Venus
Although Venus has a very similar size and interior structure as Earth, its volcanic surface and extremely hot, dense atmosphere makes it one of the most inhospitable places in the Solar System.
Equatorial Diameter
12,104 km
Surface Temperature
462°C
Mass
4.867 × 10^24 kg
Surface Gravity
8.87 m/s²
Orbital Period
225 Earth Days
Rotation Period
243 Earth Days
Mean Dist. from Sun
108 million km
Atmosphere
96% Carbon Dioxide
Planetary Structure
Due to its similar size and density to Earth, Venus is thought to share a common internal structure consisting of a crust, mantle, and core. The crust is composed of solid silicate rock, mostly basalt. Below lies a solid silicate rock mantle. The core is believed to have a liquid outer layer of iron and nickel and a dense solid inner core of iron and nickel. A principal difference from Earth is the lack of plate tectonics, likely due to a dry surface and mantle. This prevents the planet from cooling efficiently and is a likely explanation for its lack of an internally generated magnetic field.
Scientific Discoveries
- Thick clouds of sulfuric acid and dust reflect most of the Sun's light, while carbon dioxide in the atmosphere traps the Sun's heat, causing a runaway greenhouse effect.
- A day on Venus (243 Earth days) is longer than its year (225 Earth days).
- It rotates backwards (retrograde rotation) compared to most other planets.
- The atmospheric pressure on the surface of Venus is 92 times greater than on Earth.
- Venus is one of the brightest objects in our night sky—second only to the Moon—and appears as either an evening or a morning star.
- Its clouds rain sulfuric acid, but this rain evaporates before it can reach the scorching hot surface.