Ina (crater)
Ina
Ina (LRO).jpg
Ina seen by Lunar Reconnaissance Orbiter. Small crater at lower left is Osama, at upper left - Dag; the biggest hill in right part of Ina is Mons Agnes. Image width is
Coordinates 18°40?N 5°18?E / 18.66°N 5.30°E / 18.66; 5.30Coordinates: 18°40?N 5°18?E / 18.66°N 5.30°E / 18.66; 5.30
Diameter 2.9×1.9 km[1]
Depth 64 m[1]
Eponym Latin female name Ina
The floor of Ina lighted by low Sun (6.6° above the horizon). Image width is 1 km
Mons Agnes: the only named hill inside Ina. Image width is 1 km

Ina is a peculiar small depression ("crater" in IAU nomenclature) on the Moon, in Lacus Felicitatis. It is , wide and 64 m deep (from the deepest point of the bottom to the highest point of the rim).[1]

Ina is remarkable for several dozens of low hills with flat or rounded tops and very sharp rounded boundaries, looking like drops of mercury.[1][2] Their surface looks like usual surface of the Moon, and the space between them is strongly different. Ina is the most prominent of several dozens of similar features on the Moon. Their origin is unclear.[3][4][5]

Discovery, exploration and naming

Ina was discovered on photographs taken in 1971 by the Apollo 15 crew from lunar orbit.[2] It could have been found 5 years earlier, on images by Lunar Orbiter 4, but a photographic flaw prevented this.[2][6] At the end of 1972 it was observed and photographed by the Apollo 17 crew.[7][8][9] Later it was explored by orbiting spacecraft. Beginning in 2009, Lunar Reconnaissance Orbiter obtained photos of Ina with resolution of about 0.5 m/pixel and with varying illumination angles.[9][10]

In 1974 on a topophotomap, published by NASA,[11] this feature was given the Latin female name Ina, according to a tradition to give small lunar craters first human names.[12] In 1979 this name was adopted by International Astronomical Union.[13] The feature is also called D-caldera in Apollo-era publications due to its shape, and at the time it was believed to be a unique feature on the moon.[1][8]

Two neighbouring features were named together with Ina in 1976. They are small craters Osama on its southwestern edge and Dag to the northwest (both 400 m in diameter). The widest hill in the eastern part of Ina (650 m wide) is named Mons Agnes (named in 1979).

Description

Ina is located on the top of rounded upland (dome) 300 m high and 15 km in diameter.[14][15] It is situated on elongated plateau (horst) about 30 km wide.[1][14][16] This plateau stands in the middle of Lacus Felicitatis - a small lunar lake between Mare Serenitatis, Mare Vaporum and Mare Imbrium.

Ina is a D-shaped depression 2.9×1.9 km wide. It has an elevated rim 600-1000 wide and 30-40 m high. Eastern part of the rim is 10 m higher than western. Its outer slope is very gently sloping (1-3°) and lacks a distinct edge, but inner slope is very steep (tens of degrees) and has very sharp border with the depression. The deepest point of the depression is located somewhat to northwest from its center. This point is 30 m deeper than edges of the depression and 64 m deeper than the highest point of the rim.[1]

There are 2 clearly distinct types of surface inside Ina: hills and lowlands. Surface of the hills looks like usual surface of Lacus Felicitatis, and surface of the lowlands is strongly different.[10][14]

There are several dozens of the hills inside Ina. They have very diverse sizes and rounded amoeba-like edges, like drops of mercury.[1][2] Many of them are connected with other hills or with edge of depression.[1] They are rather low (5-25, usually 10-15 m[1][14][17]). Their tops are flat or slightly rounded, but the slopes are very steep. Edges of the hills are usually very sharp. Often they are surrounded by a little moat. Boundary of the hills and lowland has the same appearance as the outer boundary of the depression. The surface of the hills is very smooth compared to the lowlands. In addition, although the sample size is not great, the hills do have an impact crater density intermediate between the fresh lowlands and the ancient neighboring plains of Lacus Felicitatis.[1][10]

Ina lowlands are much more rough than hills, with lots of small irregular relief features, but their height is no more than several meters.[1] Some craters are also discernible there.[10] Somewhere the lowland contains small patches of very bright tone. They are outcrops of scattered rocks in size. Such patches are located mainly near the border of lowland and hills, especially in the lowest places.[1][6][10]

Ina lowlands are bright bluish-grey. The hills are darker and brown (like the usual lunar surface).[1][7][9][16] The lowlands resemble freshly exposed basalt with high titanium content, like the basalt seen in some young impact craters. Ina is surrounded by a weak dark halo.[6][15] The surface of its surrounds is slightly more blue than the more distant surface.[14]

Analogs

Ina is the most prominent, large and well-known representative of class of features called irregular mare patches,[18] which are also known as "meniscus hollows" for similarity of their edges to a convex meniscus.[19] Several dozens of such features are known on the Moon, all located in the maria. They are hypothesized to be volcanic in origin, but several hypotheses exist and their origin is far from certain.[18][19][20][21] Somewhat similar, but distinct, features ("hollows") are rather common on Mercury. These features differ from lunar meniscus hollows by presence of bright halo; they are also more widespread, often bigger and usually located in impact craters.[3][4][5]

Interpretations

Age

Surface of Ina lowlands seems to be much younger than the surface of the hills and outer surroundings. Evidence of this includes light color and low concentration of craters on these lowlands. The Moon surface darkens over time, and multiple meteorite impacts dot it with craters, blur sharp edges of all relief features and make slopes more gentle.[9][15][16][21] Ina seems to be one of the youngest features on the Moon.[10] The surface of the hills is much older: its age seems to be roughly equal to the age of usual surface of Lacus Felicitatis (more than 1 billion years[10]), but the slopes and edges of these hills are young: they couldn't maintain their steepness and sharpness even for 50 million years.[15][22] The dome, which hosts Ina, seems to be somewhat younger, than its surroundings, judging from crater concentration.[1][14]

On the other hand, there is a lower estimation of age of the tops of Ina's hills: 33±2 million years (it is based on crater counts with the result of 137 craters/km2 for craters >10 m in diameter).[20][23][24]

Latest research suggests Ina is not so young.[25] They looked at well-studied volcanoes on Earth that might be similar to Ina. Ina appears to be a pit crater on a shield volcano, a gently sloping mountain similar to the Kilauea volcano in Hawaii. Kilauea has a pit crater similar to Ina known as the Kilauea Iki crater, which erupted in 1959.

As lava from that eruption solidified, it created a highly porous rock layer inside the pit, with underground vesicles as large as three feet in diameter and surface void space as deep as two feet. That porous surface, Head and his colleagues say, is created by the nature of the lava erupted in the late stages of events like this one. As the subsurface lava supply starts to diminish, it erupts as "magmatic foam" - a bubbly mixture of lava and gas. When that foam cools and solidifies, it forms the highly porous surface.

The researchers suggest that an Ina eruption would have also produced magmatic foam. And because of the Moon's decreased gravity and nearly absent atmosphere, the lunar foam would have been even fluffier than on Earth, so it's expected that the structures within Ina are even more porous than on Earth.

It's the high porosity of those surfaces that throws off date estimates for Ina, both by hiding the buildup of regolith and by throwing off crater counts.

A highly porous surface, the researchers say, would allow loose rock and dust to filter into surface void space, making it appear as though less regolith has built up. That process would be perpetuated by seismic shaking in the region, much of which is caused by ongoing meteor impacts. "It's like banging on the side of a sieve to make the flour go through," Head said. "Regolith is jostled into holes rather than sitting on the surface, which makes Ina look a lot younger."

Porosity could also skew crater counts. Laboratory experiments using a high-speed projectile cannon have shown that impacts into porous targets make much smaller craters. Because of Ina's extreme porosity, the researchers say, its craters are much smaller than they would normally be, and many craters might not be visible at all. That could drastically alter the age estimate derived from crater counts.

The researchers estimate that the porous surface would reduce by a factor of three the size of craters on Ina's mounds. In other words, an impactor that would make a 100-foot-diameter crater in lunar basalt bedrock would make a crater of a little over 30 feet in a foam deposit.

Taking that scaling relationship into account, the team gets a revised age for the Ina mounds of about 3.5 billion year old. That's similar to the surface age of the volcanic shield that surrounds Ina, and places the Ina activity within the timeframe of common volcanism on the Moon.

The researchers believe this work offers a plausible explanation for Ina's formation without having to invoke the puzzling billion-year pause in volcanic activity.

"We think the young-looking features in Ina are the natural consequence of magmatic foam eruptions on the Moon," Head said. "These landforms created by these foams simply look a lot younger than they are."

Origin

Ina's origin is unclear as of 2015.[21] Firstly it was interpreted as a caldera of a very low ancient volcano.[6][7] Another version considers it as a result of powerful ejection of some gases (volcanic or even radiogenic), which removed regolith. In that case the hills are places where the original regolith was preserved. The other hypothesis says that the hills are lava flows, inflated during growth under some dense coating.[1][10][16] All these versions have flaws.[21] In particular, Ina does not seem to have a ring of volcanic ejecta, and the volcanic activity on the Moon seems to be ceased a long time ago.[15]

According to one another version, Ina appeared (and continues to form) due to collapsing of the regolith into some underground cavities. They can be ancient lava tubes[21] or a result of evaporation of some volatile compounds.[22] In that case the bright rocky places on Ina's floor are places, where the regolith has already fallen down, darker parts of lowlands are places of incomplete collapsing, and the hills are slowly diminishing remains of primigenial surface.[22]

References

  1. ^ a b c d e f g h i j k l m n o p Garry, W. B.; Robinson, M. S.; Zimbelman, J. R.; Bleacher, J. E.; Hawke, B. R.; Crumpler, L. S.; et al. (November 2012). "The origin of Ina: Evidence for inflated lava flows on the Moon" (PDF). Journal of Geophysical Research. 117 (E12): E00H31. Bibcode:2012JGRE..117.0H31G. doi:10.1029/2011JE003981. Archived from the original on November 4, 2014.  (mini-version, Bibcode2011LPI....42.2605G, map)
  2. ^ a b c d Whitaker, E.A. (1972). "An unusual mare feature". Apollo 15 Preliminary Science Report (NASA Special Publication 289) (PDF). pp. 25-84-25-85. 
  3. ^ a b Blewett, D. T.; Chabot, N. L.; Denevi, B. W.; et al. (September 2012). "Hollows on Mercury: MESSENGER Evidence for Geologically Recent Volatile-Related Activity". Science. 333 (6051): 1856-1859. Bibcode:2011Sci...333.1856B. PMID 21960626. doi:10.1126/science.1211681. 
  4. ^ a b Blewett, D. T.; Vaughan, W. M.; Xiao, Zh.; Chabot, N. L.; Denevi, B. W.; Ernst, C. M.; et al. (May 2013). "Mercury's hollows: Constraints on formation and composition from analysis of geological setting and spectral reflectance" (PDF). Journal of Geophysical Research: Planets. 118 (5): 1013-1032. Bibcode:2013JGRE..118.1013B. doi:10.1029/2012JE004174. Archived from the original on December 18, 2013. 
  5. ^ a b Thomas, R. J.; Rothery, D. A.; Conway, S. J.; Anand, M. (February 2014). "Hollows on Mercury: Materials and mechanisms involved in their formation". Icarus. 229: 221-235. Bibcode:2014Icar..229..221T. doi:10.1016/j.icarus.2013.11.018. 
  6. ^ a b c d El-Baz, F. (1972). New geological findings in Apollo 15 lunar orbital photography (PDF). Proceedings of the Lunar Science Conference. 1. pp. 44-47. Bibcode:1972LPSC....3...39E. Archived from the original on November 4, 2014. 
  7. ^ a b c Evans, R.E.; El-Baz F. (1973). "28. Geological observations from lunar orbit" (PDF). Apollo 17 Preliminary Science Report (NASA Special Publication 330). pp. 28-25-28-26. 
  8. ^ a b El-Baz, F. (1973). "D-caldera: New photographs of a unique feature" (PDF). Apollo 17 Preliminary Science Report (NASA Special Publication 330). 1: 30-13-30-17. Bibcode:1973NASSP.330...30E. Archived from the original on November 4, 2014. 
  9. ^ a b c d Staid, M.; Isaacson, P.; Petro, N.; Boardman, J.; Pieters, C. M.; Head, J. W.; et al. (March 7-11, 2011). The Spectral Properties of Ina: New Observations from the Moon Mineralogy Mapper (PDF). 42nd Lunar and Planetary Science Conference. The Woodlands, Texas (published March 2011). p. 2499. Bibcode:2011LPI....42.2499S. 
  10. ^ a b c d e f g h Robinson, M. S.; Thomas, P. C.; Braden, S. E.; Lawrence, S. J.; Garry, W. B.; LROC Team. (March 1-5, 2010). High Resolution Imaging of Ina: Morphology, Relative Ages, Formation (PDF). 41st Lunar and Planetary Science Conference (published March 2010). p. 2592. Bibcode:2010LPI....41.2592R. 
  11. ^ "Sheet 41C3S1(10) Ina". NASA lunar topophotomap (based on Apollo 15 photos). Scale 1:10,000 (1st ed.). Prepared and published by the Defence Mapping Agency Topographic Center, Washington, D.C. 1974. 
  12. ^ "Categories for Naming Features on Planets and Satellites". Gazetteer of Planetary Nomenclature. International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). Archived from the original on 2014-11-02. Retrieved . 
  13. ^ "Ina". Gazetteer of Planetary Nomenclature. International Astronomical Union (IAU) Working Group for Planetary System Nomenclature (WGPSN). 2010-10-18. Retrieved . 
  14. ^ a b c d e f Strain, P. L.; El-Baz, F. (March 17-21, 1980). The geology and morphology of Ina. Proceedings of 11th Lunar and Planetary Science Conference. 3. Houston, TX (published 1980). pp. 2437-2446. Bibcode:1980LPSC...11.2437S. 
  15. ^ a b c d e Schultz, P. H.; Staid, M. I.; Pieters, C. M. (November 2006). "Lunar activity from recent gas release" (PDF). Nature. 444 (7116): 184-186. Bibcode:2006Natur.444..184S. PMID 17093445. doi:10.1038/nature05303. Archived from the original on November 4, 2014.  (popular review, archived copy)
  16. ^ a b c d Garry, W. B.; Hawke, B. R.; Crites, S.; Giguere, T.; Lucey, P. G. (March 18-22, 2013). Optical Maturity (OMAT) of Ina 'D-Caldera', the Moon (PDF). 44th Lunar and Planetary Science Conference. The Woodlands, Texas (published March 2013). p. 3058. Bibcode:2013LPI....44.3058G. 
  17. ^ Vaughan, W.M. "Topography of Ina: image from Garry et al., 2012". Ina. Archived from the original on November 3, 2014. Retrieved . 
  18. ^ a b Wood, Charles. "Strange Little IMPs." Sky and Telescope, February 2015 issue.
  19. ^ a b Stooke, P. J. (March 19-23, 2012). Lunar Meniscus Hollows (PDF). 43rd Lunar and Planetary Science Conference. The Woodlands, Texas (published March 2012). Bibcode:2012LPI....43.1011S. 1011. 
  20. ^ a b Braden, S. E.; Robinson, M. S.; Stopar, J. D.; van der Bogert, C. H.; Hawke, B. R. (March 18-22, 2013). Age and Extent of Small, Young Volcanic Activity on the Moon (PDF). 44th Lunar and Planetary Science Conference. The Woodlands, Texas (published March 2013). p. 2843. Bibcode:2013LPI....44.2843B. 
  21. ^ a b c d e Chan, N. W.; Vaughan, W. M.; Head, J. W. (March 17-21, 2014). Lunar Ina-Like Features: Maps and Morphometry (PDF). 45th Lunar and Planetary Science Conference. The Woodlands, Texas (published March 2014). p. 1001. Bibcode:2014LPI....45.1001C.  (poster)
  22. ^ a b c Vaughan, W.M.; Head, J.W. "Ina: Lunar sublimation terrain?". Vaughan Will Vaughan's page. planetary.brown.edu. Archived from the original on 2014-11-04. Retrieved . 
  23. ^ Braden, S.; Robinson, M. S.; Stopar, J. D. (December 2013). "Evidence of young volcanic vents in the lunar maria". American Geophysical Union, Fall Meeting 2013, abstract #V53C-2809. 53. Bibcode:2013AGUFM.V53C2809B. 
  24. ^ Braden S. E.; Stopar J. D.; Robinson M. S.; Lawrence S. J.; van der Bogert C. H., Hiesinger H. (2014). "Evidence for basaltic volcanism on the Moon within the past 100 million years". Nature Geoscience. 7 (11): 787-791. Bibcode:2014NatGe...7..787B. doi:10.1038/ngeo2252.  (Supplementary material)
  25. ^ "Ina pit crater on the Moon: Extrusion of waning-stage lava lake magmatic foam results in extremely young crater retention ages Qiao,Le et al. Geology(2017),:G38594.1". 

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Ina_(crater)



 

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