Astrophysics (Index)About

Venus

(second inner-most planet in the solar system)

Venus is the second solar system planet from the Sun. Characteristics:

It has no moons. It is a rocky planet with an extremely dense atmosphere (92 atm) with more than 95% carbon dioxide, but has a minimal magnetic field. Its rotation is strikingly slow and retrograde, opposite of its orbit (and the orbit of all the solar system planets, and their rotation in general), which results in a shorter solar day (the time period required for the same spot on the surface to face the Sun again). Its surface temperature is 735 K, far hotter than any other solar system planet including Mercury, apparently the end effect of a runaway greenhouse effect, consistent with the striking amount of a greenhouse gas (carbon dioxide) in its atmosphere.

There is some thought that Venus formerly had liquid water on the surface, potentially for billions of years, presumably long enough for life to take hold and evolve, before the extreme greenhouse effect took hold. The current surface conditions of Venus make investigating this a challenge.


(planet,solar system)
Further reading:
http://en.wikipedia.org/wiki/Venus
RedshiftParsecs
/Distance
Lightyears
/Lookback Years
  
~00.3AU~0lynearestVenus
~01.3AU~0lyfurthestVenus

Referenced by pages:
apparent magnitude (m)
atmosphere
atmospheric tide
BepiColombo
carbonate-silicate cycle
carbon dioxide (CO2)
equilibrium temperature (Teq)
Galileo
greenhouse effect
habitable zone (HZ)
late heavy bombardment (LHB)
Magellan
magnetic field
magnitude
moon
obliquity
point source
Pioneer Venus Orbiter (PVO)
retrograde orbit
rocky planet
rotation period
supercritical fluid (SCF)
Shapiro delay
superrotating wind
tidal locking
Titius-Bode law
transit
transiting planet
twinkling

Index