Dominant group/Planetary science

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Within planetary science, in theory, there may be at least two meanings of dominant group: (1) a dominant group of objects, sources, and entities, or (2) a dominant group in some way associated with objects, sources, or entities, or with planetary science itself. Emphasis may be on an object rather than by association.

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In the first sense, some such objects with respect to the Moon, for example, consist of a lunar boulder, soil, and terrain. The second sense seems to use the Moon only as a back drop for investigations on Earth, for example, the effects of lunar tides or the Moon Treaty. Or, may refer to groups who influence the field of planetary science. The first is more substantive, the second more subjective.

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Contents

Notation [edit]

Notation: let the symbol Def. indicate that a definition is following.

Notation: let the symbols between [ and ] be replacement for that portion of a quoted text.

Universals [edit]

To help with definitions, their meanings and intents, there is the learning resource theory of definition.

Def. evidence that demonstrates that a concept is possible is called proof of concept.

The proof-of-concept structure consists of

  1. background,
  2. procedures,
  3. findings, and
  4. interpretation.[1]

The findings demonstrate a statistically systematic change from the status quo or the control group.

Planetary may refer to objects in orbit around a star, or objects that wander around the sky, especially at night. The latter such objects may be gaseous objects, rocky objects, or plasma objects, even liquid objects.

Rocky-objects [edit]

This geologic province map depicts features approximately 150 km across and greater due to the fact that the resolution of the maps is consistent with the resolution of the seismic refraction data. Credit: USGS.

"Silicates are the dominant group minerals in the Earth's crust."[2]

"Tcs are dominated by the volumetrically dominant Group A grains in the pillow interior and are generally between 130 and 190°C (sub-samples d–l at depths of 1.5 to 6.2 cm from the rim"[3]

Much of the use of dominant group relative to the Earth (rocky object) is described in dominant group/Geology.

Meteors [edit]

The photograph shows a meteor during the peak of the 2009 Leonid Meteor Shower, its afterglow and wake as distinct components. Credit: Navicore.

"The distribution of photographic meteors in iron, stony, and porous meteors is given in this paper".[4] "[A]mong all the 217 meteors for which we know the beginning there are 70 iron meteors, i. e. about 32 p. c., and 147 stony meteors, i. e. 68 p. c."[4] The meteor streams: Perseids, Geminids, Taurids, Lyrids, κ Cygnids and Virginids, are quite stony.[4]

"The dominant group in all cases are stony meteors."[4]

Meteorites [edit]

This is a small sample from the NWA 2373 Meteorite. Credit: James St. John.
This is a micrometeorite collected from the antarctic snow. Credit: NASA.

Roughly three-quarters of all Martian meteorites can be classified as shergottites. "[T]he most frequent type of rock (basaltic lithologies) among all known Martian meteorites is the basaltic shergottites."[5]

"The dominant group of Martian meteorites, shergottites, are divided into two subgroups consisting of basalts and lherzolites.[6]

"The highly refractory elements ... are followed by the dominant group of refractory lithophile elements (Si, P, and the alkali-earth and transition elements typical of chondrules, which condense down to 1,300 K."[7]

Micrometeorite is often abbreviated as MM. Most MMs are broadly chondritic in composition, meaning "that major elemental abundance ratios are within about 50% of those observed in carbonaceous chondrites."[8] Some MMs are chondrites, (basaltic) howardite, eucrite, and diogenite (HED) meteorites or Martian basalts, but not lunar samples.[8] "[T]he comparative mechanical weakness of carbonaceous precursor materials tends to encourage spherule formation."[8] From the number of different asteroidal precursors, the approximate fraction in MMs is 70 % carbonaceous.[8] "[T]he carbonaceous material [is] known from observation to dominate the terrestrial MM flux."[8] The "H, L, and E chondritic compositions" are "dominant among meteorites but rare among micrometeorites."[8]

"Ureilites occur about half as often as eucrites (Krot et al. 2003), are relatively friable, have less a wide range of cosmic-ray exposure ages including two less than 1 Myr, and, like the dominant group of MM precursors, contain carbon."[8]

"These particles belong to the dominant group of micrometeorites which are related to the CM chondrites and show a relatively low degree of PAH alkylation."[9]

Meteoroids [edit]

A meteoroid is a suggested term for a sand- to boulder-sized particle of debris in the Solar System. The visible path of a meteoroid that enters the Earth's atmosphere (or another body's) atmosphere is called a meteor, or colloquially a shooting star or falling star. If a meteoroid reaches the ground and survives impact, then it is called a meteorite.

"A meteoroid is a sand- to boulder-sized particle of debris in the Solar System."[10]

"The silicate spheres are the most dominant group."[11]

Moon [edit]

A map of Mare Serenitatis. The colored arrows indicate the landing places of Luna 21, Apollo 15, and Apollo 17.

The Apollo 17 highland samples are classified into groups according to proportions of meteoritic iridium (Ir), gold (Au), and germanium (Ge) by atomic concentration.[12] Ni is the elemental symbol for nickel and Re is the elemental symbol for rhenium.

"It is quite distinct from the Group 2 component (Ir/Au - 0.46-0.54) that dominates at the Apollo 17 site."[12] "[I]f the dominant Group 2 component at Apollo 17 comes from the Serenitatis projectile, then the component in Boulder 2-1 must come from another projectile, older or younger."[12] "Sixteen samples of Boulder 1 from Station 2 at the Apollo 17 site were analyzed".[12] Remaining Apollo 17 data other than from Boulder 2-1 (Boulder 1 from Station 2) are included.[12]

"Nine out of 10 well-characterized Apollo 17 breccia matrices fall into Group 2, and this includes both the blue-grey breccias which are the dominant rock type at this site"[12].

KREEP, an acronym built from the letters K (the atomic symbol for potassium), REE (Rare Earth Elements) and P (for phosphorus), is a geochemical component of some lunar impact melt breccia and basalt rocks.

"Glasses from Apollo 11, 12, 14, and 15 soil samples have been grouped on the basis of their chemistry".[13] More than half of the Apollo 14 soil glasses belong to the group of glasses that relate to KREEP-type basalts.[13] "KREEP-type glasses in the Apollo 15 soil samples closely resemble the ones in the Apollo 14 samples".[13] Of 399 glasses analyzed, the single largest group of glasses, numbering 140, relate to KREEP-type basalts.[13]

"Because KREEP glasses are the dominant group at the Fra Mauro sampling site and because the Fra Mauro formation is considered part of the Imbrian ejecta blanket, KREEP basalts appear to have been part of the lunar crust prior to formation of the Imbrium Basin."[13]

"These glasses are the dominant group in soil 60501 and also in 61221 if the pure feldspar glasses are discounted."[14]

The lunar impact glasses from the Apollo 14 landing site show significant variation and hint at the existence of multiple terrains of differing compositions near the landing site.[15] Gamma-ray spectrometer observations show a high concentration of potassium, rare Earth element, and phosphorus (KREEP) around and at the Apollo 14 landing site.[15] "Lunar impact glasses record the composition, in refractory element ratios, of the material from which they were formed."[15] By far the most populous group of Apollo 14 impact glasses by compositional distribution on a ternary diagram of aluminum (Al), iron (Fe), and titanium (Ti), is a diffuse cluster of glasses elevated in KREEP called the "high-K Fra Mauro basalt" (HKFM).[15]

"The glass data from Apollo 14 soil 14259,624 show that the bulk composition of the deposit at the site is dominated by high-K Fra Mauro ‘‘basalt."[15]

"In addition to that dominant group of glasses, we find smaller groups of more feldspathic glasses, in particular a tight cluster of ‘‘highland basalt’’ glasses, similar to glasses and soils found at the Apollo 16 site and in lunar meteorites (Figure 5 and Table 2)."[15]

Interplanetary dust [edit]

"It is found that near 1 AU, the dominant group of the local geometrical cross section changes."[16] Approximately 80 % of interplanetary dust is cometary at R ~ 0.8 AU.

Mars [edit]

This image shows an arcuate curvilinear ridge in Terra Meridiani. Credit: NASA/JPL/University of Arizona.

The "enigmatic linear and curvilinear features (hereinafter referred to as LCFs) that in general are visible as thin dark, or rarely white lines in satellite images of the Martian surface ... are in such abundance that they are even visible in Viking images."[17]

"The color code indicates the most dominant group of LCFs in the image."[17]

Asteroids [edit]

This is a composite image, to scale, of the asteroids which have been imaged at high resolution. As of 2011 they are, from largest to smallest: 4 Vesta, 21 Lutetia, 253 Mathilde, 243 Ida and its moon Dactyl, 433 Eros, 951 Gaspra, 2867 Šteins, 25143 Itokawa. Credit: NASA/JPL-Caltech/JAXA/ESA.

"Asteroids in particularly large classes tend to be broken into subgroups with the first letter denoting the dominant group and the succeeding letters denoting less prominent spectral affinities or subgroups."[18]

"The recent investigation of the orbital distribution of Centaurs (Emel’yanenko et al., 2005) showed that there are two dynamically distinct classes of Centaurs, a dominant group with semimajor axes a > 60 AU and a minority group with a < 60 AU."[19] "[T]he intrinsic number of such objects is roughly an order of magnitude greater than that for a<60 AU"[19].

"From the dominant group, the asteroids evolve to intersect the Earth's orbit on a median time scale of about 60 Myr."[20] "The MB group is the most numerous group of MCs. ... 50 % of the MB Mars-crossers [MCs] become ECs within 59.9 Myr and [this] contribution ... dominates the production of ECs"[20]. MB denotes the main belt of asteroids.[20] EC denotes Earth-crossing.[20]

Liquid objects [edit]

"Why are their essays and books about the endangered earth so monological -- that is, a conversation of a dominant group talking to itself?"[21]

Much of the use of dominant group relative to the Earth (liquid object) is described in dominant group/Geography.

Gaseous objects [edit]

Searching with Google scholar has been unsuccessful in finding any use of dominant group and the gaseous objects Jupiter, Neptune, Saturn, or Uranus. A search using "gaseous planets", "gas planets", or "giant planets" with dominant group produced no results. Dominant group is associated with comets and asteroids, in turn, near to or originating from influences by these planets.

Dominant group does show up with respect to these gaseous objects in mythology.

Much of the use of dominant group relative to the Earth (gaseous object) is described in dominant group/Atmospheric science.

Plasma objects [edit]

A magnetohydrodynamics (MHD) and chemical comet-coma model is applied to describe and analyze the plasma flow, magnetic field, and ion abundances in Comet Halley.[22] A comparison of model results is made with the data from the Giotto mission.[22]

"In the second dominant group of ions we generally see more discrepancies in the model and the HIS data".[22]

The principal application of the dominant group concept is to the ion density measurements at or within 1500 km of the comet nucleus, where "the model abundances for the light ions, up to 21 amu, are in very good agreement with the 1500 km observations."[22]

The comparison between model and measurements "generally becomes worse as one considers higher molecular masses and greater distance from the [comet] nucleus."[22]

"In fact, observations of the volatiles in 9P/Tempel 1 indicate that the abundance ratios for most species in the ejecta are in the range of those found for the dominant group of Oort Cloud comets (Mumma et al. 2005), implying that many short-period comets maintain the components they had on leaving the trans-Neptunian region at 1 m of depth from the surface, even after numerous perihelion passages."[23]

"In particular, the O isotopic ratios of the dominant Group 1 grains (Figure 4) are consistent both with spectroscopic observations of O-rich red giants and AGB stars (Harris & Lambert 1984) and with model calculations of dredge-up processes in these stars (labeled curve in Figure 4) (Boothroyd & Sackmann 1999, Dearborn 1992, El Eid 1994)."[24]

"The dominant group of detectable eclipsing binaries consists of two detached main-sequence stars."[25] "In the case of survey model 1 and a flat initial mass ratio distribution, this subgroup of systems accounts for 60% of the population of detectable eclipsing binaries."[25] "In this exploratory study we used the BiSEPS binary population synthesis code to estimate the number of eclipsing binaries and single stars detectable in the Galactic disc by an idealised Super-WASP exoplanet transit survey."[25]

See also [edit]

References [edit]

  1. ↑ Ginger Lehrman and Ian B Hogue, Sarah Palmer, Cheryl Jennings, Celsa A Spina, Ann Wiegand, Alan L Landay, Robert W Coombs, Douglas D Richman, John W Mellors, John M Coffin, Ronald J Bosch, David M Margolis (August 13, 2005). "Depletion of latent HIV-1 infection in vivo: a proof-of-concept study". Lancet 366 (9485): 549-55. doi:10.1016/S0140-6736(05)67098-5. Retrieved on 2012-05-09. 
  2. ↑ Martin Schoonen, Alexander Smirnov, Corey Cohn (December 2004). "A Perspective on the Role of Minerals in Prebiotic Synthesis". AMBIO: A Journal of the Human Environment 33 (8): 539-51. doi:10.1579/0044-7447-33.8.539. Retrieved on 2012-01-02. 
  3. ↑ Weiming Zhou, Rob Van der Voo, Donald R Peacor, Youxue Zhang (June 2000). "Variable Ti-content and grain size of titanomagnetite as a function of cooling rate in very young MORB". Earth and Planetary Science Letters 179 (1): 9-20. doi:10.1016/S0012-821X(00)00100-X. Retrieved on 2012-02-10. 
  4. ↑ 4.0 4.1 4.2 4.3 Zd. Ceplecha (1958). "On the composition of meteors". Bulletin of the Astronomical Institutes of Czechoslovakia 9: 154-9. Bibcode: 1958BAICz...9..154C. Retrieved on 2011-08-10. 
  5. ↑ Script error
  6. ↑ Takashi Mikouchi and Masamichi Miyamoto (March 2000). "Lherzolitic Martian meteorites Allan Hills 77005, Lewis Cliff 88516 and Yamato-793605: Major and minor element zoning in pyroxene and plagioclase glass". Antarctic Meteorite Research 13 (3): 256-69. Bibcode: 2000AMR....13..256M. Retrieved on 2011-08-07. 
  7. ↑ Francis Albaréde (October 29, 2009). "Volatile accretion history of the terrestrial planets and dynamic implications". Nature 461 (7268): 1227-33. doi:10.1038/nature08477. Retrieved on 2012-04-27. 
  8. ↑ 8.0 8.1 8.2 8.3 8.4 8.5 8.6 Susan Taylor, Gregory F. Herzog, Gregory, Jeremy S. Delaney, (2007). "Crumbs from the crust of Vesta: Achondritic cosmic spherules from the South Pole water well". Meteoritics & Planetary Science 42 (2): 223-33. doi:10.1111/j.1945-5100.2007.tb00229.x. Bibcode: 2007M&PS...42..223T. Retrieved on 2011-08-07. 
  9. ↑ S. J. Clemett, X. D. F. Chillier, S. Gillette, R. N. Zare, M. Maurette, C. Engrand and G. Kurat (October 1998). "Observation of Indigenous Polycyclic Aromatic Hydrocarbons in ‘Giant’ carbonaceous Antarctic Micrometeorites". Origins of Life and Evolution of Biospheres 28 (4-6): 425-48. doi:10.1023/A:1006572307223. Retrieved on 2012-01-02. 
  10. ↑ (December 10, 2012) "Meteoroid". Wikimedia Commons. San Francisco, California: Wikimedia Foundation, Inc. Retrieved on 2012-12-11. 
  11. ↑ M.B. Blanchard, D.E. Brownlee, T.E. Bunch, P.W. Hodge, F.T. Kyte (January 1980). "Meteoroid ablation spheres from deep-sea sediments". Earth and Planetary Science Letters 46 (2): 178-90. doi:10.1016/0012-821X(80)90004-7. Retrieved on 2012-01-02. 
  12. ↑ 12.0 12.1 12.2 12.3 12.4 12.5 John W. Morgan, H. Higuchi, and Edward Anders (November-December 1975). "Meteoritic material in a boulder from the Apollo 17 site - Implications for its origin". The Moon 14 (12): 373-83. doi:10.1007/BF00569671. Bibcode: 1975Moon...14..373M. Retrieved on 2011-08-07. 
  13. ↑ 13.0 13.1 13.2 13.3 13.4 Joseph Nelen, Albert Noonan, and Kurt Fredriksson (1972). "Lunar glasses, breccias, and chondrules". Proceedings of the Lunar Science Conference 2: 723-37. Bibcode: 1972LPSC....3..723N. Retrieved on 2011-08-07. 
  14. ↑ W.I. Ridley, A.M. Reid, J. Warner, R.W. Brown, R. Gooley, and C. Donaldson (March 1973). "Major Element Composition of Glasses in two Apollo 16 Soils and a Comparison with Luna 20 Glasses". Abstracts of the Lunar and Planetary Science Conference 4 (3): 625-7. Bibcode: 1973LPI.....4..625R. Retrieved on 2012-01-02. 
  15. ↑ 15.0 15.1 15.2 15.3 15.4 15.5 N. E. B. Zellner, P. D. Spudis, J. W. Delano, D. C. B. Whittet (2002). "Impact glasses from the Apollo 14 landing site and implications for regional geology". Journal of Geophysical Research 107 (E11): 5102-14. doi:10.1029/2001JE001800. Bibcode: 2002JGRE..107.5102Z. Retrieved on 2011-08-09. 
  16. ↑ Hiroshi Ishimoto (June 1998). "Collisional evolution and the resulting mass distribution of interplanetary dust". Earth, Planets, and Space 50 (6): 521-9. Bibcode: 1998EP%26S...50..521I. Retrieved on 2011-10-06. 
  17. ↑ 17.0 17.1 Jens Ormö, Goro Komatsu (June 21, 2003). "Mars Orbiter Camera observation of linear and curvilinear features in the Hellas basin: Indications for multiple processes of formation". Journal of Geophysical Research 108 (E6): 5059-71. doi:10.1029/2002JE001980. Retrieved on 2012-01-02. 
  18. ↑ Paul Robert Weissman, Torrence V. Johnson (2007). Lucy-Ann Adams McFadden, Paul Robert Weissman, Torrence V. Johnson. ed. Encyclopedia of the Solar System, Second Edition. San Diego, California, USA: Academic Press. pp. 966. ISBN 0120885891. http://books.google.com/books?id=G7UtYkLQoYoC&lr=&source=gbs_navlinks_s. Retrieved 2012-12-11. 
  19. ↑ 19.0 19.1 V. V. Emel’yanenko (December 2005). "Structure and dynamics of the Centaur population: constraints on the origin of short-period comets". Earth, Moon, and Planets 97 (3-4): 341-51. doi:10.1007/s11038-006-9095-5. Retrieved on 2011-10-06. 
  20. ↑ 20.0 20.1 20.2 20.3 Patrick Michel, Fabbio Migliorini, Alessandro Morbidelli, Vincenzo Zappalà (June 2000). "The Population of Mars-Crossers: Classification and Dynamical Evolution". Icarus 145 (2): 332-47. doi:10.1006/icar.2000.6358. Retrieved on 2011-10-06. 
  21. ↑ James H. Cone (March 22, 2000). "Whose earth is it anyway?". Cross Currents (Spring-Summer). Retrieved on 2012-02-10. 
  22. ↑ 22.0 22.1 22.2 22.3 22.4 R. Wegmann, H.U. Schmidt, W.F. Huebner, and D.C. Boice (November 1987). "Cometary MHD and chemistry". Astronomy and Astrophysics 187 (1-2): 339-50. Bibcode: 1987A&A...187..339W. Retrieved on 2011-08-07. 
  23. ↑ T. Kadono, S. Sugita, S. Sako, T. Ootsubo, M. Honda, H. Kawakita, T. Miyata, R. Furusho, and J. Watanabe (May 20, 2007). "The Thickness and Formation Age of the Surface Layer on Comet 9P/Tempel 1". The Astrophysical Journal 661 (1): L89-92. Retrieved on 2012-12-10. 
  24. ↑ Donald D. Clayton, Larry R. Nittler (September 2004). "Astrophysics with presolar stardust". Annual Review of Astronomy and Astrophysics 42: 39-78. doi:10.1146/annurev.astro.42.053102.134022. Retrieved on 2012-12-10. 
  25. ↑ 25.0 25.1 25.2 B. Willems, U. Kolb, and S. Justham (April 2006). "Eclipsing binaries in extra solar planet transit surveys: the case of SuperWASP". Monthly Notices of the Royal Astronomical Society 367 (3): 1103-12. doi:10.1111/j.1365-2966.2006.10041.x. Retrieved on 2011-10-06. 

Further reading [edit]

  • Bill Cooke (August 2006). "The Great Interplanetary Rock Swap". Astronomy 34 (8): 64–67. 
  • Script error
  • Randy Korotev (2005). "Lunar geochemistry as told by lunar meteorites". Chemie der Erde 65: 297–346. doi:10.1016/j.chemer.2005.07.001. Bibcode: 2005ChEG...65..297K. 
  • Script error
  • Susan Taylor, Gregory F. Herzog, Gregory, Jeremy S. Delaney, (2007). "Crumbs from the crust of Vesta: Achondritic cosmic spherules from the South Pole water well". Meteoritics & Planetary Science 42 (2): 223-33. doi:10.1111/j.1945-5100.2007.tb00229.x. Bibcode: 2007M&PS...42..223T. Retrieved on 2011-08-07. 
  • Script error

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