TTV constraints on additional planets in the WD 1856+534 system

Author:

Kubiak Sarah12ORCID,Vanderburg Andrew3ORCID,Becker Juliette24ORCID,Gary Bruce5ORCID,Rappaport Saul A3ORCID,Xu Siyi6ORCID,de Beurs Zoe7ORCID

Affiliation:

1. Department of Journalism and Media Communication, Colorado State University , Fort Collins, CO 80521 , USA

2. Department of Astronomy, University of Wisconsin–Madison , 475 N. Charter Street, Madison, WI 53703 , USA

3. Department of Physics and Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology , Cambridge, MA 02139 , USA

4. Division of Geological and Planetary Sciences, California Institute of Technology , Pasadena, CA 91125 , USA

5. Hereford Arizona Observatory , Hereford, AZ 85615 , USA

6. Gemini Observatory/NSF’s NOIRLab , 670 N. A’ohoku Place, Hilo, HI 96720 , USA

7. Department of Earth, Atmospheric and Planetary Sciences, Massachusetts Institute of Technology , Cambridge, MA 02139 , USA

Abstract

ABSTRACT 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  per cent 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. We show that existing transit observations can rule out planets with orbital periods less than about 500 d. 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.

Funder

NASA

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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