Mercury (planet)
From Wikipedia, the free encyclopedia
Mercury in color, taken by MESSENGER
|
|||||||||||||
| Designations | |||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| Pronunciation |  i/ˈmɜrkjəri/ |
||||||||||||
| Adjectives | Mercurian,[1] Hermian[2] | ||||||||||||
| Orbital characteristics[5] | |||||||||||||
| Epoch J2000 | |||||||||||||
| Aphelion |
|
||||||||||||
| Perihelion |
|
||||||||||||
|
|||||||||||||
| Eccentricity | 0.205 630[3] | ||||||||||||
| 115.88 d[3] | |||||||||||||
|
Average orbital speed
|
47.362 km/s[3] | ||||||||||||
| 174.796° | |||||||||||||
| Inclination |
|
||||||||||||
| 48.331° | |||||||||||||
| 29.124° | |||||||||||||
| Satellites | None | ||||||||||||
| Physical characteristics | |||||||||||||
|
Mean radius
|
|||||||||||||
| Flattening | 0[7] | ||||||||||||
|
|||||||||||||
| Volume |
|
||||||||||||
| Mass |
|
||||||||||||
|
Mean density
|
5.427 g/cm3[6] | ||||||||||||
| 0.346±0.014 | |||||||||||||
| 4.25 km/s[6] | |||||||||||||
|
Sidereal rotation period
|
|
||||||||||||
|
Equatorial rotation velocity
|
10.892 km/h (3.026 m/s) | ||||||||||||
| 2.11′ ± 0.1′[8] | |||||||||||||
|
North pole right ascension
|
|
||||||||||||
|
North pole declination
|
61.45°[3] | ||||||||||||
| Albedo | |||||||||||||
|
|||||||||||||
| −2.6[10] to 5.7[3][11] | |||||||||||||
| 4.5–13″[3] | |||||||||||||
| Atmosphere[3] | |||||||||||||
|
Surface pressure
|
trace | ||||||||||||
| Composition | |||||||||||||
Because it has almost no atmosphere to retain heat, Mercury's surface experiences the greatest temperature variation of all the planets, ranging from 100 K (−173 °C; −280 °F) at night to 700 K (427 °C; 800 °F) during the day at some equatorial regions. The poles are constantly below 180 K (−93 °C; −136 °F). Mercury's axis has the smallest tilt of any of the Solar System's planets (about 1⁄30 of a degree), but it has the largest orbital eccentricity.[a] As such it does not experience seasons in the same way as most other planets such as Earth. At aphelion, Mercury is about 1.5 times as far from the Sun as it is at perihelion. Mercury's surface is heavily cratered and similar in appearance to the Moon, indicating that it has been geologically inactive for billions of years.
Mercury is gravitationally locked and rotates in a way that is unique in the Solar System. As seen relative to the fixed stars, it rotates exactly three times for every two revolutions[b] it makes around its orbit.[13] As seen from the Sun, in a frame of reference that rotates with the orbital motion, it appears to rotate only once every two Mercurian years. An observer on Mercury would therefore see only one day every two years.
Because Mercury moves in an orbit around the Sun which lies within Earth's orbit (as does Venus), it can appear in Earth's sky in the morning or the evening, but not in the middle of the night. Also, like Venus and the Moon, it displays a complete range of phases as it moves around its orbit relative to Earth. Although Mercury can appear as a very bright object when viewed from Earth, its proximity to the Sun makes it more difficult to see than Venus. Two spacecraft have visited Mercury: Mariner 10 flew by in the 1970s and MESSENGER, launched in 2004, remains in orbit.
Internal structure
1. Crust: 100–300 km thick
2. Mantle: 600 km thick
3. Core: 1,800 km radius
Mercury is one of four terrestrial planets in the Solar System, and is a rocky body like Earth. It is the smallest planet in the Solar System, with an equatorial radius of 2,439.7 km.[3] Mercury is also smaller—albeit more massive—than the largest natural satellites in the Solar System, Ganymede and Titan. Mercury consists of approximately 70% metallic and 30% silicate material.[14] Mercury's density is the second highest in the Solar System at 5.427 g/cm3, only slightly less than Earth's density of 5.515 g/cm3.[3] If the effect of gravitational compression were to be factored out, the materials of which Mercury is made would be denser, with an uncompressed density of 5.3 g/cm3 versus Earth's 4.4 g/cm3.[15]
Mercury's density can be used to infer details of its inner structure. Although Earth's high density results appreciably from gravitational compression, particularly at the core, Mercury is much smaller and its inner regions are not as compressed. Therefore, for it to have such a high density, its core must be large and rich in iron.[16]
Geologists estimate that Mercury's core occupies about 42% of its volume; for Earth this proportion is 17%. Research published in 2007 suggests that Mercury has a molten core.[17][18] Surrounding the core is a 500–700 km mantle consisting of silicates.[19][20] Based on data from the Mariner 10 mission and Earth-based observation, Mercury's crust is believed to be 100–300 km thick.[21] One distinctive feature of Mercury's surface is the presence of numerous narrow ridges, extending up to several hundred kilometers in length. It is believed that these were formed as Mercury's core and mantle cooled and contracted at a time when the crust had already solidified.[22]
Mercury's core has a higher iron content than that of any other major planet in the Solar System, and several theories have been proposed to explain this. The most widely accepted theory is that Mercury originally had a metal-silicate ratio similar to common chondrite meteorites, thought to be typical of the Solar System's rocky matter, and a mass approximately 2.25 times its current mass.[23] Early in the Solar System's history, Mercury may have been struck by a planetesimal of approximately 1/6 that mass and several thousand kilometers across.[23] The impact would have stripped away much of the original crust and mantle, leaving the core behind as a relatively major component.[23] A similar process, known as the giant impact hypothesis, has been proposed to explain the formation of the Moon.[23]
Alternatively, Mercury may have formed from the solar nebula before the Sun's energy output had stabilized. It would initially have had twice its present mass, but as the protosun contracted, temperatures near Mercury could have been between 2,500 and 3,500 K and possibly even as high as 10,000 K.[24] Much of Mercury's surface rock could have been vaporized at such temperatures, forming an atmosphere of "rock vapor" that could have been carried away by the solar wind.[24]
A third hypothesis proposes that the solar nebula caused drag on the particles from which Mercury was accreting, which meant that lighter particles were lost from the accreting material and not gathered by Mercury.[25] Each hypothesis predicts a different surface composition, and two space missions, MESSENGER and BepiColombo, both will make observations to test them.[26][27] MESSENGER has found higher-than-expected potassium and sulfur levels on the surface, suggesting that the giant impact hypothesis and vaporization of the crust and mantle did not occur because potassium and sulfur would have been driven off by the extreme heat of these events. The findings would seem to favor the third hypothesis; however, further analysis of the data is needed.[28]
Surface geology
Mercury's surface is very similar in appearance to that of the Moon, showing extensive mare-like plains and heavy cratering, indicating that it has been geologically inactive for billions of years. Because our knowledge of Mercury's geology has been based only on the 1975 Mariner flyby and terrestrial observations, it is the least understood of the terrestrial planets.[18] As data from the recent MESSENGER flyby is processed, this knowledge will increase. For example, an unusual crater with radiating troughs has been discovered that scientists called "the spider".[29] It later received the name Apollodorus.[30]
Albedo features are areas of markedly different reflectivity, as seen by telescopic observation. Mercury possesses dorsa (also called "wrinkle-ridges"), Moon-like highlands, montes (mountains), planitiae (plains), rupes (escarpments), and valles (valleys).[31][32]
Names for features on Mercury come from a variety of sources. Names coming from people are limited to the deceased. Craters are named for artists, musicians, painters, and authors who have made outstanding or fundamental contributions to their field. Ridges, or dorsa, are named for scientists who have contributed to the study of Mercury. Depressions or fossae are named for works of architecture. Montes are named for the word "hot" in a variety of languages. Plains or planitiae are named for Mercury in various languages. Escarpments or rupēs are named for ships of scientific expeditions. Valleys or valles are named for radio telescope facilities.[33]
Mercury was heavily bombarded by comets and asteroids during and shortly following its formation 4.6 billion years ago, as well as during a possibly separate subsequent episode called the late heavy bombardment that came to an end 3.8 billion years ago.[34] During this period of intense crater formation, the planet received impacts over its entire surface,[32] facilitated by the lack of any atmosphere to slow impactors down.[35] During this time the planet was volcanically active; basins such as the Caloris Basin were filled by magma, producing smooth plains similar to the maria found on the Moon.[36][37]
Data from the October 2008 flyby of MESSENGER gave researchers a greater appreciation for the jumbled nature of Mercury's surface. Mercury's surface is more heterogeneous than either Mars's or the Moon's, both of which contain significant stretches of similar geology, such as maria and plateaus.[38]
Impact basins and craters
The so-called "Weird Terrain" was formed at the point antipodal to the Caloris Basin impact
Craters on Mercury range in diameter from small bowl-shaped cavities to multi-ringed impact basins hundreds of kilometers across. They appear in all states of degradation, from relatively fresh rayed craters to highly degraded crater remnants. Mercurian craters differ subtly from lunar craters in that the area blanketed by their ejecta is much smaller, a consequence of Mercury's stronger surface gravity.[39] According to IAU rules, each new crater must be named after an artist that was famous for more than fifty years, and dead for more than three years, before the date the crater is named.[40]
The largest known crater is Caloris Basin, with a diameter of 1,550 km.[41] The impact that created the Caloris Basin was so powerful that it caused lava eruptions and left a concentric ring over 2 km tall surrounding the impact crater. At the antipode of the Caloris Basin is a large region of unusual, hilly terrain known as the "Weird Terrain". One hypothesis for its origin is that shock waves generated during the Caloris impact traveled around the planet, converging at the basin's antipode (180 degrees away). The resulting high stresses fractured the surface.[42] Alternatively, it has been suggested that this terrain formed as a result of the convergence of ejecta at this basin's antipode.[43]
Overall, about 15 impact basins have been identified on the imaged part of Mercury. A notable basin is the 400 km wide, multi-ring Tolstoj Basin that has an ejecta blanket extending up to 500 km from its rim and a floor that has been filled by smooth plains materials. Beethoven Basin has a similar-sized ejecta blanket and a 625 km diameter rim.[39] Like the Moon, the surface of Mercury has likely incurred the effects of space weathering processes, including Solar wind and micrometeorite impacts.[44]
Plains
There are two geologically distinct plains regions on Mercury.[39][45] Gently rolling, hilly plains in the regions between craters are Mercury's oldest visible surfaces,[39] predating the heavily cratered terrain. These inter-crater plains appear to have obliterated many earlier craters, and show a general paucity of smaller craters below about 30 km in diameter.[45] It is not clear whether they are of volcanic or impact origin.[45] The inter-crater plains are distributed roughly uniformly over the entire surface of the planet.[citation needed]
Smooth plains are widespread flat areas that fill depressions of various sizes and bear a strong resemblance to the lunar maria. Notably, they fill a wide ring surrounding the Caloris Basin. Unlike lunar maria, the smooth plains of Mercury have the same albedo as the older inter-crater plains. Despite a lack of unequivocally volcanic characteristics, the localisation and rounded, lobate shape of these plains strongly support volcanic origins.[39] All the Mercurian smooth plains formed significantly later than the Caloris basin, as evidenced by appreciably smaller crater densities than on the Caloris ejecta blanket.[39] The floor of the Caloris Basin is filled by a geologically distinct flat plain, broken up by ridges and fractures in a roughly polygonal pattern. It is not clear whether they are volcanic lavas induced by the impact, or a large sheet of impact melt.[39]
One unusual feature of the planet's surface is the numerous compression folds, or rupes, that crisscross the plains. As the planet's interior cooled, it may have contracted and its surface began to deform, creating these features. The folds can be seen on top of other features, such as craters and smoother plains, indicating that the folds are more recent.[46] Mercury's surface is flexed by significant tidal bulges raised by the Sun—the Sun's tides on Mercury are about 17 times stronger than the Moon's on Earth.[47]
Surface conditions and "atmosphere" (exosphere)
The surface temperature of Mercury ranges from 100 K to 700 K[49] at the most extreme places: 0°N, 0°W, or 180°W. It never rises above 180 K at the poles,[12] due to the absence of an atmosphere and a steep temperature gradient between the equator and the poles. The subsolar point reaches about 700 K during perihelion (0°W or 180°W), but only 550 K at aphelion (90° or 270°W).[50] On the dark side of the planet, temperatures average 110 K.[12][51] The intensity of sunlight on Mercury's surface ranges between 4.59 and 10.61 times the solar constant (1,370 W·m−2).[52]
Although the daylight temperature at the surface of Mercury is generally extremely high, observations strongly suggest that ice (frozen water) exists on Mercury. The floors of deep craters at the poles are never exposed to direct sunlight, and temperatures there remain below 102 K; far lower than the global average.[53] Water ice strongly reflects radar, and observations by the 70 m Goldstone telescope and the VLA in the early 1990s revealed that there are patches of very high radar reflection near the poles.[54] Although ice was not the only possible cause of these reflective regions, astronomers believed it was the most likely.[55]
The icy regions are believed to contain about 1014–1015 kg of ice,[56] and may be covered by a layer of regolith that inhibits sublimation.[57] By comparison, the Antarctic ice sheet on Earth has a mass of about 4×1018 kg, and Mars's south polar cap contains about 1016 kg of water.[56] The origin of the ice on Mercury is not yet known, but the two most likely sources are from outgassing of water from the planet's interior or deposition by impacts of comets.[56]
Mercury is too small and hot for its gravity to retain any significant atmosphere over long periods of time; it does have a "tenuous surface-bounded exosphere"[58] containing hydrogen, helium, oxygen, sodium, calcium, potassium and others. This exosphere is not stable—atoms are continuously lost and replenished from a variety of sources. Hydrogen and helium atoms probably come from the solar wind, diffusing into Mercury's magnetosphere before later escaping back into space. Radioactive decay of elements within Mercury's crust is another source of helium, as well as sodium and potassium. MESSENGER found high proportions of calcium, helium, hydroxide, magnesium, oxygen, potassium, silicon and sodium. Water vapor is present, released by a combination of processes such as: comets striking its surface, sputtering creating water out of hydrogen from the solar wind and oxygen from rock, and sublimation from reservoirs of water ice in the permanently shadowed polar craters. The detection of high amounts of water-related ions like O+, OH−, and H2O+ was a surprise.[59][60] Because of the quantities of these ions that were detected in Mercury's space environment, scientists surmise that these molecules were blasted from the surface or exosphere by the solar wind.[61][62]
Sodium, potassium and calcium were discovered in the atmosphere during the 1980–1990s, and are believed to result primarily from the vaporization of surface rock struck by micrometeorite impacts.[63] In 2008 magnesium was discovered by MESSENGER probe.[64] Studies indicate that, at times, sodium emissions are localized at points that correspond to the planet's magnetic poles. This would indicate an interaction between the magnetosphere and the planet's surface.[65]
On November 29, 2012, NASA confirmed that images from MESSENGER had detected that craters at the north pole contained water ice. Sean C. Solomon was quoted in the New York Times as estimating the volume of the ice as large enough to "encase Washington, D.C., in a frozen block two and a half miles deep".[48][c]
Magnetic field and magnetosphere
Despite its small size and slow 59-day-long rotation, Mercury has a significant, and apparently global, magnetic field. According to measurements taken by Mariner 10, it is about 1.1% as strong as Earth's. The magnetic field strength at the Mercurian equator is about 300 nT.[66][67] Like that of Earth, Mercury's magnetic field is dipolar.[65] Unlike Earth, Mercury's poles are nearly aligned with the planet's spin axis.[68] Measurements from both the Mariner 10 and MESSENGER space probes have indicated that the strength and shape of the magnetic field are stable.[68]
It is likely that this magnetic field is generated by way of a dynamo effect, in a manner similar to the magnetic field of Earth.[69][70] This dynamo effect would result from the circulation of the planet's iron-rich liquid core. Particularly strong tidal effects caused by the planet's high orbital eccentricity would serve to keep the core in the liquid state necessary for this dynamo effect.[71]
Mercury's magnetic field is strong enough to deflect the solar wind around the planet, creating a magnetosphere. The planet's magnetosphere, though small enough to fit within Earth,[65] is strong enough to trap solar wind plasma. This contributes to the space weathering of the planet's surface.[68] Observations taken by the Mariner 10 spacecraft detected this low energy plasma in the magnetosphere of the planet's nightside. Bursts of energetic particles were detected in the planet's magnetotail, which indicates a dynamic quality to the planet's magnetosphere.[65]
During its second flyby of the planet on October 6, 2008, MESSENGER discovered that Mercury's magnetic field can be extremely "leaky". The spacecraft encountered magnetic "tornadoes" – twisted bundles of magnetic fields connecting the planetary magnetic field to interplanetary space – that were up to 800 km wide or a third of the radius of the planet. These "tornadoes" form when magnetic fields carried by the solar wind connect to Mercury's magnetic field. As the solar wind blows past Mercury's field, these joined magnetic fields are carried with it and twist up into vortex-like structures. These twisted magnetic flux tubes, technically known as flux transfer events, form open windows in the planet's magnetic shield through which the solar wind may enter and directly impact Mercury's surface.[72]
The process of linking interplanetary and planetary magnetic fields, called magnetic reconnection, is common throughout the cosmos. It occurs in Earth's magnetic field, where it generates magnetic tornadoes as well. The MESSENGER observations show the reconnection rate is ten times higher at Mercury. Mercury's proximity to the Sun only accounts for about a third of the reconnection rate observed by MESSENGER.[72]
Orbit, rotation, and longitude
Orbit of Mercury (yellow). Dates refer to 2006.
Animation of Mercury's and Earth's revolution around the Sun
Mercury has the most eccentric orbit of all the planets; its eccentricity is 0.21 with its distance from the Sun ranging from 46,000,000 to 70,000,000 km (29,000,000 to 43,000,000 mi). It takes 87.969 earth days to complete an orbit. The diagram on the right illustrates the effects of the eccentricity, showing Mercury's orbit overlaid with a circular orbit having the same semi-major axis. The higher velocity of the planet when it is near perihelion is clear from the greater distance it covers in each 5-day interval. In the diagram the varying distance of Mercury to the Sun is represented by the size of the planet, which is inversely proportional to Mercury's distance from the Sun. This varying distance to the Sun, combined with a 3:2 spin–orbit resonance of the planet's rotation around its axis, result in complex variations of the surface temperature.[14] This resonance makes a single day on Mercury last exactly two Mercury years, or about 176 Earth days.[73]
Mercury's orbit is inclined by 7 degrees to the plane of Earth's orbit (the ecliptic), as shown in the diagram on the right. As a result, transits of Mercury across the face of the Sun can only occur when the planet is crossing the plane of the ecliptic at the time it lies between Earth and the Sun. This occurs about every seven years on average.[74]
Mercury's axial tilt is almost zero,[75] with the best measured value as low as 0.027 degrees.[8] This is significantly smaller than that of Jupiter, which has the second smallest axial tilt of all planets at 3.1 degrees. This means that to an observer at Mercury's poles, the center of the Sun never rises more than 2.1 arcminutes above the horizon.[8]
At certain points on Mercury's surface, an observer would be able to see the Sun rise about halfway, then reverse and set before rising again, all within the same Mercurian day. This is because approximately four Earth days before perihelion, Mercury's angular orbital velocity equals its angular rotational velocity so that the Sun's apparent motion ceases; closer to perihelion, Mercury's angular orbital velocity then exceeds the angular rotational velocity. Thus, to a hypothetical observer on Mercury, the Sun appears to move in a retrograde direction. Four Earth days after perihelion, the Sun's normal apparent motion resumes.[14]
For the same reason, there are two points on Mercury's equator, 180 degrees apart in longitude, at either of which, around perihelion in alternate Mercurian years (once a Mercurian day), the Sun passes overhead, then reverses its apparent motion and passes overhead again, then reverses a second time and passes overhead a third time, taking a total of about 16 Earth-days for this entire process. In the other alternate Mercurian years, the same thing happens at the other of these two points. The amplitude of the retrograde motion is small, so the overall effect is that, for two or three weeks, the Sun is almost stationary overhead, and is at its most brilliant because Mercury is at perihelion, its closest to the Sun. This prolonged exposure to the Sun at its brightest makes these two points the hottest places on Mercury. Conversely, there are two other points on the equator, 90 degrees of longitude apart from the first ones, where the Sun passes overhead only when the planet is at aphelion in alternate years, when the apparent motion of the Sun in the Mercurian sky is relatively rapid. These points, which are the ones on the equator where the apparent retrograde motion of the Sun happens when it is crossing the horizon as described in the preceding paragraph, receive much less solar heat than the first ones described above.
Mercury attains inferior conjunction (nearest approach to Earth) every 116 Earth days on average,[3] but this interval can range from 105 days to 129 days due to the planet's eccentric orbit. Mercury can come as near as 82.2 Gm to Earth, and that is slowly declining: The next approach to within 82.1 Gm is in 2679, and to within 82 Gm in 4487, but it will not be closer to Earth than 80 Gm until AD 28,622.[76] Its period of retrograde motion as seen from Earth can vary from 8 to 15 days on either side of inferior conjunction. This large range arises from the planet's high orbital eccentricity.[14]
Longitude convention
The longitude convention for Mercury puts the zero of longitude at one of the two hottest points on the surface, as described above. However, when this area was first visited, by Mariner 10, this zero meridian was in darkness, so it was impossible to select a feature on the surface to define the exact position of the meridian. Therefore, a small crater further west was chosen, called Hun Kal, which provides the exact reference point for measuring longitude. The center of Hun Kal defines the 20° West meridian. A 1970 International Astronomical Union resolution suggests that longitudes be measured positively in the westerly direction on Mercury.[77] The two hottest places on the equator are therefore at longitudes 0°W and 180°W, and the coolest points on the equator are at longitudes 90°W and 270°W. However the MESSENGER project uses an east-positive convention.[78]Spin–orbit resonance
For many years it was thought that Mercury was synchronously tidally locked with the Sun, rotating once for each orbit and always keeping the same face directed towards the Sun, in the same way that the same side of the Moon always faces Earth. Radar observations in 1965 proved that the planet has a 3:2 spin–orbit resonance, rotating three times for every two revolutions around the Sun; the eccentricity of Mercury's orbit makes this resonance stable—at perihelion, when the solar tide is strongest, the Sun is nearly still in Mercury's sky.[79]
The original reason astronomers thought it was synchronously locked was that, whenever Mercury was best placed for observation, it was always nearly at the same point in its 3:2 resonance, hence showing the same face. This is because, coincidentally, Mercury's rotation period is almost exactly half of its synodic period with respect to Earth. Due to Mercury's 3:2 spin–orbit resonance, a solar day (the length between two meridian transits of the Sun) lasts about 176 Earth days.[14] A sidereal day (the period of rotation) lasts about 58.7 Earth days.[14]
Simulations indicate that the orbital eccentricity of Mercury varies chaotically from nearly zero (circular) to more than 0.45 over millions of years due to perturbations from the other planets.[14][80] This is thought to explain Mercury's 3:2 spin–orbit resonance (rather than the more usual 1:1), because this state is more likely to arise during a period of high eccentricity.[81] Numerical simulations show that a future secular orbital resonant perihelion interaction with Jupiter may cause the eccentricity of Mercury's orbit to increase to the point where there is a 1% chance that the planet may collide with Venus within the next five billion years.[82][83]
Advance of perihelion
In 1859, the French mathematician and astronomer Urbain Le Verrier reported that the slow precession of Mercury's orbit around the Sun could not be completely explained by Newtonian mechanics and perturbations by the known planets. He suggested, among possible explanations, that another planet (or perhaps instead a series of smaller 'corpuscules') might exist in an orbit even closer to the Sun than that of Mercury, to account for this perturbation.[84] (Other explanations considered included a slight oblateness of the Sun.) The success of the search for Neptune based on its perturbations of the orbit of Uranus led astronomers to place faith in this possible explanation, and the hypothetical planet was named Vulcan, but no such planet was ever found.[85]The perihelion precession of Mercury is 5600 arcseconds (1.5556°) per century relative to Earth, or 574.10±0.65 arcseconds per century[86] relative to the inertial ICFR. Newtonian mechanics, taking into account all the effects from the other planets, predicts a precession of 5557 arcseconds (1.5436°) per century.[86] In the early 20th century, Albert Einstein's General Theory of Relativity provided the explanation for the observed precession. The effect is very small: the Mercurian relativistic perihelion advance excess is just 42.98 arcseconds per century; therefore, it requires a little over twelve million orbits for a full excess turn. Similar, but much smaller, effects operate for other planets: 8.62 arcseconds per century for Venus, 3.84 for Earth, 1.35 for Mars, and 10.05 for 1566 Icarus.[87][88]
Observation
Mercury's apparent magnitude varies between −2.6[10] (brighter than the brightest star Sirius) and about +5.7 (approximating the theoretical limit of naked-eye visibility). The extremes occur when Mercury is close to the Sun in the sky.[10][11] Observation of Mercury is complicated by its proximity to the Sun, as it is lost in the Sun's glare for much of the time. Mercury can be observed for only a brief period during either morning or evening twilight.[89]
Mercury can, like several other planets and the brightest stars, be seen during a total solar eclipse.[90]
Like the Moon and Venus, Mercury exhibits phases as seen from Earth. It is "new" at inferior conjunction and "full" at superior conjunction. The planet is rendered invisible from Earth on both of these occasions because of its being obscured by the Sun's disk.[89]
Mercury is technically brightest as seen from Earth when it is at a full phase. Although the planet is farthest away from Earth when it is full the greater illuminated area that is visible and the opposition brightness surge more than compensates for the distance.[10] The opposite is true for Venus, which appears brightest when it is a crescent, because it is much closer to Earth than when gibbous.[10][91]
Nonetheless, the brightest (full phase) appearance of Mercury is an essentially impossible time for practical observation, because of the extreme proximity of the Sun. Mercury is best observed at the first and last quarter, although they are phases of lesser brightness. The first and last quarter phases occur at greatest elongation east and west, respectively. At both of these times Mercury's separation from the Sun ranges anywhere from 17.9° at perihelion to 27.8° at aphelion.[92][93] At greatest elongation west, Mercury rises at its earliest before the Sun, and at greatest elongation east, it sets at its latest after the Sun.[94]
At tropical and subtropical latitudes, Mercury is more easily seen than at higher latitudes. In low latitudes and at the right times of year, the ecliptic intersects the horizon at a very steep angle. When Mercury is vertically above the Sun in the sky and is at maximum elongation from the Sun (28 degrees), and when the Sun is 18 degrees below the horizon, so the sky is just completely dark,[d] Mercury is 10 degrees above the horizon. This is the greatest angle of elevation at which Mercury can be seen in a completely dark sky.
At temperate latitudes, Mercury is more often easily visible from Earth's Southern Hemisphere than from its Northern Hemisphere. This is because Mercury's maximum possible elongations west of the Sun always occur when it is early autumn in the Southern Hemisphere, whereas its maximum possible eastern elongations happen during late winter in the Southern Hemisphere.[94] In both of these cases, the angle Mercury strikes with the ecliptic is maximized, allowing it to rise several hours before the Sun in the former instance and not set until several hours after sundown in the latter in countries located at southern temperate zone latitudes, such as Argentina and South Africa.[94] By contrast, at the major population centers of the northern temperate latitudes, Mercury is never above the horizon of a more-or-less fully dark night sky.[citation needed]
Another possibility is looking up the planet during daylight with a nice blue sky and when close to greatest elongation or when gibbous (but not too gibbous as it is too close to the Sun !) the planet can be found easily even with a telescope as small as 8cm aperture. But one has to know the exact coordinates and avoid pointing the telescope to the Sun. But modern pushto / goto telescopes can make this easy. This bypasses the limitation of twilight observing when the ecliptic has a small angle with the horizon (e.g. in autumn evenings).
Ground-based telescope observations of Mercury reveal only an illuminated partial disk with limited detail. The first of two spacecraft to visit the planet was Mariner 10, which mapped about 45% of its surface from 1974 to 1975. The second is the MESSENGER spacecraft, which after three Mercury flybys between 2008 and 2009, attained orbit around Mercury on March 17, 2011,[95] to study and map the rest of the planet.[96]
The Hubble Space Telescope cannot observe Mercury at all, due to safety procedures that prevent its pointing too close to the Sun.[97]
Naked-eye viewing
Mercury is seen most easily when it is close to its greatest elongation, which means that its angular separation from the Sun is greatest. Mercury can be near greatest western elongation, which means it is west of the Sun in the sky, so it is visible soon before sunrise, or greatest eastern elongation, which means it is visible soon after sunset. However, the exact dates of the greatest elongations are not the best ones on which to try to see Mercury. The phase of the planet greatly affects its apparent brightness. At greatest elongation, it is approximately at half phase. It is brighter when it is gibbous, which means that the best times to see Mercury are a few days before greatest eastern elongation, in the evening, or a few days after greatest western elongation, in the morning. The apparent inclination of the ecliptic to the horizon is also important. When the inclination is large, as occurs near the spring equinox in the evening, and near the autumnal equinox in the morning (this is true for observers in both hemispheres), Mercury is higher in the sky when the Sun is just below the horizon, which makes it easier to see than at other times. The inclination of the ecliptic is also greater for observers at low latitudes than high ones. It is helpful if Mercury is close to aphelion at the time of observation, because this makes it further from the Sun than at other times. However, it also makes the planet less brightly illuminated, so the visibility advantage is not great. At present, Mercury is fairly close to aphelion when viewed at greatest western elongation at the March equinox, or at greatest eastern elongation at the September equinox. (Over long periods of time, this changes as Mercury's orbit shifts.)[citation needed]Putting all these factors together, the best time for an observer in the Southern Hemisphere to see Mercury is in the morning, near the March equinox, a few days after Mercury is at greatest western elongation, or in the evening, near the September equinox, a few days before greatest eastern elongation. An observer in the Northern Hemisphere cannot optimize all the factors simultaneously. Usually, the best chances of seeing the planet are in the evening, near the March equinox, a few days before greatest eastern elongation, or in the morning, near the September equinox, a few days after greatest western elongation. The inclination of the ecliptic is then large, but Mercury is not close to aphelion.[citation needed]
Mercury's period of revolution around the Sun is 88 days. It therefore makes about 4.15 revolutions around the Sun in one Earth-year. In successive years the position of Mercury on its orbit therefore shifts by 0.15 revolutions when seen on specific dates, such as the equinoxes. Therefore, if, for example, greatest eastern elongation happens on the March equinox of some year, about three years later greatest western elongation will happen near the March equinox, because the position of Mercury on its orbit at the equinox will have changed by about half (.45) a revolution. Thus, if the timings of elongations and equinoxes are unfavourable for observing Mercury in some year, they will be fairly favourable within about three years later.[citation needed] Furthermore, because the shift of 0.15 revolutions in a year makes up a seven-year cycle (0.15 × 7 ≈ 1.0), in the seventh year Mercury will follows almost exactly (earlier by 7 days) the sequence of phenomena it showed seven years before.[92]
When conditions are near optimal, Mercury is easy to see. However, optimal conditions are rare, and many casual observers search for Mercury without success.[citation needed]
Observation history
Ancient astronomers
The earliest known recorded observations of Mercury are from the Mul.Apin tablets. These observations were most likely made by an Assyrian astronomer around the 14th century BC.[98] The cuneiform name used to designate Mercury on the Mul.Apin tablets is transcribed as Udu.Idim.Gu\u4.Ud ("the jumping planet").[e][99] Babylonian records of Mercury date back to the 1st millennium BC. The Babylonians called the planet Nabu after the messenger to the gods in their mythology.[100]The ancient Greeks of Hesiod's time knew the planet as Στίλβων (Stilbon), meaning "the gleaming", and Ἑρμάων (Hermaon).[101] Later Greeks called the planet Apollo when it was visible in the morning sky, and Hermes when visible in the evening. Around the 4th century BC, Greek astronomers came to understand that the two names referred to the same body, Hermes (Ἑρμής: Hermēs), a planetary name that is retained in modern Greek (Ερμής: Ermis).[102] The Romans named the planet after the swift-footed Roman messenger god, Mercury (Latin Mercurius), which they equated with the Greek Hermes, because it moves across the sky faster than any other planet.[103][104] The astronomical symbol for Mercury is a stylized version of Hermes' caduceus.[105]
The Roman-Egyptian astronomer Ptolemy wrote about the possibility of planetary transits across the face of the Sun in his work Planetary Hypotheses. He suggested that no transits had been observed either because planets such as Mercury were too small to see, or because the transits were too infrequent.[106]
In ancient China, Mercury was known as Chen Xing (辰星), the Hour Star. It was associated with the direction north and the phase of water in the Wu Xing.[107] Modern Chinese, Korean, Japanese and Vietnamese cultures refer to the planet literally as the "water star" (水星), based on the Five elements.[108] Hindu mythology used the name Budha for Mercury, and this god was thought to preside over Wednesday.[109] The god Odin (or Woden) of Germanic paganism was associated with the planet Mercury and Wednesday.[110] The Maya may have represented Mercury as an owl (or possibly four owls; two for the morning aspect and two for the evening) that served as a messenger to the underworld.[111]
The ancient association of Mercury with Wednesday is still visible in the names of Wednesday in various modern languages of Latin descent, e.g. mercredi in French, miércoles in Spanish, or miercuri in Romanian. The names of the days of the week were, in late classical times, all related to the names of the seven bodies that were then considered to be planets.[f][citation needed]
In ancient Indian astronomy, the Surya Siddhanta, an Indian astronomical text of the 5th century, estimates the diameter of Mercury as 4,841 kilometres (3,008 mi), an error of less than 1% from the currently accepted diameter of 4,880 kilometres (3,032 mi). This estimate was based upon an inaccurate guess of the planet's angular diameter as 3.0 arcminutes (50 millidegrees).[citation needed]
In medieval Islamic astronomy, the Andalusian astronomer Abū Ishāq Ibrāhīm al-Zarqālī in the 11th century described the deferent of Mercury's geocentric orbit as being oval, like an egg or a pignon, although this insight did not influence his astronomical theory or his astronomical calculations.[112][113] In the 12th century, Ibn Bajjah observed "two planets as black spots on the face of the Sun", which was later suggested as the transit of Mercury and/or Venus by the Maragha astronomer Qotb al-Din Shirazi in the 13th century.[114] (Note that most such medieval reports of transits were later taken as observations of sunspots.[115])
In India, the Kerala school astronomer Nilakantha Somayaji in the 15th century developed a partially heliocentric planetary model in which Mercury orbits the Sun, which in turn orbits Earth, similar to the Tychonic system later proposed by Tycho Brahe in the late 16th century.[116]
Ground-based telescopic research
The first telescopic observations of Mercury were made by Galileo in the early 17th century. Although he observed phases when he looked at Venus, his telescope was not powerful enough to see the phases of Mercury. In 1631, Pierre Gassendi made the first telescopic observations of the transit of a planet across the Sun when he saw a transit of Mercury predicted by Johannes Kepler. In 1639, Giovanni Zupi used a telescope to discover that the planet had orbital phases similar to Venus and the Moon. The observation demonstrated conclusively that Mercury orbited around the Sun.[14]
A very rare event in astronomy is the passage of one planet in front of another (occultation), as seen from Earth. Mercury and Venus occult each other every few centuries, and the event of May 28, 1737 is the only one historically observed, having been seen by John Bevis at the Royal Greenwich Observatory.[117] The next occultation of Mercury by Venus will be on December 3, 2133.[118]
The difficulties inherent in observing Mercury mean that it has been far less studied than the other planets. In 1800, Johann Schröter made observations of surface features, claiming to have observed 20 km high mountains. Friedrich Bessel used Schröter's drawings to erroneously estimate the rotation period as 24 hours and an axial tilt of 70°.[119] In the 1880s, Giovanni Schiaparelli mapped the planet more accurately, and suggested that Mercury's rotational period was 88 days, the same as its orbital period due to tidal locking.[120] This phenomenon is known as synchronous rotation. The effort to map the surface of Mercury was continued by Eugenios Antoniadi, who published a book in 1934 that included both maps and his own observations.[65] Many of the planet's surface features, particularly the albedo features, take their names from Antoniadi's map.[121]
In June 1962, Soviet scientists at the Institute of Radio-engineering and Electronics of the USSR Academy of Sciences led by Vladimir Kotelnikov became first to bounce radar signal off Mercury and receive it, starting radar observations of the planet.[122][123][124] Three years later radar observations by Americans Gordon Pettengill and R. Dyce using 300-meter Arecibo Observatory radio telescope in Puerto Rico showed conclusively that the planet's rotational period was about 59 days.[125][126] The theory that Mercury's rotation was synchronous had become widely held, and it was a surprise to astronomers when these radio observations were announced. If Mercury were tidally locked, its dark face would be extremely cold, but measurements of radio emission revealed that it was much hotter than expected. Astronomers were reluctant to drop the synchronous rotation theory and proposed alternative mechanisms such as powerful heat-distributing winds to explain the observations.[127]
Italian astronomer Giuseppe Colombo noted that the rotation value was about two-thirds of Mercury's orbital period, and proposed that the planet's orbital and rotational periods were locked into a 3:2 rather than a 1:1 resonance.[128] Data from Mariner 10 subsequently confirmed this view.[129] This means that Schiaparelli's and Antoniadi's maps were not "wrong". Instead, the astronomers saw the same features during every second orbit and recorded them, but disregarded those seen in the meantime, when Mercury's other face was toward the Sun, because the orbital geometry meant that these observations were made under poor viewing conditions.[119]
Ground-based optical observations did not shed much further light on the innermost planet, but radio astronomers using interferometry at microwave wavelengths, a technique that enables removal of the solar radiation, were able to discern physical and chemical characteristics of the subsurface layers to a depth of several meters.[130][131] Not until the first space probe flew past Mercury did many of its most fundamental morphological properties become known. Moreover, recent technological advances have led to improved ground-based observations. In 2000, high-resolution lucky imaging observations were conducted by the Mount Wilson Observatory 1.5 meter Hale telescope. They provided the first views that resolved surface features on the parts of Mercury that were not imaged in the Mariner mission.[132] Most of the planet has been mapped by the Arecibo radar telescope, with 5 km resolution, including polar deposits in shadowed craters of what may be water ice.[133]
Research with space probes
Reaching Mercury from Earth poses significant technical challenges, because the planet orbits so much closer to the Sun than Earth. A Mercury-bound spacecraft launched from Earth must travel over 91 million kilometers into the Sun's gravitational potential well. Mercury has an orbital speed of 48 km/s, whereas Earth's orbital speed is 30 km/s. Thus the spacecraft must make a large change in velocity (delta-v) to enter a Hohmann transfer orbit that passes near Mercury, as compared to the delta-v required for other planetary missions.[134]
The potential energy liberated by moving down the Sun's potential well becomes kinetic energy; requiring another large delta-v change to do anything other than rapidly pass by Mercury. To land safely or enter a stable orbit the spacecraft would rely entirely on rocket motors. Aerobraking is ruled out because the planet has very little atmosphere. A trip to Mercury requires more rocket fuel than that required to escape the Solar System completely. As a result, only two space probes have visited the planet so far.[135] A proposed alternative approach would use a solar sail to attain a Mercury-synchronous orbit around the Sun.[136]
Mariner 10
Mariner 10, the first probe to visit the innermost planet
The first spacecraft to visit Mercury was NASA's Mariner 10 (1974–1975).[103] The spacecraft used the gravity of Venus to adjust its orbital velocity so that it could approach Mercury, making it both the first spacecraft to use this gravitational "slingshot" effect and the first NASA mission to visit multiple planets.[134] Mariner 10 provided the first close-up images of Mercury's surface, which immediately showed its heavily cratered nature, and revealed many other types of geological features, such as the giant scarps which were later ascribed to the effect of the planet shrinking slightly as its iron core cools.[137] Unfortunately, due to the length of Mariner 10's orbital period, the same face of the planet was lit at each of Mariner 10's close approaches. This made observation of both sides of the planet impossible,[138] and resulted in the mapping of less than 45% of the planet's surface.[139]
On March 27, 1974, two days before its first flyby of Mercury, Mariner 10's instruments began registering large amounts of unexpected ultraviolet radiation near Mercury. This led to the tentative identification of Mercury's moon. Shortly afterward, the source of the excess UV was identified as the star 31 Crateris, and Mercury's moon passed into astronomy's history books as a footnote.[citation needed]
The spacecraft made three close approaches to Mercury, the closest of which took it to within 327 km of the surface.[140] At the first close approach, instruments detected a magnetic field, to the great surprise of planetary geologists—Mercury's rotation was expected to be much too slow to generate a significant dynamo effect. The second close approach was primarily used for imaging, but at the third approach, extensive magnetic data were obtained. The data revealed that the planet's magnetic field is much like Earth's, which deflects the solar wind around the planet. The origin of Mercury's magnetic field is still the subject of several competing theories.[141]
On March 24, 1975, just eight days after its final close approach, Mariner 10 ran out of fuel. Because its orbit could no longer be accurately controlled, mission controllers instructed the probe to shut down.[142] Mariner 10 is thought to be still orbiting the Sun, passing close to Mercury every few months.[143]
MESSENGER
A second NASA mission to Mercury, named MESSENGER (MErcury Surface, Space ENvironment, GEochemistry, and Ranging), was launched on August 3, 2004, from the Cape Canaveral Air Force Station aboard a Boeing Delta 2 rocket. It made a fly-by of Earth in August 2005, and of Venus in October 2006 and June 2007 to place it onto the correct trajectory to reach an orbit around Mercury.[144] A first fly-by of Mercury occurred on January 14, 2008, a second on October 6, 2008,[145] and a third on September 29, 2009.[146] Most of the hemisphere not imaged by Mariner 10 has been mapped during these fly-bys. The probe successfully entered an elliptical orbit around the planet on March 18, 2011. The first orbital image of Mercury was obtained on March 29, 2011. The probe finished a one-year mapping mission,[145] and then entered a one-year extended mission into 2013. In addition to continued observations and mapping of Mercury, MESSENGER observed the 2012 solar maximum.[147]
The mission is designed to clear up six key issues: Mercury's high density, its geological history, the nature of its magnetic field, the structure of its core, whether it has ice at its poles, and where its tenuous atmosphere comes from. To this end, the probe is carrying imaging devices which will gather much higher resolution images of much more of the planet than Mariner 10, assorted spectrometers to determine abundances of elements in the crust, and magnetometers and devices to measure velocities of charged particles. Detailed measurements of tiny changes in the probe's velocity as it orbits will be used to infer details of the planet's interior structure.[26]
