Erriapus

Erriapus is a fascinating moon in our Solar System that has captured the attention of astronomers and space enthusiasts alike. With a Erriapus radius of 4 km, making it 1592.8× 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 1.73e+7 km (0.116 AU) from the Sun, Erriapus occupies a significant place in the Solar System's architecture. As a moon, Erriapus demonstrates the incredible diversity of natural satellites that orbit larger celestial bodies throughout our Solar System.

The Erriapus physical characteristics reveal a world of remarkable dimensions and properties. The Erriapus radius measures 4 km, making it 1592.8× smaller than Earth's size. The Erriapus mass of 6.80e+14 kg represents 8782352941.2× smaller than Earth's mass, giving this world substantial gravitational influence.

The Erriapus orbit reveals fascinating details about its journey around the Sun and its relationship to other Solar System objects. The Erriapus orbit has a semimajor axis of 1.73e+7 km (0.116 AU), placing it 8.6× smaller than Earth's distance from the Sun. The Erriapus orbit is moderately elliptical with an eccentricity of 0.474 (28.4× Earth's orbital eccentricity), creating noticeable seasonal variations in solar radiation. The Erriapus orbit takes 0.24 hours to complete (36223.8× smaller than Earth's orbital period), defining the length of its year. The orbital inclination of 34.6° indicates how much the Erriapus orbit is tilted relative to the Solar System's ecliptic plane. This high inclination suggests Erriapus may have experienced significant gravitational perturbations or formed in a different region of the Solar System.

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

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