Kavli Affiliate: Saul A. Rappaport
| First 5 Authors: Sarah Kubiak, Andrew Vanderburg, Juliette Becker, Bruce Gary, Saul A. Rappaport
| Summary:
WD 1856+534 b (or WD 1856 b for short) is the first known transiting planet
candidate around a white dwarf star. WD 1856 b is about the size of Jupiter,
has a mass less than about 12 Jupiter masses, and orbits at a distance of about
2% of an astronomical unit. The formation and migration history of this object
is still a mystery. Here, we present constraints on the presence of long-period
companions (where we explored eccentricity, inclination, mass, and period for
the possible companion) in the WD 1856+534 planetary system from Transit Timing
Variations (TTVs). We show that existing transit observations can rule out
planets with orbital periods less than about 500 days. With additional transit
observations over the next decade, it will be possible to test whether WD 1856
also hosts additional long-period planets that could have perturbed WD 1856 b
into its current close-in orbit.
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