Atmosphere of Mercury

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Atmosphere of Mercury[1]
SpeciesCD,[n 1] cm−2SD,[n 2] cm−3
Hydrogen (H) ~ 3 × 109 ~ 250
Molecular hydrogen < 3 × 1015 < 1.4 × 107 < 3 × 1011 ~ 6 × 103
Atomic oxygen < 3 × 1011 ~ 4 × 104
Molecular oxygen < 9 × 1014 < 2.5 × 107
Sodium ~ 2 × 1011 1.7–3.8 × 104
Potassium ~ 2 × 109 ~ 400
Calcium ~ 1.1 × 108 ~ 300
Magnesium ~ 4 × 1010 ~ 7.5 × 103
Argon ~ 1.3 × 109 < 6.6 × 106
Water < 1 × 1012 < 1.5 × 107
Other neon, silicon, sulfur, argon,
iron, carbon dioxide, etc.
  1. ↑ Column density
  2. ↑ Surface density

Mercury has a very tenuous and highly variable atmosphere (surface-bound exosphere) containing hydrogen, helium, oxygen, sodium, calcium, potassium and water vapor, with a combined pressure level of about 10−14 bar (1 nPa).[2] The exospheric species originate either from the Solar wind or from the planetary crust. Solar light pushes the atmospheric gases away from the Sun, creating a comet-like tail behind the planet.

The existence of a Mercurian atmosphere had been contentious before 1974, although by that time a consensus had formed that Mercury, like the Moon, lacked any substantial atmosphere. This conclusion was confirmed in 1974 when the Mariner 10 spacecraft discovered only a tenuous exosphere. Later, in 2008, improved measurements were obtained by the MESSENGER spacecraft, which discovered magnesium in the Mercurian exosphere.

Composition

The Mercurian exosphere consists of a variety of species originating either from the Solar wind or from the planetary crust.[3] The first constituents discovered were atomic hydrogen (H), helium (He) and atomic oxygen (O), which were observed by the ultraviolet photometer of the Mariner 10 spacecraft in 1974. The near-surface concentrations of these elements were estimated to vary from 230 cm−3 for hydrogen to 44,000 cm−3 for oxygen, with an intermediate concentration of helium.[3] In 2008 the MESSENGER probe confirmed the presence of atomic hydrogen, although its concentration appeared higher than the 1974 estimate.[4] Mercury's exospheric hydrogen and helium are believed to come from the Solar wind, while the oxygen is likely to be of crustal origin.[3]

Ca and Mg in the tail

The fourth species detected in Mercury's exosphere was sodium (Na). It was discovered in 1985 by Drew Potter and Tom Morgan, who observed its Fraunhofer emission lines at 589 and 589.6 nm.[5] The average column density of this element is about 1 × 1011 cm−2. Sodium is observed to concentrate near the poles, forming bright spots.[6] Its abundance is also enhanced near the dawn terminator as compared to the dusk terminator.[7] Some research has claimed a correlation of the sodium abundance with certain surface features such as Caloris or radio bright spots;[5] however these results remain controversial. A year after the sodium discovery, Potter and Morgan reported that potassium (K) is also present in the exosphere of Mercury, though with a column density two orders of magnitude lower than that of sodium. The properties and spatial distribution of these two elements are otherwise very similar.[8] In 1998 another element, calcium (Ca), was detected with column density three orders of magnitude below that of sodium.[9] Observations by the MESSENGER probe in 2009 showed that calcium is concentrated mainly near the equator—opposite to what is observed for sodium and potassium.[10]

In 2008 the MESSENGER probe's Fast Imaging Plasma Spectrometer (FIPS) discovered several molecular and different ions in the vicinity of Mercury, including H2O+ (ionized water vapor) and H2S+ (ionized hydrogen sulfide).[11] Their abundances relative to sodium are about 0.2 and 0.7, respectively. Other ions such as H3O+ (hydroxonium), OH (hydroxyl), O2+ and Si+ are present as well.[12] During its 2009 flyby, the Ultraviolet and Visible Spectrometer (UVVS) channel of the Mercury Atmospheric and Surface Composition Spectrometer (MASCS) on board the MESSENGER spacecraft first revealed the presence of magnesium in the Mercurian exosphere. The near-surface abundance of this newly detected constituent is roughly comparable to that of sodium.[10]

Properties

Mariner 10's ultraviolet observations have established an upper bound on the exospheric surface density at about 105 particles per cubic centimeter. This corresponds to a surface pressure of less than 10−14 bar (1 nPa).[13]

The temperature of the Mercurian exosphere depends on species as well as geographical location. For exospheric atomic hydrogen, the temperature appears to be about 420 K, a value obtained by both Mariner 10 and MESSENGER.[4] The temperature for sodium is much higher, reaching 750–1500 K on the equator and 1,500–3,500 K at the poles.[14] Some observations show that Mercury is surrounded by a hot corona of calcium atoms with temperature between 12,000 and 20,000 K.[9]

Tails

Because of Mercury's proximity to the Sun, the pressure of Solar light is much stronger than at Earth's location. Solar radiation pushes neutral atoms away from Mercury, creating a comet-like tail behind the planet.[15] The main component in the tail is sodium, which has been detected as far as 56,000 km (about 23 RM) from the planet.[15] This sodium tail expands rapidly to a diameter of about 20,000 km at a distance of 17,500 km.[16] In 2009 MESSENGER also detected calcium and magnesium in the tail, although these elements were only observed at distances less than 8 RM from the planet.[15]

See also

References

Notes

  1. ↑ Killen 2007, p. 456, Table 5
  2. ↑ "NASA—Mercury". Archived from the original on 6 October 2009. Retrieved 2009-09-26. 
  3. ↑ 3.0 3.1 3.2 Killen, 2007, pp. 433–434
  4. ↑ 4.0 4.1 McClintock 2008, p. 93
  5. ↑ 5.0 5.1 Killen, 2007, pp. 434–436
  6. ↑ Killen, 2007, pp. 438–442
  7. ↑ Killen, 2007, pp. 442–444
  8. ↑ Killen, 2007, pp. 449–452
  9. ↑ 9.0 9.1 Killen, 2007, pp. 452–453
  10. ↑ 10.0 10.1 McClintock 2009, p. 612–613
  11. ↑ "MESSENGER Scientists 'Astonished' to Find Water in Mercury's Thin Atmosphere". The Planetary Society. 2008-07-03. Archived from the original on 6 April 2010. Retrieved 2010-03-28. 
  12. ↑ Zurbuchen 2008, p. 91, Table 1
  13. ↑ Domingue, 2007, pp. 162–163
  14. ↑ Killen, 2007, pp. 436–438
  15. ↑ 15.0 15.1 15.2 McClintock 2009, p. 610–611
  16. ↑ Killen, 2007, p. 448

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