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1. The Stars Kepler Missed: Investigating the Kepler Target Selection Function Using Gaia DR2

   https://doi.org/10.3847/1538-3881/abee1d  

   Wolniewicz, Linnea M.; Berger, Travis A.; Huber, Daniel (April 2021, The Astronomical Journal)
2. The Gaia–Kepler Stellar Properties Catalog. II. Planet Radius Demographics as a Function of Stellar Mass and Age

   https://doi.org/10.3847/1538-3881/aba18a  

   Berger, Travis A.; Huber, Daniel; Gaidos, Eric; van Saders, Jennifer L.; Weiss, Lauren M. (September 2020, The Astronomical Journal)

   null (Ed.)
3. Kepler and TESS Observations of PG 1159-035

   https://doi.org/10.3847/1538-4357/ac8871  

   Oliveira da Rosa, Gabriela; Kepler, S. O.; Córsico, Alejandro H.; Costa, J. E. S.; Hermes, J. J.; Kawaler, S. D.; Bell, Keaton J.; Montgomery, M. H.; Provencal, J. L.; Winget, D. E.; et al (September 2022, The Astrophysical Journal)

   Abstract PG 1159-035 is the prototype of the PG 1159 hot (pre-)white dwarf pulsators. This important object was observed during the Kepler satellite K2 mission for 69 days in 59 s cadence mode and by the TESS satellite for 25 days in 20 s cadence mode. We present a detailed asteroseismic analysis of those data. We identify a total of 107 frequencies representing 32ℓ= 1 modes, 27 frequencies representing 12ℓ= 2 modes, and eight combination frequencies. The combination frequencies and the modes with very highkvalues represent new detections. The multiplet structure reveals an average splitting of 4.0 ± 0.4μHz forℓ= 1 and 6.8 ± 0.2μHz forℓ= 2, indicating a rotation period of 1.4 ± 0.1 days in the region of period formation. In the Fourier transform of the light curve, we find a significant peak at 8.904 ± 0.003μHz suggesting a surface rotation period of 1.299 ± 0.002 days. We also present evidence that the observed periods change on timescales shorter than those predicted by current evolutionary models. Our asteroseismic analysis finds an average period spacing forℓ= 1 of 21.28 ± 0.02 s. Theℓ= 2 modes have a mean spacing of 12.97 ± 0.4 s. We performed a detailed asteroseismic fit by comparing the observed periods with those of evolutionary models. The best-fit model hasT_eff= 129, 600 ± 11 100 K,M_*= 0.565 ± 0.024M_⊙, and $\log g={7.41}_{-0.54}^{+0.38}$, within the uncertainties of the spectroscopic determinations. We argue for future improvements in the current models, e.g., on the overshooting in the He-burning stage, as the best-fit model does not predict excitation for all of the pulsations detected in PG 1159-035. 

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4. Photometric and Spectroscopic Properties of Type Ia Supernova 2018oh with Early Excess Emission from the Kepler 2 Observations

   https://doi.org/10.3847/1538-4357/aaec74  

   Li, W.; Wang, X.; Vinkó, J.; Mo, J.; Hosseinzadeh, G.; Sand, D. J.; Zhang, J.; Lin, H.; Zhang, T.; Wang, L.; et al (January 2019, The Astrophysical Journal)
5. Dynamics and Origins of the Near-resonant Kepler Planets

   https://doi.org/10.3847/1538-4357/acc9ae  

   Goldberg, Max; Batygin, Konstantin (April 2023, The Astrophysical Journal)

   Abstract Short-period super-Earths and mini-Neptunes encircle more than ∼50% of Sun-like stars and are relatively amenable to direct observational characterization. Despite this, environments in which these planets accrete are difficult to probe directly. Nevertheless, pairs of planets that are close to orbital resonances provide a unique window into the inner regions of protoplanetary disks, as they preserve the conditions of their formation, as well as the early evolution of their orbital architectures. In this work, we present a novel approach toward quantifying transit timing variations within multiplanetary systems and examine the near-resonant dynamics of over 100 planet pairs detected by Kepler. Using an integrable model for first-order resonances, we find a clear transition from libration to circulation of the resonant angle at a period ratio of ≈0.6% wide of exact resonance. The orbital properties of these systems indicate that they systematically lie far away from the resonant forced equilibrium. Cumulatively, our modeling indicates that while orbital architectures shaped by strong disk damping or tidal dissipation are inconsistent with observations, a scenario where stochastic stirring by turbulent eddies augments the dissipative effects of protoplanetary disks reproduces several features of the data. 

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