Galatea

Galatea is a fascinating moon in our Solar System that has captured the attention of astronomers and space enthusiasts alike. With a Galatea radius of 88 km, making it 72.4× smaller than Earth's size, this celestial body presents unique characteristics that distinguish it from other objects in our cosmic neighborhood. Positioned at an average distance of 61,953 km (0.000 AU) from the Sun, Galatea occupies a significant place in the Solar System's architecture. As a moon, Galatea demonstrates the incredible diversity of natural satellites that orbit larger celestial bodies throughout our Solar System.

The Galatea physical characteristics reveal a world of remarkable dimensions and properties. The Galatea radius measures 88 km, making it 72.4× smaller than Earth's size. The Galatea mass of 2.00e+18 kg represents 2986000.0× smaller than Earth's mass, giving this world substantial gravitational influence. The Galatea density of 1 g/cm³ (5.5× smaller than Earth's density) provides clues about its internal composition, while the surface gravity of 0.03 m/s² (327.0× smaller than Earth's gravity) determines how objects behave on its surface. The low density indicates a composition dominated by lighter elements, characteristic of gas giants or icy bodies.

The Galatea orbit reveals fascinating details about its journey around the Sun and its relationship to other Solar System objects. The Galatea orbit has a semimajor axis of 61,953 km (0.000 AU), placing it 2414.7× smaller than Earth's distance from the Sun. The Galatea orbit is nearly circular with an eccentricity of 0 (167.0× smaller than Earth's orbital eccentricity), resulting in relatively stable solar heating throughout its year. The Galatea orbit takes 0.00 hours to complete (73605013.4× smaller than Earth's orbital period), defining the length of its year. The orbital inclination of 0.05° indicates how much the Galatea orbit is tilted relative to the Solar System's ecliptic plane. This low inclination means Galatea follows a path very close to the plane where most planets orbit, suggesting a stable formation history.

The Galatea rotation and axial orientation provide crucial insights into its daily and seasonal cycles, as well as its orbital dynamics. The Galatea axial tilt of 0° determines the intensity and nature of seasonal variations. With minimal axial tilt, Galatea experiences virtually no seasonal changes, maintaining relatively constant temperatures throughout its year. The orbital orientation parameters reveal additional details about Galatea's position in space. The mean anomaly of 0° indicates the planet's current position in its orbit relative to its perihelion. The argument of periapsis of 0° shows how the orbit's orientation changes over time due to gravitational perturbations. The longitude of ascending node of 0° defines the reference point where the orbit crosses the ecliptic plane.

The Galatea temperature and atmospheric conditions are fundamental to understanding its habitability and environmental characteristics. The Galatea average temperature of 0.0 K (-273.1 °C) (-459.7°F) provides the baseline for understanding its climate. These extremely cold temperatures make Galatea inhospitable to life as we know it, with any atmosphere likely frozen solid on the surface. Compared to Earth's average temperature of 15°C (59°F), Galatea presents a dramatically different thermal environment. Being closer to the Sun than Earth, Galatea receives more intense solar radiation, contributing to its temperature profile.

The Galatea escape velocity and shape characteristics reveal important details about its gravitational field and rotational dynamics. The Galatea escape velocity of 0 m/s determines how easily objects can break free from its gravitational pull. This relatively low escape velocity means that gases and light molecules can easily escape into space, making it difficult for Galatea to retain a substantial atmosphere. The Galatea flattening of 0.0000% indicates how much the planet's rotation affects its shape. This minimal flattening suggests a nearly spherical shape, indicating either slow rotation or a very rigid internal structure.