Study of the composition, structure, and dynamics of exoplanet atmospheres through spectroscopy, photometry, and modeling.
Planetary atmospheres: Understanding the characteristics and dynamics of atmospheres surrounding planets, including Earth, Mars, Venus, and Jupiter.
Exoplanet detection methods: Learning how scientists detect exoplanets using various methods, such as radial velocity, transit, and microlensing.
Stellar properties: Exploring the properties of stars that host exoplanets, such as their size, mass, age, and chemical composition.
Atmosphere modeling: Understanding the principles behind modeling planetary atmospheres using computer simulations and numerical methods.
Atmospheric composition: Studying the chemical composition of exoplanet atmospheres, including the abundance of various elements and molecules such as water, carbon dioxide, and methane.
Clouds and Hazes: Exploring how clouds and hazes in exoplanet atmospheres affect the transmission and emission spectra of exoplanets.
Energy balance and climate: Understanding how energy from the host star is absorbed and redistributed in exoplanet atmospheres, affecting atmospheric circulation and climate.
Atmospheric dynamics: Analyzing the dynamics of exoplanet atmospheres, such as the formation of weather patterns and atmospheric circulation.
Biosignatures: Learning how certain molecules in exoplanet atmospheres, such as oxygen and methane, could potentially indicate the presence of life.
Spectroscopy: Understanding the principles behind analyzing the different wavelengths of light emitted or absorbed by exoplanet atmospheres using spectroscopy techniques.
Instrumentation: Exploring the technologies and instruments used to observe and study exoplanet atmospheres, such as telescopes, coronagraphs, and spectrometers.
Data analysis: Learning how scientists analyze and interpret the data from exoplanet observations, including performing statistical analyses and identifying trends.
Planetary formation and evolution: Exploring the theories behind how exoplanets formed and evolved, and how their atmospheres may have changed over time.
Habitability: Studying the conditions necessary for exoplanets to be habitable, such as the presence of liquid water, a stable climate, and a protective atmosphere.
Planetary system architecture: Exploring the organization and dynamics of planetary systems beyond our own, including the potential for multiple planet systems and orbital resonances.
Hydrogen-dominated atmospheres: These are atmospheres that primarily consist of hydrogen gas. They are mostly found in gas giants and have very low densities.
Helium-dominated atmospheres: These are atmospheres that are dominated by helium gas. They are also found in gas giants and have a higher density than hydrogen-dominated atmospheres.
Carbon-rich atmospheres: These are atmospheres where the abundance of carbon is higher than that of oxygen. They are usually found in planets that are closer to their star and have temperatures higher than 800 Kelvin.
Oxygen-rich atmospheres: These are atmospheres where the abundance of oxygen is higher than that of carbon. They tend to be found in planets that are farther away from their star and have temperatures lower than 800 Kelvin.
Nitrogen-rich atmospheres: These are atmospheres where the abundance of nitrogen is higher than other elements like oxygen and carbon. They are usually found in planets that are farther away from their star and have temperatures lower than 500 Kelvin.
Methane atmospheres: These are atmospheres that are rich in methane gas. They are typically found in planets that have temperatures between 200 Kelvin to 300 Kelvin.
Water vapor atmospheres: These are atmospheres that contain a significant amount of water vapor. They tend to be found in planets that are at moderate temperatures and are located in the habitable zone of their star.
Cloud and haze-dominated atmospheres: These are atmospheres that are dominated by clouds and haze. They are usually found in planets that are warmer than Neptune and have a high atmospheric pressure.