Dysnomia

Dysnomia is a fascinating moon in our Solar System that has captured the attention of astronomers and space enthusiasts alike. With a Dysnomia radius of 350 km, making it 18.2× 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 37,273 km (0.000 AU) from the Sun, Dysnomia occupies a significant place in the Solar System's architecture. As a moon, Dysnomia demonstrates the incredible diversity of natural satellites that orbit larger celestial bodies throughout our Solar System.

The Dysnomia physical characteristics reveal a world of remarkable dimensions and properties. The Dysnomia radius measures 350 km, making it 18.2× smaller than Earth's size. The Dysnomia mass of 1.45e+20 kg represents 41186.2× smaller than Earth's mass, giving this world substantial gravitational influence.

The Dysnomia orbit reveals fascinating details about its journey around the Sun and its relationship to other Solar System objects. The Dysnomia orbit has a semimajor axis of 37,273 km (0.000 AU), placing it 4013.6× smaller than Earth's distance from the Sun. The Dysnomia orbit is nearly circular with an eccentricity of 0.006 (2.7× smaller than Earth's orbital eccentricity), resulting in relatively stable solar heating throughout its year. The Dysnomia orbit takes 0.00 hours to complete (1999249.3× smaller than Earth's orbital period), defining the length of its year. The orbital inclination of 45.49° indicates how much the Dysnomia orbit is tilted relative to the Solar System's ecliptic plane. This high inclination suggests Dysnomia may have experienced significant gravitational perturbations or formed in a different region of the Solar System.

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

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