Tag Archives: Planet Venus

Venus and Earth: worlds apart

At first glance, Venus appears much like the Earth: their size and mass are fairly similar and so are their densities. Like Earth, Venus’ rocks are likely mostly basaltic, created during intense periods of volcanic activity when the planets formed around four and a half billion years ago. Both planets have an atmosphere, too.

But it turns out that any similarities end there. Close up, they are worlds of extremes.

Earth and Venus – worlds apart. Credits: Earth: NASA; Venus: Magellan Project/NASA/JPL

The Venus greenhouse
Under a thick, choking atmosphere of carbon dioxide and sulphuric dioxide clouds the surface pressure is 90 times greater than on Earth – that would be like walking underwater at a depth of 900 metres in Earth’s oceans! Then there’s the oven-hot 465 degrees Celsius surface temperature to contend with – the hottest planetary surface in the Solar System.

The dominant component of the Venus atmosphere, carbon dioxide, is a so-called greenhouse gas. Just like a greenhouse in which you might grow tomatoes, carbon dioxide is very good at trapping heat.

On Earth, the natural greenhouse effect is dominated by water vapour, a very efficient greenhouse gas, with contributions from carbon dioxide, methane and ozone. Without this naturally warming greenhouse effect we’d be shivering at -18 degrees Celsius!

An inhospitable surface lies beneath Venus’ thick cloud cover. Credits: ESA/C.Carreau.

On Venus, only ten percent of the incoming solar radiation reaches the surface; most of it is reflected back into space by the planet’s dense cloud cover, making Venus appear to shine brightly in the night sky.

Despite the small amount of solar radiation reaching the surface, it is trapped effectively by gases in the lower atmosphere, giving rise to the high temperatures. Scientists think that Venus was once more like the Earth, but at some point it started heating up uncontrollably.  Any water that may have once existed in oceans on the surface evaporated into the atmosphere causing further runaway heating. It’s like an Earth gone wrong with a runaway greenhouse effect that some planetary scientists say should be a warning as to what may become of our home planet if human activities – such as burning fossil fuels and destroying forests, which intensifies the natural greenhouse effect – continue.

A volcanic pressure cooker
Venus’ surface is a land of gently rolling uplands and volcanoes interspersed with low-lying plains and dotted with large impact craters. There are few small impact craters thanks to the planet’s thick atmosphere that burns up small meteoritic debris before it can strike the surface.  The oldest craters are in fact very young, no more than 500 million years old, suggesting that perhaps the planet undergoes regular global eruptions of lava that covers the entire surface.

On Earth, the steady eruption of volcanoes and shifting plates of crust that give rise to earthquakes mean that energy is released gradually over long periods of time. Venus, however, is like a volcanic pressure cooker with a tightly sealed lid that is only occasionally ruptured, but with catastrophic consequences.

Artist’s view of ESA’s Venus Express flying over atmospheric storms. Credits: ESA – AOES Medialab.

A backwards planet
Venus rotates backwards with respect to Earth, therefore the Sun appears to rise from the west. It also rotates very slowly – one Venus day takes 243 Earth days, which is longer than its 225 day year! However, since the planet rotates backwards, the time between a day measured from noon to noon becomes 117 days. Despite these long days, the winds on Venus are so fierce that they race around the planet in just four days.

ESA’s Venus Express, currently the only spacecraft in orbit around Earth’s mysterious sister planet, is providing spectacular detail of the complexities of the atmosphere, right down to the surface. Studying Venus is extremely important to learn how Earth and Venus, despite forming in the same neighbourhood and with similar planetary processes occurring on both worlds, grew up to be so different.

Venus and Earth: vital statistics

  Venus Earth
Mass 4.87x1024 kilograms  5.98 x1024 kilograms 
Equatorial radius  6052 kilometres 6378 kilometres
Density (mean) 5250 kilograms per cubic metre 5520 kilograms per cubic metre
Average distance form the Sun 108 million kilometres (0.7 Astronomical Units) 150 million kilometres (1 Astronomical Unit)
Rotation period 243 Earth days (retrograde) 23 hours 56 minutes
Year length (orbital period) 224.7 (Earth) days 365.2 days
Surface temperature (mean) 465 oC 15 oC
Atmospheric pressure on the surface 90 bars 1 bar (sea level)
Visual albedo (reflectivity)  0.76 0.37
Highest point on the surface Maxwell Montes (17 kilometres) Mount Everest (8.8 kilometres)
Major atmospheric components 96% carbon dioxide, 3% nitrogen 78% nitrogen, 21%oxygen, 1%argon
Surface materials Basaltic rock and altered materials Basaltic and granite rock and altered materials
Orbit inclination 3.4 o 0 o (per definition)
Obliquity of rotation axis 178 o 23.5 o
Surface gravity (at equator) 8.9 metres per square second 9.8 metres per square second

Venus exploration timeline

While ESA’s Venus Express is currently the only spacecraft in orbit around Venus, many spacecraft have returned data from the planet over the last half-century. As space- and ground-based telescopes prepare to watch Venus during the transit on 5-6 June, here's a look back at some of the highlights of Venus exploration:

1962 – Mariner 2 (US) – first successful flyby of Venus; confirmed high surface temperatures and pressures, a carbon dioxide rich atmosphere, continuous cloud cover, and the slow retrograde rotation of the planet.

1967 – Venera 4 (USSR) – first spacecraft to survive entry into another planet’s atmosphere. Returned atmospheric data, and deployed a parachute system to an altitude of 25km, becoming the first successful probe to perform in situ analysis of another planet’s environment.

Surface photo of Venus by Venera 13. Credits: NASA/NSSDC.

1967 – Mariner 5 (US)– successful flyby returning data on magnetic fields and plasmas, as well as UV emissions from the atmosphere.

1969 – Venera 5 and 6 (USSR) – atmospheric probes detected the presence of nitrogen and oxygen.

1970: Venera 7 (USSR) – first soft-landing on Venus and the first time data was returned from a manmade object after landing on another planet. It measured a surface temperature of 475°C and a surface pressure of 90 bar.

1972: Venera 8 (USSR) – landed on Venus and was the first to measure wind speeds as it descended through the atmosphere (from 100 metres/second above 48 kilometres to 1 metre/second below 10 kilometres).

1974: Mariner 10 (US) – Venus flyby en route to Mercury; tracked global atmospheric circulation with visible and ultraviolet imagery. It was the first spacecraft to have an imaging system.

1975: Venera 9 and 10 (USSR) – First spacecraft in orbit around Venus. They photographed the clouds and looked at the upper atmosphere, while the landers returned the first black and white panoramic images of the surface.

Venus by Magellan

Radar image of the surface of Venus by Magellan. Credits: Magellan Project/NASA/JPL

1978-1992: Pioneer Venus 1 and 2 – included a large entry probe and three smaller entry probes, providing vertical profiles of the atmosphere. Also the first orbiter to make radar mapping of the surface. Over a decade, it recorded a 90% decrease of sulphur dioxide, possibly indicating a large volcanic eruption just before the arrival.

1978 Venera 11 and 12 (USSR) – successful landing on the surface, and detection of lightning and thunder.

1982: Venera 13 and 14 (USSR) – the landers sent back the first colour pictures of the surface.

1983: Venera 15 and 16 (USSR) – the orbiters provided radar maps and atmospheric analyses.

1985: Vega 1 and 2 (USSR) – released landers and balloons at Venus en route to Halley's comet that recorded winds running at 240 kilometres/hour. Landers provided precise temperature profiles down to the surface and in situ measurements of cloud composition.

1990-94: Magellan (US) – mapped 98 per cent of the surface of Venus using synthetic aperture radar, at a resolution of 300 metres per pixel.

1990: Galileo (US) – flyby en route to Jupiter. First spacecraft observations of Venus' lower clouds and spectral imaging of the night side near infrared emissions.

1998, 1999: Cassini-Huygens (US, ESA) – flybys en route to Saturn.

Venus Express in orbit around Venus

ESA's Venus Express has been in orbit around Venus since 2006. Credits: ESA.

2006 – present: Venus Express (ESA)– the first European spacecraft to orbit Venus.

2006 and 2007: Messenger (US) – flybys en route to Mercury.

2010: Akatsuki (JAXA) – Japanese orbiter, failed orbit insertion but a second attempt will be made in 2015.

2015+: Bepi-Colombo (ESA) – with a scheduled launch in 2015, two flybys of Venus are planned en route to Mercury.

Note that the dates marked are those of operation at Venus, rather than launch dates.

ESA Euronews: Unveiling Venus

It can be called the morning or evening star, depending on where you are or what time it is, but it is anything but a star. In fact, it is one of our nearest planetary neighbours. Venus and Mars may be Earth's close cousins, but they are oh-so different. Only now are we starting to peer through Venus' clouds to reveal the burning planet's secrets.

Find out more about Venus and what we've learnt from Venus Express, and discover how ESA plans to observe the planet as it transits across the face of the Sun on 5-6 June.