Indirect and direct [[Methods of detecting exoplanets|observation methods]] such as radial velocity and [[coronagraph]]s can give envelope estimates of exoplanet parameters such as mass, planetary radius, and orbital radius/eccentricity. Since distance from the host star and planetary size are generally believed to influence exoplanet geodynamic regime, inferences can be drawn from such information. For example, an exoplanet close enough to its host star to be [[Tidal locking|tidally locked]] may have drastically different “dark” and “light” side temperatures and correspondingly bipolar geodynamic regimes (see insolation section below). | Indirect and direct [[Methods of detecting exoplanets|observation methods]] such as radial velocity and [[coronagraph]]s can give envelope estimates of exoplanet parameters such as mass, planetary radius, and orbital radius/eccentricity. Since distance from the host star and planetary size are generally believed to influence exoplanet geodynamic regime, inferences can be drawn from such information. For example, an exoplanet close enough to its host star to be [[Tidal locking|tidally locked]] may have drastically different “dark” and “light” side temperatures and correspondingly bipolar geodynamic regimes (see insolation section below). |