Abstract
In this chapter, we provide a table with the currently available high-precision, interferometrically measured stellar angular diameters (Sect. 3.1), elaborate on a number of individual exoplanetary systems that were characterized by means of interferometric studies (Sect. 3.2), and briefly comment on our overall results (Sect. 3.3).
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- 1.
Note that the concept of optimistic versus conservative HZ boundaries did not exist until 2013 (see Sect. 2.4).
- 2.
The distinction between optimistic and conservative HZ boundaries did not exist in 2011 (see Sect. 2.4).
- 3.
Especially for a transit depth much greater than the one of 55 Cnc e, the question can be asked whether an interferometric measurement obtained during planetary transit or during the presence of star spots could produce a radius estimate that is thus artificially reduced. As seen in van Belle (2008), this effect is expected to be very small. Interferometric visibility variations in a single data point due to a transiting planet will impact current diameter measurements at the δθ ≃ 0. 6% level, buried in the measurement noise of the result based on all obtained visibility measurements. Since spots feature lower contrast ratios than transiting planets, expected visibility variations are even smaller.
- 4.
Due to the grazing transit in the GJ 436 system, limb-darkening models play a larger role in the calculation of the planetary radius calculated than for central transits. Knowing the stellar effective temperature to a higher precision thus provides particularly important constraints for this system.
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von Braun, K., Boyajian, T. (2017). Results. In: Extrasolar Planets and Their Host Stars. SpringerBriefs in Astronomy. Springer, Cham. https://doi.org/10.1007/978-3-319-61198-3_3
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