Larissa

Larissa is a fascinating moon in our Solar System that has captured the attention of astronomers and space enthusiasts alike. With a Larissa radius of 97 km, making it 65.7× 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 73,548 km (0.000 AU) from the Sun, Larissa occupies a significant place in the Solar System's architecture. As a moon, Larissa demonstrates the incredible diversity of natural satellites that orbit larger celestial bodies throughout our Solar System.

The Larissa physical characteristics reveal a world of remarkable dimensions and properties. The Larissa radius measures 97 km, making it 65.7× smaller than Earth's size. The Larissa mass of 5.00e+18 kg represents 1194400.0× smaller than Earth's mass, giving this world substantial gravitational influence. The Larissa density of 1 g/cm³ (5.5× smaller than Earth's density) provides clues about its internal composition, while the surface gravity of 0.034 m/s² (288.5× 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 Larissa orbit reveals fascinating details about its journey around the Sun and its relationship to other Solar System objects. The Larissa orbit has a semimajor axis of 73,548 km (0.000 AU), placing it 2034.0× smaller than Earth's distance from the Sun. The Larissa orbit is nearly circular with an eccentricity of 0.001 (11.9× smaller than Earth's orbital eccentricity), resulting in relatively stable solar heating throughout its year. The Larissa orbit takes 0.00 hours to complete (56897411.9× smaller than Earth's orbital period), defining the length of its year. The orbital inclination of 0.2° indicates how much the Larissa orbit is tilted relative to the Solar System's ecliptic plane. This low inclination means Larissa follows a path very close to the plane where most planets orbit, suggesting a stable formation history.

The Larissa rotation and axial orientation provide crucial insights into its daily and seasonal cycles, as well as its orbital dynamics. The Larissa axial tilt of 0° determines the intensity and nature of seasonal variations. With minimal axial tilt, Larissa experiences virtually no seasonal changes, maintaining relatively constant temperatures throughout its year. The orbital orientation parameters reveal additional details about Larissa'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 Larissa temperature and atmospheric conditions are fundamental to understanding its habitability and environmental characteristics. The Larissa average temperature of 0.0 K (-273.1 °C) (-459.7°F) provides the baseline for understanding its climate. These extremely cold temperatures make Larissa 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), Larissa presents a dramatically different thermal environment. Being closer to the Sun than Earth, Larissa receives more intense solar radiation, contributing to its temperature profile.

The Larissa escape velocity and shape characteristics reveal important details about its gravitational field and rotational dynamics. The Larissa 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 Larissa to retain a substantial atmosphere. The Larissa 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.