Venus, the second planet from the Sun, is one of the most prominent and mysterious planets in the Solar System. Although it is similar in size and mass to Earth, Venus’s surface and climate are completely different, harsh, and unable to support life as we know it. From its extreme temperatures to its dense atmosphere, the planet presents major challenges for scientists and spacecraft. This article will analyze the surface structure and climate of Venus, exploring the factors that make this planet so special.

The Surface of Venus

The surface of Venus is mainly covered by vast plains, highlands, and a few extinct or active volcanoes. Unlike Earth, whose surface is broken up by oceans and continents, Venus has a uniform surface with alternating regions of different landforms. About 70% of Venus’s surface is covered by vast basalt plains, while the remainder is made up of plateaus and lowlands.

The High Grounds of Venus

Some regions on Venus feature remarkable elevations, called “tesserae.” These tesserae are often rugged in shape and are considered to be among the oldest features on the surface of Venus, possibly formed through complex tectonic processes. The largest highland region on Venus is Ishtar Terra, which is roughly the size of the continent of Australia, with several high mountains such as Maxwell Montes, the tallest mountain on Venus, which is about 11 km high.

Volcanic System

Venus is known for its large number of volcanoes, arguably more than any other planet in the Solar System. There are hundreds of thousands of volcanoes on Venus, ranging from large ones hundreds of kilometers in diameter to smaller ones just a few kilometers. Some notable volcanoes include Maat Mons, the tallest volcano on Venus, at about 8 kilometers high. Many scientists believe that the volcanoes on Venus are still active, based on signs of recent topographic changes and recent eruptions in the geologic past.

Lowlands and Plains

In addition to the highlands, Venus also has vast plains, often covered with basalt layers caused by volcanic activity. These plains contain many impact craters, but in much smaller numbers than those of planets like Mars or the Moon, suggesting that Venus’s surface is geologically “young”, with an estimated age of only 300 to 500 million years. The lack of craters also suggests that Venus may have undergone extensive resurfacing, possibly due to global volcanic activity.

Harsh Climate on Venus

The climate on Venus is one of the most extreme environments in the solar system. With a surface temperature higher than that of Mercury, the closest planet to the Sun, Venus has an average temperature of about 465°C, hot enough to melt lead. This temperature remains constant throughout the planet, day and night, at the equator and at the poles. This is due to a phenomenon called the “excessive greenhouse effect,” which traps heat from the Sun and prevents it from escaping.

Greenhouse Effect on Venus

Venus’s harsh climate is largely due to the greenhouse effect caused by its dense atmosphere, which is mostly composed of CO₂ (about 96.5%). This atmosphere is so thick that the pressure on the surface of Venus is 92 times that of Earth, equivalent to the pressure at a depth of 900 meters below sea level. When sunlight from the Sun hits the surface of Venus, this energy is absorbed and then emitted as infrared radiation. However, the thick layer of CO₂ prevents this infrared radiation from escaping into space, trapping the heat and causing an extremely powerful greenhouse effect.

As a result, the surface of Venus maintains a consistently high temperature, even when it receives no sunlight for long periods of time. The presence of large amounts of sulfur dioxide (SO₂) and other sulfur compounds in the atmosphere also contributes to the greenhouse effect, creating dense cloud layers that reflect sunlight.

Dense Cloud Layers

Not only is Venus’ atmosphere dense, it also contains dense clouds that cover the entire planet. These clouds are largely made up of sulfuric acid (H₂SO₄), which is extremely corrosive. Not only do the clouds on Venus enhance the greenhouse effect, they also reflect up to 75% of sunlight, making the planet the brightest when viewed from Earth.

The dense cloud layers on Venus move very quickly, reaching speeds of up to 360 km/h, many times faster than the planet rotates. This creates powerful jet streams and “super vortices” at the poles, where the jets of air move in the opposite direction of the planet’s rotation. The presence of sulfuric acid in the cloud layers also leads to acid rain on Venus, although the droplets usually evaporate before reaching the surface due to the high temperatures.

The Difference Between Day and Night on Venus

Although Venus has a very high and uniform surface temperature, the planet has a very unique day-night cycle. A day on Venus lasts 243 Earth days, which is longer than a Venusian year (about 225 Earth days). This means that Venus rotates on its axis very slowly, and if you were standing on the planet’s surface, you would see the Sun rise and set only twice in a Venusian year.

However, due to the strong greenhouse effect and dense atmosphere, the temperature on Venus does not change significantly between day and night. This is in stark contrast to other planets in the Solar System, where the temperature change between day and night is often very pronounced.

The Mysteries of Venus’s Climate

Despite extensive research into the climate of Venus, the planet still holds many unsolved mysteries. One of the big questions is what caused the extreme greenhouse effect on Venus. It is hypothesized that billions of years ago, Venus may have had Earth-like climatic conditions, with water oceans and a temperate climate. However, due to a major event or series of events, such as a sudden increase in volcanic activity or a change in its orbit, Venus experienced an extreme climate change, leading to an uncontrolled greenhouse effect and the complete evaporation of its water.

Another mystery is the presence of small amounts of oxygen (O₂) in Venus’ atmosphere. Although very small, the presence of O₂ could hint at complex chemical processes taking place on the planet, possibly involving reactions between sulfur compounds and sunlight.

Scientists have also detected the presence of phosphine (PH₃), a chemical compound that is often considered a sign of microbial life in anaerobic conditions. However, this is still controversial and more research is needed to determine the exact origin of phosphine on Venus.

The Future of Venus Research

Venus, with its harsh environment and unsolved mysteries, is becoming an important target for future space missions. These missions are aimed not only at exploring the planet’s surface and climate, but also at better understanding the formation and evolution of rocky planets in the Solar System.

One of the most recent missions is the Japanese Akatsuki mission, launched in 2010, which aims to study the atmosphere and weather phenomena on Venus. The mission has made interesting discoveries about the planet’s powerful anticyclones and jet streams. In addition, NASA and the ESA (European Space Agency) are also planning new missions to explore Venus in the next decade.

Surface and Climate of Venus

The surface and climate of Venus offer a challenging view of the planet. Although similar in size and mass to Earth, Venus is a completely different world, with extreme temperatures, a dense atmosphere, and unsolved mysteries. Studying Venus not only helps us better understand the planet, but also provides important information for understanding geological and climate processes that may occur on other planets, including Earth.

In the future, with the development of technology and new space missions, we may be able to solve the remaining mysteries of Venus. Do you think Venus may contain other surprises that we have not yet discovered? Let’s wait and see what new discoveries from this challenging planet!