for AO1

3
Spectroscopy with Giraffe Hubert et al.

• - with VLT/Giraffe multifiber spectrograph
• parts of first anticenter long run field
• study B stars to detect emission in Ha
• ? 2 faint Be stars detected...
• ? see CW8 (Hubert et al.)

4
Optical photometry with the INT Fabregat et al.

• with WFI/INT (La Palma) with Ha and Sloan R
  filters ?detect emission line stars
• whole exoplanet field of the first long run
  towards the galactic center done in August 2005
  (8 pointings 4 CCDs)
• more observations in December 2005 for the
  exoplanet field of the first long run toward the
  galactic anticenter

5
Figure shows 1/32 of the whole field (1917 stars
with Rlt16.5) ? we expect to detect 300 emission
line stars in the whole field
6
Stromgren photometry Fabregat et al.

• Stromgren photometry of the whole field already
  obtained, but not yet reduced
• allows to perform a photometric spectral
  classification of the detected emission line
  stars
• ? detect Be stars (30 for center field) among
  emission line stars

Diagram without reddening m1-c1
7
IR photometry with Spitzer Neiner et al.

• - photometry in 4 IR bands with Spitzer/IRAC
• - half of first anticenter field observed in 2004
• 30000 stars detected and identified in each
  band
• cross-correlation with 2MASS, DENIS and Corotsky
• analysis of SEDs to find OB stars with IR excess
• ? detection of 10 Be stars
• (in anticenter field)

8
Possible Be star observed with Spitzer
Typical Be star SED
9
Faint Be stars discovered for Corot

• Anticenter field
• - 2 Be stars with Giraffe
• 10 Be stars with Spitzer
• 4 Be stars with Calar Alto (see Fabregat et al.,
  CW5)
• a few Be stars with the INT (to be observed in 2
  weeks...)
• Center field
• 30 Be stars in the center field with the INT

10
Program accepted for AO1 collaboration Be stars
group and B stars group

• Observed all faint Be stars (40) some B stars
  (250) in the center and anticenter fields
• ?Search for signatures of rotational modulation
  and pulsations
• Perform seismic modelling of the stellar interior
  structure
• Statistical study to fine-tune the excitation
  mechanism in B stars and calibrate evolutionary
  models
• Study occurence of Be phenomenon and relation
  with pulsations, magnetic field, rotation
• Link between Be outbursts and pulsation beating