Extrasolar Planets
A Near-Infrared Chemical Inventory Of The Atmosphere Of 55 Cancri e 
We present high-resolution near-infrared spectra taken during eight transits of 55 Cancri e, a nearby low-density super-Earth with a short orbital period (< 18 hours).
Exoplanets Prediction in Multiplanetary Systems
We present the results of a search for additional exoplanets in all multiplanetary systems discovered to date, employing a logarithmic spacing between planets in our Solar System known as the Titius-Bode (TB) relation.
A Readily Implemented Atmosphere Sustainability Constraint for Terrestrial Exoplanets Orbiting Magnetically Active Stars
With more than 4,300 confirmed exoplanets and counting, the next milestone in exoplanet research is to determine which of these newly found worlds could harbor life.
Impact Of Photochemical Hazes And Gases On Exoplanet Atmospheric Thermal Structure
We investigate the impact of photochemical hazes and disequilibrium gases on the thermal structure of hot-Jupiters, using a detailed 1-D radiative-convective model.
Relative Occurrence Rates Of Terrestrial Planets Orbiting FGK Stars
This paper aims to derive a map of relative planet occurrence rates that can provide constraints on the overall distribution of terrestrial planets around FGK stars.
Aerosols In Exoplanet Atmospheres
Observations of exoplanet atmospheres have shown that aerosols, like in the Solar System, are common across a variety of temperatures and planet types. The formation and distribution of these aerosols are inextricably intertwined with the composition and thermal structure of the atmosphere.
Revisiting the Planet Mass and Stellar Metallicity Relation for Low-Mass Exoplanets Orbiting GKM Class Stars
The growing database of exoplanets have shown us the statistical characteristics of various exoplanet populations, providing insight towards their origins.
The Epoch of Giant Planet Migration Planet Search Program. I. Near-Infrared Radial Velocity Jitter of Young Sun-like Stars
We present early results from the Epoch of Giant Planet Migration program, a precise RV survey of over one hundred intermediate-age (∼20−200 Myr) G and K dwarfs with the Habitable-Zone Planet Finder spectrograph (HPF) at McDonald Observatory's Hobby-Eberly Telescope (HET).
Around Which Stars Can TESS Detect Earth-like Planets? The Revised TESS Habitable Zone Catalog
In the search for life in the cosmos, NASA's Transiting Exoplanet Survey Satellite (TESS) mission has already monitored about 74% of the sky for transiting extrasolar planets, including potentially habitable worlds.
Probing The Capability Of Future Direct Imaging Missions To Spectrally Constrain The Frequency Of Earth-like Planets
A critical question in astrobiology is whether exoEarth candidates (EECs) are Earth-like, in that they originate life that progressively oxygenates their atmospheres similarly to Earth. We propose answering this question statistically by searching for O2 and O3 on EECs with missions such as HabEx or LUVOIR.
Characterizing Atmospheres of Transiting Earth-like Exoplanets Orbiting M Dwarfs with James Webb Space Telescope
A number of transiting, potentially habitable Earth-sized exoplanets have recently been detected around several nearby M dwarf stars. These worlds represent important targets for atmospheric characterization for the upcoming NASA James Webb Space Telescope.
Searching for Small Circumbinary Planets I. The STANLEY Automated Algorithm and No New Planets in Existing Systems
No circumbinary planets have been discovered smaller than 3 Earth radii, yet planets of this small size comprise over 75% of the discoveries around single stars.
Possible Atmospheric Diversity Of Low Mass Exoplanets, Some Central Aspects
Exoplanetary science continues to excite and surprise with its rich diversity. We discuss here some key aspects potentially influencing the range of exoplanetary terrestrial-type atmospheres which could exist in nature.
Magnetospheres of Terrestrial Exoplanets and Exomoons: Implications for Habitability and Detection
Characterizing habitable exoplanets and/or their moons is of paramount importance. Here we show the results of our magnetic field topological modeling which demonstrate that terrestrial exoplanet-exomoon coupled magnetospheres work together to protect the early atmospheres of both the exoplanet and the exomoon.
The Fundamental Connections Between the Solar System and Exoplanetary Science
Over the past several decades, thousands of planets have been discovered outside of our Solar System. These planets exhibit enormous diversity, and their large numbers provide a statistical opportunity to place our Solar System within the broader context of planetary structure, atmospheres, architectures, formation, and evolution.
The Tierras Observatory: An Ultra-precise Photometer To Characterize Nearby Terrestrial Exoplanets
We report on the status of the Tierras Observatory, a refurbished 1.3-m ultra-precise fully-automated photometer located at the F. L. Whipple Observatory atop Mt. Hopkins, Arizona.
Lava Worlds: From Early Earth to Exoplanets
The magma ocean concept was first conceived to explain the geology of the Moon, but hemispherical or global oceans of silicate melt could be a widespread "lava world" phase of rocky planet accretion, and could persist on planets on short-period orbits around other stars.
Planet Cartography With Neural Learned Regularization
Finding potential life harboring exo-Earths is one of the aims of exoplanetary science. Detecting signatures of life in exoplanets will likely first be accomplished by determining the bulk composition of the planetary atmosphere via reflected/transmitted spectroscopy.
A Distinct Population of Small Planets: Sub-Earths
There is a well-known gap in the sizes of small planets, between super-Earths and mini-Neptunes. This is explained by the envelope stripping of mini-Neptunes at short orbits.
The Role of Early Giant Planet Instability in the Terrestrial Planet Formation
The terrestrial planets are believed to have formed by violent collisions of tens of lunar- to Mars-size protoplanets at time t<200 Myr after the protoplanetary gas disk dispersal (t_0).
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