Differences between Earth and Venus
Contents
Earth vs. Venus[edit]
Venus is often called Earth's "sister planet" due to their similar size, mass, density, and composition.[1][2][3] Both are terrestrial planets that formed around the same time, approximately 4.5 billion years ago.[1] However, despite these foundational similarities, the two worlds evolved into vastly different environments. Earth supports a wide diversity of life, while Venus has a hostile surface, making it the hottest planet in the solar system.[1][4][5]
Comparison Table[edit]
| Category | Earth | Venus |
|---|---|---|
| Diameter | 12,756 km (7,926 mi) | 12,104 km (7,521 mi) |
| Mass | 5.97 x 10²⁴ kg | 4.87 x 10²⁴ kg |
| [2]Orbital Period (Year) | 365.25 Earth days | 224.7 Earth days |
| [1]Rotational Period (Sidereal Day) | 23 hours, 56 minutes | 243 Earth days (retrograde) |
| [1]Average Surface Temperature | 15°C (59°F) | 464°C (867°F) |
| Atmospheric Composition | 78% Nitrogen, 21% Oxygen, 1% Other | 96.5% Carbon Dioxide, 3.5% Nitrogen |
| Surface Pressure | 1 bar | 92-93 bars |
| Magnetic Field | Substantial, internally generated | Very weak, induced by solar wind |
Atmosphere[edit]
The most significant difference between Earth and Venus is their atmospheres. Venus possesses a thick, dense atmosphere composed almost entirely of carbon dioxide, with clouds of sulfuric acid. This creates an extreme greenhouse effect, trapping heat and raising the planet's surface temperature to an average of 464°C (867°F). The atmospheric pressure at the surface of Venus is over 90 times that of Earth's, comparable to the pressure deep in Earth's oceans. In contrast, Earth's atmosphere is primarily nitrogen and oxygen, which provides a more moderate greenhouse effect, allowing for stable temperatures and liquid water.
Surface[5] and Geology[edit]
Due to its extreme surface conditions, Venus lacks liquid water. Its surface[1] is a dry, rocky landscape dominated by volcanic features. While both planets have varied terrains with mountains and plains, Venus does not show evidence of the plate tectonics that shape Earth's surface. Instead, volcanic activity appears to be the primary agent of geological change on Venus. The surface of Venus is also considered relatively young, having undergone a resurfacing event an estimated 300 to 600 million years ago.
Rotation and Orbit[edit]
Venus's rotation is unusual. It rotates on its axis very slowly, taking 243 Earth days to complete one rotation. This rotation[1] is also retrograde, meaning it spins in the opposite direction to its orbit around the Sun and in the opposite direction of most other planets. A Venusian day[1] is longer than its year of 225 Earth days. This slow rotation is a contributing factor to its lack of a significant, internally generated magnetic field like Earth's. Instead, Venus has a weak induced magnetic field created by the interaction of the solar wind with its ionosphere.
