ExoExplorers

Abstract: A rich diversity of extrasolar planetary systems has been discovered in recent decades, with many displaying unexpected architectures that challenge theories of planet formation informed by the Solar System. In particular, many giant planets have high orbital eccentricities, and many others orbit extremely close to their host stars. A proposed solution to both of these puzzles is high-eccentricity migration, in which an initially distant “cold” Jupiter is excited to high eccentricities, allowing for tidal interactions during close passages that drag the planet onto a close-in “hot” orbit. Secular (long-term) perturbations from a third body of planetary or stellar nature are a potential source of the eccentricity excitations, a phenomenon known as the Eccentric Kozai-Lidov (EKL) mechanism. I will discuss novel insights into the three-body problem that provide a new analytical understanding of the eccentricity evolution of planets subject to EKL from a distant perturber. Then, I will discuss recent work to characterize the effect of EKL from stellar companions on the giant planet population. We perform a population synthesis study of cold giant planets in stellar binaries, including the additional effects of tides, general relativity, and stellar evolution. The eccentricity distribution of the cold Jupiters is calculated, considering that planet-planet scattering may generate modest eccentricities on ~Myr timescales before EKL shapes the distribution on ~Myr-Gyr timescales. We find that the simulated eccentricity distribution is statistically consistent with the observed sample, suggesting that the EKL mechanism in stellar binaries may play an important role in driving the eccentricities of cold Jupiters and contributing to the formation of hot Jupiters.

Abstract:The disintegrating ultra-short period rocky exoplanet K2-22b periodically emits dusty clouds in a dynamically chaotic process resulting in a variable transit depth from 0-1.3%. The effluents that sublimate off the surface and condense out in space are probably representative of the formerly interior layers convectively transported to the molten surface. Transmission spectroscopy of these transiting clouds reveal spectral fingerprints of the interior composition of this rocky world. We used JWST's Mid-Infrared Instrument (MIRI) as a low-resolution slitless spectrograph to observe four predicted transit windows for K2-22b. For each observation, we extracted a transmission spectrum over the spectral range of 4.3-11.8 μm. We detect one transit at high significance and two at low significance. We find that the data 1) disfavor featureless, iron-dominated core material, 2) are consistent with some form of magnesium silicate minerals, likely from mantle material, and 3) show a distinct and unexpected feature at ∼5 μm. The unexpected feature, also seen weakly in the low-significance transits, is consistent with some gas features, possibly NO and/or CO2. These findings warrant further study to improve the constraints on the composition of this disintegrating rocky world.

Abstract: Multi-planet system architectures are powerful tools to constrain the evolutionary pathways of observed exoplanets. Therefore, understanding the predictive and descriptive power of empirical models of system architectures is critical to probing system formation histories. In this work, we analyzed 52 TESS multi-planet systems previously studied using DYNAMITE (Dietrich & Apai, 2020), who used empirical models based on Kepler planets to predict additional planets in each system. We used additional TESS data to search for these predicted planets, and thereby evaluated the predictive power of the underlying empirical models. Specifically, we studied whether a period ratio method or clustered period model more accurately predicted additional planets. We found that neither model is highly predictive, highlighting the need for additional data and nuanced models to describe the full exoplanet population.

Abstract: In just a few short years, JWST has already revolutionized our understanding of exoplanetary atmospheres. However, cutting edge characterization is still being done with ground-based facilities. Space-based, low resolution spectroscopy (such as with JWST) and ground-based, high resolution spectroscopy are the two main avenues with which we can study transiting exoplanet atmospheres. In this talk, I will discuss the differing capabilities of these two methods for measuring and interpreting exoplanet atmospheric spectra, and I will highlight ways in which ground-based spectroscopy in particular is transforming our understanding of planet formation and climate. Additionally, high and low resolution spectroscopy have complementary strengths and weaknesses, and the combination of the two can provide a more powerful probe of a planet's atmosphere than can be achieved by either method individually. I will describe how combining the two methods can result in more precise inferences and more comprehensive pictures of a planet's atmosphere.