Questions about the planet Venus?

Question

1)When was it discovered?

2)What are some Visitation by spacecraft from Earth?

3)Diameter, distance from sun, gravity?

4) What is its core composed of?

5)Outerlayers composed by?

6)Visited by what spacecrafts?

Thank You.

Answer 1

1)When was it discovered?

It's a bright planet, so it's been visible to the naked eye since the first men walked on the earth, and to the eyes of the animals we evolved from.  We've known about it for thousands of years.  However, Galileo was the first to observe that Venus has phases like the moon's in 1610.

2)What are some Visitation by spacecraft from Earth?

Venera 1 probe was the first probe sent to Venus (by the soviets).

Mariner 2 probe (the first probe sent successfully by the Americans).

Venera 3 was the first to land on the planet.

Venus Express probe was the most recent project launched, as far as I know

3)Diameter, distance from sun, gravity?

Diameter: 12106.32km (7522.51 miles).

Distance from sun: It has an average orbit of 108 million km (67 million miles) from the sun.

Gravity: At the surface, about 0.904g.

4) What is its core composed of?

Iron.

5)Outerlayers composed by?

Not sure, sorry.

6)Visited by what spacecrafts?

Didn't you already ask this?

Answer 2

Venus, the jewel of the sky, was once know by ancient astronomers as the morning star and evening star. Early astronomers once thought Venus to be two separate bodies. Venus, which is named after the Roman goddess of love and beauty, is veiled by thick swirling cloud cover.

Astronomers refer to Venus as Earth's sister planet. Both are similar in size, mass, density and volume. Both formed about the same time and condensed out of the same nebula. However, during the last few years scientists have found that the kinship ends here. Venus is very different from the Earth. It has no oceans and is surrounded by a heavy atmosphere composed mainly of carbon dioxide with virtually no water vapor. Its clouds are composed of sulfuric acid droplets. At the surface, the atmospheric pressure is 92 times that of the Earth's at sea-level.

Venus is scorched with a surface temperature of about 482° C (900° F). This high temperature is primarily due to a runaway greenhouse effect caused by the heavy atmosphere of carbon dioxide. Sunlight passes through the atmosphere to heat the surface of the planet. Heat is radiated out, but is trapped by the dense atmosphere and not allowed to escape into space. This makes Venus hotter than Mercury.

A Venusian day is 243 Earth days and is longer than its year of 225 days. Oddly, Venus rotates from east to west. To an observer on Venus, the Sun would rise in the west and set in the east.

Until just recently, Venus' dense cloud cover has prevented scientists from uncovering the geological nature of the surface. Developments in radar telescopes and radar imaging systems orbiting the planet have made it possible to see through the cloud deck to the surface below. Four of the most successful missions in revealing the Venusian surface are NASA's Pioneer Venus mission (1978), the Soviet Union's Venera 15 and 16 missions (1983-1984), and NASA's Magellan radar mapping mission (1990-1994). As these spacecraft began mapping the planet a new picture of Venus emerged.

Venus' surface is relatively young geologically speaking. It appears to have been completely resurfaced 300 to 500 million years ago. Scientists debate how and why this occurred. The Venusian topography consists of vast plains covered by lava flows and mountain or highland regions deformed by geological activity. Maxwell Montes in Ishtar Terra is the highest peak on Venus. The Aphrodite Terra highlands extend almost half way around the equator. Magellan images of highland regions above 2.5 kilometers (1.5 miles) are unusually bright, characteristic of moist soil. However, liquid water does not exist on the surface and cannot account for the bright highlands. One theory suggests that the bright material might be composed of metallic compounds. Studies have shown the material might be iron pyrite (also know as "fools gold"). It is unstable on the plains but would be stable in the highlands. The material could also be some type of exotic material which would give the same results but at lower concentrations.

Venus is scarred by numerous impact craters distrubuted randomly over its surface. Small craters less that 2 kilometers (1.2 miles) are almost non-existent due to the heavy Venusian atmosphere. The exception occurs when large meteorites shatter just before impact, creating crater clusters. Volcanoes and volcanic features are even more numerous. At least 85% of the Venusian surface is covered with volcanic rock. Hugh lava flows, extending for hundreds of kilometers, have flooded the lowlands creating vast plains. More than 100,000 small shield volcanoes dot the surface along with hundreds of large volcanos. Flows from volcanos have produced long sinuous channels extending for hundreds of kilometers, with one extending nearly 7,000 kilometers (4,300 miles).

Giant calderas more than 100 kilometers (62 miles) in diameter are found on Venus. Terrestrial calderas are usually only several kilometers in diameter. Several features unique to Venus include coronae and arachnoids. Coronae are large circular to oval features, encircled with cliffs and are hundreds of kilometers across. They are thought to be the surface expression of mantle upwelling. Archnoids are circular to elongated features similar to coronae. They may have been caused by molten rock seeping into surface fractures and producing systems of radiating dikes and fractures.

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 eccentricity 0.0068

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 albedo 0.65

Magnitude (Vo) -4.4

Mean surface temperature 482°C

Atmospheric pressure (bars) 92

Atmospheric composition

Carbon dioxide

Nitrogen

Trace amounts of: Sulfur dioxide, water vapor,

carbon monoxide, argon, helium, neon,

hydrogen chloride, and hydrogen fluoride.



96%

3+%

Answer 3

Lots of questions.

Here are the answers I believe.

http://en.wikipedia.org/wiki/Venus

Answer 4

http://en.wikipedia.org/wiki/Venus