Detection of Close-In Extrasolar Giant Planets Using the Fourier-Kelvin Stellar Interferometer

@article{Danchi2003DetectionOC,
  title={Detection of Close-In Extrasolar Giant Planets Using the Fourier-Kelvin Stellar Interferometer},
  author={William C. Danchi and Drake L. Deming and Marc J. Kuchner and Sara Seager},
  journal={The Astrophysical Journal Letters},
  year={2003},
  volume={597},
  pages={L57 - L60}
}
We evaluate the direct detection of extrasolar giant planets with a two-aperture nulling infrared interferometer, working at angles θ < λ/2B and using a new "ratio-of-two-wavelengths" technique. Simple arguments suggest that interferometric detection and characterization should be quite possible for planets much closer than the conventional inner working angle, or angular resolution limit. We show that the peak signal from a nulling infrared interferometer of baseline ≲40 m will often occur… 
The Fourier-Kelvin Stellar Interferometer: A Progress Report and Preliminary Results from our Laboratory Testbed
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Characterisation of zodiacal environment of stellar targets for future missions dedicated to the direct detection of extrasolar planets
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CALIBRATING AN INTERFEROMETRIC NULL
One of the biggest challenges associated with a nulling-interferometer-based approach to detecting extrasolar Earth-like planets comes from the extremely stringent requirements of path length,
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Precise Doppler experiments suggest that a massive (m sin i = 0.86MJ) planet orbits at semimajor axis a = 3.4 AU around ϵ Eri, a nearby star with a massive debris disk. The dynamical perturbations
Nulling interferometry: performance comparison between space and ground-based sites for exozodiacal disc detection
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Imaging properties of rotating nulling interferometers.
  • O. Lay
  • Physics
    Applied optics
  • 2005
TLDR
The synthesized point-spread function for a rotating nulling interferometer utilizing phase chopping is shown to consist of a main peak, satellite peaks, and their associated sidelobes, and simple analytic expressions are derived for the modulation efficiency and angular resolution.
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