The innermost planet of the solar system and second smallest after Pluto.
Mercury is surpassed in size (but not in mass) by both Ganymede
and Titan. In ancient Greece it had two names
– Apollo for its appearance as a morning star and Hermes as an evening
star – although Greek astronomers knew that a single body was involved.
Being named after the fleet-footed god Hermes, or its Roman equivalent Mercury,
is especially apt as the planet races around the Sun
at an average speed of 48 km/s, completing one circuit in 88 days.
| Photomosaic of Mercury by Mariner
Until the 1960s it was thought that Mercury's day (the time it takes to
spin on its axis) was the same length as its year (the time it takes to
complete one orbit) so that it always kept one face to the Sun. However,
Doppler radar measurements in 1965
showed that Mercury actually rotates three times in two of its years.
This fact and Mercury's highly elliptical orbit (see below) would lead to
strange effects for an astronaut on the surface. At some longitudes the
Sun would appear to rise briefly, set, and rise again before traveling westward
across the sky. At sunset, the Sun would set, rise again briefly, and then
set again. In other places, an observer could watch the Sun come to a standstill
and then move backward for a while, before continuing its original motion,
having done a complete loop. See Mercury, rotation.
Although Mercury's mean distance from the Sun is 57,910,000km (0.387 AU),
its orbit is very elongated. The range from
perihelion to aphelion
is 46 to 70 million km.
Mercury's perihelion precesses around
the Sun at a rate that 19th century astronomers couldn't properly explain.
The "advance" of the perihelion was 476 arc-seconds per century –
42.6" more than expected. This discrepancy remained a nagging problem for
many decades, and it was even suggested that the answer might lie in the
existence of an intra-Mercurian planet, sometimes called Vulcan.
In the end, the puzzle was solved in much more dramatic style, by applying
a new theory of gravity: Einstein's general theory
Despite being fairly close to us, Mercury is one of the least-studied planets
in the solar system. Until 2008, it had been visited by only one spacecraft,
Mariner 10, which flew by three times in 1974 and 1975, mapping 45% of the
surface. Mariner observed a world similar in general respects to the Moon:
heavily cratered but with regions of relatively smooth plains, some of which
may be the result of ancient volcanic activity, others due to the deposition
of ejecta from cratering impacts. Its most distinctive features is the Caloris
Basin, a colossal, multiringed basin about about 1,350km (840 miles)
in diameter, whose inner floor contains mostly smooth plains, known as Caloris
Planitia, but also many ridges and fractures, some of them radial and others
arranged in two or three concentric rings. Its name, meaning "basin of heat,"
stems from the fact that it lies near the subsolar point when Mercury is
at perihelion and thus can experience temperatures as high as 700K.
| Ridges and fractures on the floor
of Caloris Basin
There are also great escarpments, up
to 1,500km long and 3km high, some of which slice through the rings of craters
and other features in a way that shows they were formed by compression of
the crust when Mercury's interior cooled and shrank. Estimates suggest that
the planet's surface area decreased by about 0.1% and its radius by about
Radar images taken by astronomers at the Jet Propulsion Laboratory and the
California Institute of Technology in 1991 suggest that the polar regions
of Mercury may be covered with patches of water-ice. Although this seems
impossible due to the planet's sizzling heat, the polar regions receive
very little sunlight and may get as cold as -148°C.
Mercury is the second densest major body in the solar system, after the
Earth, pointing to a relatively enormous iron core
with a radius of 1,800 to 1,900km – proportionately much larger than
Earth's and making up most of the planet. Above this is a relatively thin
silicate mantle and crust, only 500 to 600km in total from top to bottom.
| Interiors of Earth and Mercury compared
Mercury has a weak magnetic field about 1% as strong as Earth's. Recent
research into irregularities in the rate of Mercury's spin suggest that
this magnetic field may be due to a molten outer core.
Mercury has an extremely thin atmosphere, about one trillionth the density
of Earth's, composed mainly of atoms of argon, neon, and helium that have
been blasted off the surface by the solar
Current and future probes
On August 3, 2004, NASA launched a spacecraft called MESSENGER
that will go into orbit Mercury in 2011. MESSENGER made its first flyby
of the planet on January 14, 2008, sending back images including the first
ones of the hemisphere of Mercury that Mariner 10 missed (see below for
images of Mercury acquired by MESSENGER during its first flyby). Europe
and Japan are also developing a robot mission to Mercury, called BepiColombo,
for launch early in the next decade.
|distance from Sun (mean)
||57.9 million km (35.9 million miles, 0.387 AU)
||4,879 km (3,032 miles), 0.382 × Earth
||negligible – traces of sodium, helium, hydrogen,
|max. temperature (day)
|min. temperature (night)
|surface gravity (Earth=1)
||4.3 km/s (15,480 km/h, 9,621 mph)
|number of moons
Images of Mercury returned by MESSENGER
|This image was taken today by NASA's MESSENGER
spacecraft at a distance of approximately 17,000 miles following the
spacecraft's closest approach to Mercury. It shows features as small
as 6 miles in size. Similar to previously mapped portions of Mercury,
this hemisphere appears heavily cratered. It also reveals some unique
and distinctive features. On the upper right is the giant Caloris
basin, including its western portions never before seen by spacecraft.
Formed by the impact of a large asteroid or comet, Caloris is one
of the largest, and perhaps one of the youngest basins in the solar
Credit: NASA/Johns Hopkins University Applied Physics Laboratory/Carnegie
Institution of Washington
|MESSENGER acquired this image on Jan.
14, 2008, as part of a mosaic that covers much of the sunlit portion
of a hemisphere not view by previous spacecraft. Images such as this
can be read in terms of a sequence of geological events and provide
insight into the relative timing of processes that have acted on Mercury's
surface in the past. The double-ringed crater at upper right of this
image appears to be filled with smooth plains material, perhaps volcanic
in nature. This crater was subsequently disrupted by the formation
of a prominent cliff, the surface expression of a major crustal fault
system that runs alongside part of its southern rim. This may have
led to the uplift seen across a portion of the crater's floor. A smaller
crater in the upper left of the image also has been cut by the cliff,
showing that the fault beneath the cliff was active after both of
these craters had formed. Credit: NASA/Johns Hopkins University APL/Carnegie
|This image obtained by MESSENGER reveals
a variety of intriguing surface features, including craters as small
as 300 yards across. The image also shows landscapes near Mercury's
equator on the side of the planet never before imaged by spacecraft.
These highly detailed close-ups enable planetary geologists to study
the processes that have shaped Mercury's surface over the past 4 billion
years. One of the highest and longest scarps cliffs yet seen on Mercury
curves from the top center down across the right side of this image.
Great forces in Mercury's crust have thrust the terrain occupying
the left two-thirds of the picture up and over the terrain to the
right. An impact crater has subsequently destroyed a small part of
the scarp near the top of the image. This image was taken from a distance
of 3,600 miles from surface and shows a region approximately 100 miles
across. Credit: NASA/Johns Hopkins APL/Carnegie Institution
scar found on Mercury's surface (Jan 31, 2008)
volcanic past revealed (Jan 30, 2008)
meteorite from Mercury unveiled (May 16, 2002)