2 Pallas

2 Pallas is a fascinating asteroid in our Solar System that has captured the attention of astronomers and space enthusiasts alike. With a 2 Pallas radius of 545 km, making it 11.7× 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 4.15e+8 km (2.772 AU) from the Sun, 2 Pallas occupies a significant place in the Solar System's architecture. As an asteroid, 2 Pallas represents the remnants of the early Solar System, providing valuable insights into the formation and evolution of our cosmic neighborhood.

The 2 Pallas physical characteristics reveal a world of remarkable dimensions and properties. The 2 Pallas radius measures 545 km, making it 11.7× smaller than Earth's size. The 2 Pallas mass of 2.11e+20 kg represents 28303.3× smaller than Earth's mass, giving this world substantial gravitational influence.

The 2 Pallas orbit reveals fascinating details about its journey around the Sun and its relationship to other Solar System objects. The 2 Pallas orbit has a semimajor axis of 4.15e+8 km (2.772 AU), placing it 2.8× Earth's distance from the Sun. At its closest approach (perihelion), 2 Pallas comes within 3.19e+8 km of the Sun, while at its farthest point (aphelion), it reaches 5.10e+8 km, creating a 46.0% variation in solar distance. The 2 Pallas orbit is moderately elliptical with an eccentricity of 0.231 (13.8× Earth's orbital eccentricity), creating noticeable seasonal variations in solar radiation. The 2 Pallas orbit takes 0.47 hours to complete (18718.6× smaller than Earth's orbital period), defining the length of its year. The orbital inclination of 0° indicates how much the 2 Pallas orbit is tilted relative to the Solar System's ecliptic plane. This low inclination means 2 Pallas follows a path very close to the plane where most planets orbit, suggesting a stable formation history.

The 2 Pallas rotation and axial orientation provide crucial insights into its daily and seasonal cycles, as well as its orbital dynamics. The 2 Pallas axial tilt of 0° determines the intensity and nature of seasonal variations. With minimal axial tilt, 2 Pallas experiences virtually no seasonal changes, maintaining relatively constant temperatures throughout its year. The orbital orientation parameters reveal additional details about 2 Pallas'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 2 Pallas temperature and atmospheric conditions are fundamental to understanding its habitability and environmental characteristics. The 2 Pallas average temperature of 0.0 K (-273.1 °C) (-459.7°F) provides the baseline for understanding its climate. These extremely cold temperatures make 2 Pallas 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), 2 Pallas presents a dramatically different thermal environment. Being farther from the Sun than Earth, 2 Pallas receives less solar radiation, resulting in cooler conditions. The elliptical orbit creates significant temperature variations throughout the year, with extreme seasonal changes.

The 2 Pallas escape velocity and shape characteristics reveal important details about its gravitational field and rotational dynamics. The 2 Pallas 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 2 Pallas to retain a substantial atmosphere. The 2 Pallas 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.