Moons of Mars

Color image of Phobos (MRO, 23 March 2008)
Color image of Deimos (MRO, 21 February 2009)

The two moons of Mars are Phobos and Deimos.[1] Both were discovered by Asaph Hall in August 1877[2] and are named after the Greek mythological twin characters Phobos (panic/fear) and Deimos (terror/dread) who accompanied their father Ares, god of war, into battle. Ares was known as Mars to the Romans.

Phobos orbits closer to Mars, with a semi-major axis of 9,377 km (5,827 mi) to Deimos' 23,460 km (14,580 mi).

History

Early speculation

Curiosity's view of the Martian moons: Phobos passing in front of Deimos – in real-time (video-gif, 1 August 2013)

The existence of the moons of Mars had been speculated about since the moons of Jupiter were discovered. It is known that when Galileo, as a hidden report about him having observed two bumps on the sides of Saturn (later discovered to be its rings), used the anagram smaismrmilmepoetaleumibunenugttauiras for Altissimum planetam tergeminum observavi ("I have observed the most distant planet to have a triple form"), Johannes Kepler had misinterpreted it to mean Salve umbistineum geminatum Martia proles (Hello, furious twins, sons of Mars).[3]

Perhaps inspired by Kepler (and quoting Kepler's third law of planetary motion), Jonathan Swift's satire Gulliver's Travels (1726) refers to two moons in Part 3, Chapter 3 (the "Voyage to Laputa"), in which Laputa's astronomers are described as having discovered two satellites of Mars orbiting at distances of 3 and 5 Martian diameters with periods of 10 and 21.5 hours. Phobos and Deimos (both found in 1877, more than a century after Swift's novel) have actual orbital distances of 1.4 and 3.5 Martian diameters, and their respective orbital periods are 7.66 and 30.35 hours.[4][5] In the 20th century, V. G. Perminov, a spacecraft designer of early Soviet Mars and Venus spacecraft, speculated Swift found and deciphered records that Martians left on Earth.[6] However, the view of most astronomers is that Swift was simply employing a common argument of the time, that as the inner planets Venus and Mercury had no satellites, Earth had one and Jupiter had four (known at the time), that Mars by analogy must have two. Furthermore, as they had not yet been discovered, it was reasoned that they must be small and close to Mars. This would lead Swift to making a roughly accurate estimate of their orbital distances and revolution periods. In addition Swift could have been helped in his calculations by his friend, the mathematician John Arbuthnot.[7]

Voltaire's 1752 short story "Micromégas", about an alien visitor to Earth, also refers to two moons of Mars. Voltaire was presumably influenced by Swift.[8][9] In recognition of these 'predictions', two craters on Deimos are named Swift and Voltaire,[10][11] while on Phobos there is one named regio, Laputa Regio, and one named planitia, Lagado Planitia, both of which are named after places in Gulliver's Travels (the fictional Laputa, a flying island, and Lagado, imaginary capital of the fictional nation Balnibarbi).[12] Many of the craters on Phobos are also named after characters in Gulliver's Travels.[13]

Discovery

Asaph Hall discovered Deimos on 12 August 1877 at about 07:48 UTC and Phobos on 18 August 1877, at the US Naval Observatory in Washington, D.C., at about 09:14 GMT (contemporary sources, using the pre-1925 astronomical convention that began the day at noon, give the time of discovery as 11 August 14:40 and 17 August 16:06 Washington mean time respectively).[14][15][16] At the time, he was deliberately searching for Martian moons. Hall had previously seen what appeared to be a Martian moon on 10 August, but due to bad weather, he could not definitively identify them until later.

Hall recorded his discovery of Phobos in his notebook as follows:[17]

The telescope used to discover the Martian moons

"I repeated the examination in the early part of the night of 11th [August 1877], and again found nothing, but trying again some hours later I found a faint object on the following side and a little north of the planet. I had barely time to secure an observation of its position when fog from the River stopped the work. This was at half past two o'clock on the night of the 11th. Cloudy weather intervened for several days.
"On 15 August the weather looking more promising, I slept at the Observatory. The sky cleared off with a thunderstorm at 11 o'clock and the search was resumed. The atmosphere however was in a very bad condition and Mars was so blazing and unsteady that nothing could be seen of the object, which we now know was at that time so near the planet as to be invisible.
"On 16 August the object was found again on the following side of the planet, and the observations of that night showed that it was moving with the planet, and if a satellite, was near one of its elongations. Until this time I had said nothing to anyone at the Observatory of my search for a satellite of Mars, but on leaving the observatory after these observations of the 16th, at about three o'clock in the morning, I told my assistant, George Anderson, to whom I had shown the object, that I thought I had discovered a satellite of Mars. I told him also to keep quiet as I did not wish anything said until the matter was beyond doubt. He said nothing, but the thing was too good to keep and I let it out myself. On 17 August between one and two o'clock, while I was reducing my observations, Professor Newcomb came into my room to eat his lunch and I showed him my measures of the faint object near Mars which proved that it was moving with the planet.
"On 17 August while waiting and watching for the outer moon, the inner one was discovered. The observations of the 17th and 18th put beyond doubt the character of these objects and the discovery was publicly announced by Admiral Rodgers."

The telescope used for the discovery was the 26-inch (66 cm) refractor (telescope with a lens) then located at Foggy Bottom.[18] In 1893 the lens was remounted and put in a new dome, where it remains into the 21st century.[19]

The names, originally spelled Phobus and Deimus, respectively, were suggested by Henry Madan (1838–1901), Science Master of Eton, from Book XV of the Iliad, where Ares summons Fear and Fright.[20]

Mars moon hoax

In 1959, Walter Scott Houston perpetrated a celebrated April Fool's hoax in the April edition of the Great Plains Observer, claiming that "Dr. Arthur Hayall of the University of the Sierras reports that the moons of Mars are actually artificial satellites". Both Dr. Hayall and the University of the Sierras were fictitious. The hoax gained worldwide attention when Houston's claim was repeated in earnest by a Soviet scientist, Iosif Shklovsky,[21] who, based on a later-disproven density estimate, suggested Phobos was a hollow metal shell.

Recent surveys

Searches have been conducted for additional satellites. In 2003, Scott S. Sheppard and David C. Jewitt surveyed early the entire Hill sphere of Mars for irregular satellites. However scattered light from Mars prevented them from searching the inner few arcminutes where the satellites Phobos and Deimos reside. No new satellites were found to an apparent limiting red magnitude of 23.5, which corresponds to radii of about 0.09 km using an albedo of 0.07.[22]

Characteristics

Apparent sizes of the moons of Mars, Deimos and Phobos, and the Moon as viewed from the surface of their respective planets (Curiosity rover, 1 August 2013)

If viewed from Mars's surface near its equator, full Phobos looks about one third as big as a full moon on Earth. It has an angular diameter of between 8' (rising) and 12' (overhead). It would look smaller when the observer is further away from the Martian equator, and is completely invisible from Mars's polar ice caps. Deimos looks more like a bright star or planet for an observer on Mars, only slightly bigger than Venus looks from Earth; it has an angular diameter of about 2'. The Sun's angular diameter as seen from Mars, by contrast, is about 21'. Thus there are no total solar eclipses on Mars, as the moons are far too small to completely cover the Sun. On the other hand, total lunar eclipses of Phobos are very common, happening almost every night.[23]

The motions of Phobos and Deimos would appear very different from that of our own Moon. Speedy Phobos rises in the west, sets in the east, and rises again in just eleven hours, while Deimos, being only just outside synchronous orbit, rises as expected in the east but very slowly. Despite its 30-hour orbit, it takes 2.7 days to set in the west as it slowly falls behind the rotation of Mars.

Both moons are tidally locked, always presenting the same face towards Mars. Since Phobos orbits Mars faster than the planet itself rotates, tidal forces are slowly but steadily decreasing its orbital radius. At some point in the future, when it approaches Mars closely enough (see Roche limit), Phobos will be broken up by these tidal forces.[24] Several strings of craters on the Martian surface, inclined further from the equator the older they are, suggest that there may have been other small moons that suffered the fate expected of Phobos, and that the Martian crust as a whole shifted between these events.[25] Deimos, on the other hand, is far enough away that its orbit is being slowly boosted instead,[26] as in the case of our own Moon.

Orbital details

Name and pronunciation Image Diameter (km) Surface

Area (km)

 Mass (kg) Semi-major
axis (km)		 Orbital
period (h)		 Average moonrise
period (h, d)
Mars I Phobos /ˈfoʊbəs/
FOH-bəs
22.2 km (13.8 mi)(27×21.6×18.8 km) 1,548 km 1.08×1016 9,377 km (5,827 mi) 7.66 11.12 h (0.463 d)
Mars II Deimos /ˈdaɪmɒs/
DY-moss
12.6 km (7.8 mi)
(10×12×16 km)		 483 km 2×1015 23,460 km (14,580 mi) 30.35 131 h (5.44 d)
The relative sizes of and distance between Mars, Phobos, and Deimos, to scale

(Load the image in full size to see both Moons of Mars.)

Origin

Animation illustrating the asteroid-belt origin for the moons

The origin of the Martian moons is still controversial.[27] Phobos and Deimos both have much in common with carbonaceous C-type asteroids, with spectra, albedo, and density very similar to those of C- or D-type asteroids.[28] Based on their similarity, one hypothesis is that both moons may be captured main-belt asteroids.[5][29] Both moons have very circular orbits which lie almost exactly in Mars's equatorial plane, and hence a capture origin requires a mechanism for circularizing the initially highly eccentric orbit, and adjusting its inclination into the equatorial plane, most probably by a combination of atmospheric drag and tidal forces,[30] although it is not clear that sufficient time is available for this to occur for Deimos.[27] Capture also requires dissipation of energy. The current atmosphere of Mars is too thin to capture a Phobos-sized object by atmospheric braking.[27] Geoffrey Landis has pointed out that the capture could have occurred if the original body was a binary asteroid that separated under tidal forces.[29]

Phobos could be a second-generation Solar System object that coalesced in orbit after Mars formed, rather than forming concurrently out of the same birth cloud as Mars.[31]

Another hypothesis is that Mars was once surrounded by many Phobos- and Deimos-sized bodies, perhaps ejected into orbit around it by a collision with a large planetesimal.[32] The high porosity of the interior of Phobos (based on the density of 1.88 g/cm3, voids are estimated to comprise 25 to 35 percent of Phobos' volume) is inconsistent with an asteroidal origin.[33] Observations of Phobos in the thermal infrared suggest a composition containing mainly phyllosilicates, which are well known from the surface of Mars. The spectra are distinct from those of all classes of chondrite meteorites, again pointing away from an asteroidal origin.[34] Both sets of findings support an origin of Phobos from material ejected by an impact on Mars that reaccreted in Martian orbit,[35] similar to the prevailing theory for the origin of Earth's moon.

The moons of Mars may have started with a huge collision with a protoplanet one third the mass of Mars that formed a ring around Mars. The inner part of the ring formed a large moon. Gravitational interactions between this moon and the outer ring formed Phobos and Deimos. Later, the large moon crashed into Mars, but the two small moons remained in orbit. This theory agrees with the fine-grained surface of the moons and their high porosity. The outer disk would create fine-grained material.[36][37]

Exploration

While many Martian probes provided images and other data about Phobos and Deimos, only few were dedicated to these satellites and intended to perform a flyby or landing on the surface.

Two probes under the Soviet Phobos program were successfully launched in 1988, but neither conducted the intended jumping landings on Phobos and Deimos due to failures (although Phobos 2 successfully photographed Phobos). The post-Soviet Russian Fobos-Grunt probe was intended to be the first sample return mission from Phobos, but a rocket failure left it stranded in Earth orbit in 2011.

In 1997 and 1998, the Aladdin mission was selected as a finalist in the NASA Discovery Program. The plan was to visit both Phobos and Deimos, and launch projectiles at the satellites. The probe would collect the ejecta as it performed a slow flyby. These samples would be returned to Earth for study three years later. Ultimately, NASA rejected this proposal in favor of MESSENGER, a probe to Mercury.

In 2007, the European Space Agency and EADS Astrium proposed and developed a mission to Phobos in 2016 with a lander and sample return, but this mission was never flown. Since 2007 the Canadian Space Agency has been considering the PRIME mission to Phobos with orbiter and lander. Since 2008 NASA Glenn Research Center began studying a Phobos and Deimos sample return mission. Since 2013 NASA developed the Phobos Surveyor mission concept with an orbiter and a small rover that is proposed to launch sometime after 2023. Proposed NASA's PADME mission proposes to launch in 2020 and reach Mars orbit in 2021 to conduct multiple flybys of the Martian moons. Also, NASA is assessing the OSIRIS-REx II, concept mission for a sample return from Phobos.[38] Another sample return mission from Deimos, called Gulliver. has been conceptualized. Russia plans to repeat Fobos-Grunt mission around 2024.

Orbits of moons and spacecraft orbiting Mars.[40]

See also

References

  1. ↑ "NASA - Under the Moons of Mars". Nasa.gov. Retrieved 28 February 2013.
  2. ↑ "The Planet Mars: A History of Observation and Discovery. Chapter 5: 1877. University of Arizona Press". Uapress.arizona.edu. Retrieved 2013-02-28.
  3. ↑ Galileo, Kepler, & Two Anagrams: Two Wrong Solutions Turn Into Two Correct Solutions
  4. ↑ MathPages – Galileo's Anagrams and the Moons of Mars
  5. 1 2 "Close Inspection for Phobos". One idea is that Phobos and Deimos, Mars's other moon, are captured asteroids.
  6. ↑ V. G. Perminov – The Difficult Road to Mars (1999) – NASA Archived 5 August 2006 at the Wayback Machine.
  7. ↑ Roscoe Lamont, 'The Moons of Mars' in Popular Astronomy Vol. 33 (1925), pp496 - 8
  8. ↑ William Sheehan, The Planet Mars: A History of Observation and Discovery
  9. ↑ Voltaire explained that since Mars is further from the Sun than Earth is, it could not make do with less than two moons. (Patrick Moore, 2000, The Wandering Astronomer)
  10. ↑ "Swift". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
  11. ↑ "Voltaire". Gazetteer of Planetary Nomenclature. USGS Astrogeology Research Program.
  12. ↑ Gazetteer of Planetary Nomenclature USGS Astrogeology Research Program, Phobos
  13. ↑ "Gazetteer of Planetary Nomenclature, Phobos Craers". International Astronomical Union. Retrieved 10 January 2018.
  14. ↑ "Notes: The Satellites of Mars". The Observatory, Vol. 1, No. 6. 20 September 1877. pp. 181–185. Retrieved 12 September 2006.
  15. ↑ Hall, A. (17 October 1877). "Observations of the Satellites of Mars" (Signed 21 September 1877). Astronomische Nachrichten, Vol. 91, No. 2161. pp. 11/12–13/14. Retrieved 12 September 2006.
  16. ↑ Morley, T. A.; A Catalogue of Ground-Based Astrometric Observations of the Martian Satellites, 1877-1982, Astronomy and Astrophysics Supplement Series, Vol. 77, No. 2 (February 1989), pp. 209–226 (Table II, p. 220: first observation of Phobos on 1877-08-18.38498)
  17. ↑ "The Discovery of the Satellites of Mars". Monthly Notices of the Royal Astronomical Society, Vol. 38, No. 4. 8 February 1878. pp. 205–209. Retrieved 12 September 2006.
  18. ↑ Naval Observatory 26-inch Refractor
  19. ↑ The 26-inch "Great Equatorial" Refractor
  20. ↑ Hall, A. (14 March 1878). "Names of the Satellites of Mars" (Signed 7 February 1878). Astronomische Nachrichten, Vol. 92, No. 2187. pp. 47–48. Retrieved 12 September 2006.
  21. ↑ Jefferson City Post-Tribune 4 May 1959
  22. ↑ Astron. J., 128, 2542–2546 (2004)
  23. ↑ Moon Shadows: "Somewhere near the martian equator, Phobos eclipses the sun nearly every day."
  24. ↑ Nemiroff, R.; Bonnell, J., eds. (14 April 2008). "Phobos: Doomed Moon of Mars". Astronomy Picture of the Day. NASA. In 100 million years or so Phobos will likely be shattered by stress caused by the relentless tidal forces, the debris forming a decaying ring around Mars.
  25. ↑ New Map Provides More Evidence Mars Once Like Earth: "… the new map shows evidence of features, transform faults, that are a "tell-tale" of plate tectonics on Earth."
  26. ↑ Sahife 6: "Deimos orbits far enough away from Mars that it is being slowly pushed farther and farther away from the planet."
  27. 1 2 3 Burns, J. A. "Contradictory Clues as to the Origin of the Martian Moons," in Mars, H. H. Kieffer et al., eds., U. Arizona Press, Tucson, 1992
  28. ↑ "New Views of Martian Moons".
  29. 1 2 Landis, G. A. "Origin of Martian Moons from Binary Asteroid Dissociation," American Association for the Advancement of Science Annual Meeting; Boston, MA, 2001; abstract.
  30. ↑ Cazenave, A.; Dobrovolskis, A.; Lago, B. (1980). "Orbital history of the Martian satellites with inferences on their origin". Icarus. 44 (3): 730–744. Bibcode:1980Icar...44..730C. doi:10.1016/0019-1035(80)90140-2.
  31. ↑ Martin Pätzold & Olivier Witasse (4 March 2010). "Phobos Flyby Success". ESA. Retrieved 4 March 2010.
  32. ↑ Craddock, R. A.; (1994); The Origin of Phobos and Deimos, Abstracts of the 25th Annual Lunar and Planetary Science Conference, held in Houston, TX, 14–18 March 1994, p. 293
  33. ↑ Andert, T. P.; Rosenblatt, P.; Pätzold, M.; Häusler, B.; et al. (7 May 2010). "Precise mass determination and the nature of Phobos". Geophysical Research Letters. American Geophysical Union. 37 (L09202): n/a. Bibcode:2010GeoRL..37.9202A. doi:10.1029/2009GL041829. Retrieved 1 October 2010.
  34. ↑ Giuranna, M.; Roush, T. L.; Duxbury, T.; Hogan, R. C.; et al. (2010). "Compositional Interpretation of PFS/MEx and TES/MGS Thermal Infrared Spectra of Phobos" (PDF). European Planetary Science Congress Abstracts, Vol. 5. Retrieved 1 October 2010.
  35. ↑ "Mars Moon Phobos Likely Forged by Catastrophic Blast". www.space.com. Space.com. 27 September 2010. Retrieved 1 October 2010.
  36. ↑ 1.Pascal Rosenblatt, Sébastien Charnoz, Kevin M. Dunseath, Mariko Terao-Dunseath, Antony Trinh, Ryuki Hyodo, Hidenori Genda, Stéven Toupin. Accretion of Phobos and Deimos in an extended debris disc stirred by transient moons. Nature Geoscience, 2016; DOI: 10.1038/ngeo2742
  37. ↑ CNRS. "A giant impact: Solving the mystery of how Mars' moons formed." ScienceDaily. ScienceDaily, 4 July 2016. <www.sciencedaily.com/releases/2016/07/160704144236.htm>.
  38. ↑ OSIRIS-REx II to Mars: Mars Sample Return from Phobos and Deimos. Elifritz, T. L. (2012)
  39. ↑
  40. ↑ Webster, Guy (4 May 2015). "Traffic Around Mars Gets Busy". NASA. Retrieved May 5, 2015.

Further reading

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