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AP summary Corot Be star group

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

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Presentation Transcript
slide1
AP summary

Corot Be star group

GEPI, Meudon: Hubert, Floquet, Martayan, Fremat, Neiner

Univ. Valencia: Fabregat, Gutiérrez-Soto, Suso

Brazil: Janot-Pacheco, Andrade, Daflon

in collaboration with the B stars group (Aerts et al.)

slide2
Search for faint Be stars in the exoplanet fields
  • Spectroscopy with the VLT/Giraffe
  • Hα and R photometry with the WFI/INT + Stromgren photometry
  • IR photometry with IRAC/Spitzer
  •  Program accepted for AO1
slide3
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 Hα
  •  2 faint Be stars detected...
  •  see CW8 (Hubert et al.)
slide4
Optical photometry with the INT

Fabregat et al.

  • with WFI/INT (La Palma) with Hα and Sloan R filters detect emission line stars
  • whole exoplanet field of the first long run towards the galactic center donein August 2005 (8 pointings * 4 CCDs)
  • more observations in December 2005 for the exoplanet field of the first long run toward the galactic anticenter
slide5
Figure shows 1/32 of the whole field (1917 stars with R<16.5)

 we expect to detect ~300 emission line stars in the whole field

slide6
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]

slide7
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)
slide8
2MASS

Be

Black-body B

B

IR excess

Spitzer colors

Possible Be star observed with Spitzer

Typical Be star SED

slide9
Faint Be stars discovered for Corot
  • Anticenter field:
  • - 2 Be stars with Giraffe
  • 10 Be stars with Spitzer
  • a few Be stars with the INT (to be reduced...)
  • Center field:
  • ~30 Be stars in the center field with the INT
slide10
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
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