![]() Further studies of WD1856+534 b, alongside new dedicated searches for substellar objects around white dwarfs, will shed further light on the mysteries of post-main-sequence planetary systems.Ībstract = "WD1856+534 b is a Jupiter-sized, cool giant planet candidate transiting the white dwarf WD1856+534. WD1856+534 b could have formed either as a result of common envelope evolution or migration under the Kozai–Lidov mechanism. High-altitude cloud decks can allow lower masses. Though the transmission spectrum shows no prominent absorption features, it is sufficiently precise to constrain the mass of WD1856+534 b to be >0.84 M J (to 2σ confidence), assuming a clear atmosphere and a Jovian composition. ![]() We also present a modified radiative transfer prescription. We introduce the concept of a “limb darkening corrected, time-averaged transmission spectrum” and propose that this is more suitable than (R p,λ,l R s) 2 for comparisons to atmospheric models for planets with grazing transits. Consequently, many standard modeling assumptions do not hold. WD1856+534 b provides a unique transit configuration compared to other known exoplanets: the planet is 8× larger than its star and occults over half of the stellar disk during mid-transit. Nevertheless, our phase-folded white light curve reached a precision of 0.12%. This system is challenging to observe due to the faintness of the host star and the short transit duration. ![]() Here, we report an optical transmission spectrum of WD1856+534 b obtained from ten transits using the Gemini Multi- Object Spectrograph. WD1856+534 b is a Jupiter-sized, cool giant planet candidate transiting the white dwarf WD1856+534.
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