2 research outputs found
Kepler-80 Revisited: Assessing the Participation of a Newly Discovered Planet in the Resonant Chain
In this paper, we consider the chain of resonances in the Kepler-80 system
and evaluate the impact that the additional member of the resonant chain
discovered by Shallue & Vanderburg (2018) has on the dynamics of the system and
the physical parameters that can be recovered by a fit to the transit timing
variations (TTVs). Ultimately, we calculate the mass of Kepler-80 g to be when assuming all planets have zero eccentricity, and when relaxing that assumption. We show that the outer
five planets are in successive three-body mean-motion resonances (MMRs). We
assess the current state of two-body MMRs in the system and find that the
planets do not appear to be in two-body MMRs. We find that while the existence
of the additional member of the resonant chain does not significantly alter the
character of the Kepler-80 three-body MMRs, it can alter the physical
parameters derived from the TTVs, suggesting caution should be applied when
drawing conclusions from TTVs for potentially incomplete systems. We also
compare our results to those of MacDonald et al. (2021), who perform a similar
analysis on the same system with a different method. Although the results of
this work and MacDonald et al. (2021) show that different fit methodologies and
underlying assumptions can result in different measured orbital parameters, the
most secure conclusion is that which holds true across all lines of analysis:
Kepler-80 contains a chain of planets in three-body MMRs but not in two-body
MMRs.Comment: Accepted to A
HD 219134 Revisited: Planet d Transit Upper Limit and Planet f Transit Nondetection with ASTERIA and TESS
HD 219134 is a K3V dwarf star with six reported radial-velocity discovered planets. The two innermost planets b and c show transits, raising the possibility of this system to be the nearest (6.53 pc), brightest (V = 5.57) example of a star with a compact multiple transiting planet system. Ground-based searches for transits of planets beyond b and c are not feasible because of the infrequent transits, long transit duration (~5 hr), shallow transit depths (<1%), and large transit time uncertainty (~half a day). We use the space-based telescopes the Arcsecond Space Telescope Enabling Research in Astrophysics (ASTERIA) and the Transiting Exoplanet Survey Satellite (TESS) to search for transits of planets f (P = 22.717 days and M sin i = 7.3 ± 0.04M_⊕) and d (P = 46.859 days and M sin i = 16.7 ± 0.64M_⊕). ASTERIA was a technology demonstration CubeSat with an opportunity for science in an extended program. ASTERIA observations of HD 219134 were designed to cover the 3σ transit windows for planets f and d via repeated visits over many months. While TESS has much higher sensitivity and more continuous time coverage than ASTERIA, only the HD 219134 f transit window fell within the TESS survey's observations. Our TESS photometric results definitively rule out planetary transits for HD 219134 f. We do not detect the Neptune-mass HD 219134 d transits and our ASTERIA data are sensitive to planets as small as 3.6 R_⊕. We provide TESS updated transit times and periods for HD 219134 b and c, which are designated TOI 1469.01 and 1469.02 respectively