Announced during the XIX th IAP Colloquium "Extrasolar Planets: Today & Tormorrow", Paris, June 2003 (Mayor et al.)
The planetary signal is not seen in the AAT data (Jones et al., XIX IAP colloquium). This is probably due to the poor phase coverage of the small AAT radial-velocity set.
Planetary signature or stellar activity?
- A large ISO Infra-Red excess is detected for HD 10647 (Decin et al. 2000)
- HD 10647 is chromospherically active (log R'HK=-4.68).
- HD 10647: vsini=4.88 km/s
but:
- The calibrated rotational period is more than two orders of magnitude smaller than the observed velocity period (P~1040 d with a false-alarm probability under 0.01%, see periodograms below).
- No photometric variations (flagged as a constant star in the HIPPARCOS catalogue).
- No clear correlation between the line bisectors and the velocities (the bisector span is constant, see the plot below).
Bottom: Residuals around the solution |
showing that the line profiles are not variable. Line profile effects can thus not be responsible for the observed RV variations |
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The maximum near 1000 d is highly significant (at least 4 sigma). |
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Extrasolar planet page
Planet Search and Stellar Kinematics group page
Geneva observatory
University of Geneva