Direct Observation of Extrasolar Planets With an Infrared Interferometer

Details Direct Observation of Extrasolar Planets With an Infrared Interferometer Direct Observation of Extrasolar Planets With an Infrared Interferometer

Sep 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996dps....28.1207m&link_type=abstract

American Astronomical Society, DPS meeting #28, #12.07; Bulletin of the American Astronomical Society, Vol. 28, p.1112

Astronomy and Astrophysics

Astronomy

Scientific paper

The unexpected discovery of Jupiter-size planets very close to their parent stars (such as 51 Peg B) creates a challenge for theories of planetary formation and structure. Only a direct measurement of their mass and luminosity (not accessible via the current radial velocity techniques) can help discriminate between the different planetary models that have been proposed for this new class of objects. Direct observation of such extrasolar planets with an infrared interferometer is a difficult task because of the very high dynamic range required (typically 10(3) to 10(4) ), but not impossible if a very careful spatial filtering and calibration is imposed upon the recombined beams. Dynamic ranges of 10(3) have already been demonstrated on selected stars with the FLUOR fiber recombination unit at the IOTA interferometer. We propose here an observing strategy to monitor hot extrasolar planets of the 51 Peg class, for which the next generation IR interferometers (VLTI, Keck...) provide a set of adequate baselines and a sufficient sensitivity. Simulations show that with the current fiber beam combination technology, the photometry of the planet can be established within 10%, and the inclination of its orbit within 10 degrees, in less than 2 months of observing time.

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