Nitishsay features breaking science news about the latest discoveries in science, space, the environment, technology, and more -- from leading universities, scientific journals, and research organizations.

About Venus Planet | Solar System

Venus

Venus is the second planet from the Sun. It is named after the Roman goddess of love and beauty. 
As the second-brightest natural object in the night sky after the Moon, 
Venus can cast shadows and, rarely, is visible to the naked eye in broad daylight.
Venus
Venus 
In ancient times, Venus was often thought to be two different stars, the evening star and the morning star — that is, 
the ones that first appeared at sunset and sunrise. In Latin, they were respectively known as Vesper and Lucifer.
Venus is a terrestrial planet and is sometimes called Earth's "sister planet" because of their similar size, mass, proximity to the Sun, and bulk composition. 
It is radically different from Earth in other respects. It has the densest atmosphere of the four terrestrial planets, consisting of more than 96% carbon dioxide. 

Source: National Geographic



The atmospheric pressure at the planet's surface is 92 times that of Earth, or roughly the pressure found 900 m (3,000 ft) underwater on Earth.


Physical characteristics

Venus is one of the four terrestrial planets in the Solar System, meaning that it is a rocky body like Earth. 


Venus' southern hemisphere
Venus' southern hemisphere, as seen in the ultraviolet. (Image credit: ESA)

It is similar to Earth in size and mass, and is often described as Earth's "sister" or "twin".
The diameter of Venus is 12,103.6 km (7,520.8 mi)—only 638.4 km (396.7 mi) less than Earth's—and its mass is 81.5% of Earth's. 
Conditions on the Venusian surface differ radically from those on Earth because its dense atmosphere is 96.5% carbon dioxide, 
with most of the remaining 3.5% being nitrogen.
The surface of Venus is extremely dry. During its evolution, ultraviolet rays from the sun evaporated water quickly, keeping it in a prolonged molten state. 
There is no liquid water on its surface today because the scorching heat created by its ozone-filled atmosphere would cause any to boil away. 


Surface geology

Much of the Venusian surface appears to have been shaped by volcanic activity. Venus has several times as many volcanoes as Earth, 
and it has 167 large volcanoes that are over 100 km (62 mi) across.
Almost a thousand impact craters on Venus are evenly distributed across its surface. On other cratered bodies, such as Earth and the Moon, craters show a range of states of degradation. 
On the Moon, degradation is caused by subsequent impacts, whereas on Earth it is caused by wind and rain erosion. On Venus, about 85% of the craters are in pristine condition. 





Venus Statistics
Mass (kg)4.869e+24
Mass (Earth = 1).81476
Equatorial radius (km)6,051.8
Equatorial radius (Earth = 1).94886
Mean density (gm/cm^3)5.25
Mean distance from the Sun (km)108,200,000
Mean distance from the Sun (Earth = 1)0.7233
Rotational period (days)-243.0187
Orbital period (days)224.701
Mean orbital velocity (km/sec)35.02
Orbital eccentricity0.0068
Tilt of axis (degrees)177.36
Orbital inclination (degrees)3.394
Equatorial surface gravity (m/sec^2)8.87
Equatorial escape velocity (km/sec)10.36
Visual geometric albedo0.65
Magnitude (Vo)-4.4
Mean surface temperature482°C
Atmospheric pressure (bars)92
Atmospheric composition
Carbon dioxide
NitrogenTrace amounts of: Sulfur dioxide, water vapor,
carbon monoxide, argon, helium, neon,
hydrogen chloride, and hydrogen fluoride.

96%
3+% 

Post a comment

0 Comments