Simulations of Infrared Very Long Baseline Interferometry of the Exoplanets Gliese 581c and Gliese 581d

Details Simulations of Infrared Very Long Baseline Interferometry of the Exoplanets Gliese 581c and Gliese 581d Simulations of Infrared Very Long Baseline Interferometry of the Exoplanets Gliese 581c and Gliese 581d

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008jsara...2...55p&link_type=abstract

Journal of the Southeastern Association for Research in Astronomy, vol. 2, p. 55-58

Astronomy and Astrophysics

Astronomy

Solar System: General, Stars: Individual (Gl 581), Techniques: Interferometric

Scientific paper

There are several potential advantages to the use of interferometry for direct detection of extrasolar planetary emission. Destructive interference can be used to strongly suppress emission from the much brighter primary star. High angular resolution, which can be significantly better that the diffraction limit of the individual telescopes, will help to separate the emission from an extrasolar planet and its primary star as well as from sources of background emission. This paper presents research and calculations pertaining to the development of a preliminary model of an interferometer designed to detect mid-IR emissions from Gl 581c and GL 581d ( Bloh et al. 2007). The instrument model is used to analyze emissions from Gl 581d based on a simple model atmosphere and radiative transfer calculation. The atmosphere is assumed to be a pure CO2 blackbody with a single temperature, the effective temperature, and the surface a blackbody 100 K warmer. The surface is broken up into 32 subsections of equal latitude and longitude intervals and a disk averaged spectrum is calculated.

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