User:Maa0519/sandbox
Note: This page is a user sandbox page, and is not an official Wikipedia page.
Here, I present a draft to changes I might make to an official Wikipedia article, specifically the North Polar Basin (Mars)/Vastitas Borealis pages. I am contributing to two different Wikipedia pages. I discovered that each page had a contradictory definition of the other, so my aim here is to draft changes to the articles to make their differences more apparent.
Start Borealis Basin (North Polar Basin) Material
[edit]*Note: I believe it would be wise to change the main name of this article from the "North Polar Basin" to the "Borealis Basin" because the term North Polar Basin implies the feature has some relation to the North Pole of Mars, when it is really almost the entire Northern Hemisphere. *
Introductory paragraphs to add in 1st section
[edit]*Note: The first sentence here is from the original article.*
_with_poles_HiRes.jpg) The Borealis Basin is the large region lying north of the black line. Volcanic eruptions on the Tharsis bluge, the higher elevation region on the left of the image, covered over parts of the basin after its formation. | |
| Location | Northern Hemisphere, Mars |
|---|---|
| Coordinates | 67°N 208°E / 67°N 208°E |
The North Polar Basin, more commonly know as the Borealis Basin, is a large basin in the northern hemisphere of Mars that covers 40% of the planet.[1][2] Some scientists have postulated that the basin formed during the impact of a single, large body roughly 2% the mass of Mars, having a diameter of about 1,900 km (1,200 miles).[1][3] However, the basin is not currently recognized as an impact basin by the IAU. The basin is one of the flattest areas in the Solar System, and has an elliptical shape.[2][1] Chryse Planitia, the landing site of the Viking 1 lander, is a bay that opens into this basin.
Because the Borealis basin covers 40% of the surface of Mars, and much of the Northern Hemisphere, many currently recognized regions of Mars lie within it:
Borealis Impact
[edit]Formation of the Borealis Basin
[edit]*Note: The first parapraph of this section is taken directly from the North Polar Basin (Mars) Wikipedia article.*
One possible explanation for the basin's low, flat and relatively crater-free topography is that the basin was formed by a single large impact. Two simulations of a possible impact sketched a profile for the collision: low velocity—6 to 10 km (3.7 to 6.2 mi) per second—oblique angle and a diameter of 1,600–2,700 km (990–1,680 mi).[3][5] Topographical data from Mars Global Surveyor are consistent with the models and also suggest that the elliptical crater has axes of length 10,600 km (6,600 mi) and 8,500 km (5,300 mi), centered on 67°N 208°E / 67°N 208°E, though this has been partially obscured by later volcanic eruptions that created the Tharsis bulge along its rim.[2] There is evidence for a secondary rim as well, a characteristic many impact craters have .[2][6] This would make the North Polar Basin by far the largest impact crater in the Solar System, approximately four times the diameter of the next largest craters: Utopia Planitia, which is embedded inside the North Polar Basin, the South Pole–Aitken basin on the Moon, and Hellas Planitia on Mars's southern hemisphere.[7]
This impact would have resulted in significant crustal melting and a general increase in the rate of crustal formation for a period of 40 million years following the impact.[8] Such a large impact would have disturbed the mantle, altering the normal convection currents and causing upwellings which further increase the amount of melting at the impact site.[8] Overall, such an event would actually increase the rate of cooling of the Martian interior.[8] The lack of magnetic anomalies observed in the northern hemisphere could be explainded by such an impact, as the shock waves produced might have demagnetized the crust.[8]
Potential formation of Phobos and Deimos via Borealis impact
[edit]The origin of Mars' moons, Phobos and Deimos (pictured right), is unknown and remains controversial. One theory is that the moons are captured asteroids.[9] However, the moons' near circular orbits and low inclination relative to the Martian equator are not in agreement with the capture hypothesis.[10] The detection of minerals on Phobos similar to those in the Martian lithosphere, and the unusually low density and high porosity of Phobos, such that the moon would not be expected to remain aggregate if dynamically captured, suggest that the moons could have formed via accreation in Martian orbit, similar to how Earth's Moon formed.[10]
While estimates of the mass ejected by a large, Borealis-size impact vary, simulations suggest that a body approximately 0.02 Mars masses in size is capable of producing a sizable debris disk in Martian orbit, on the order of 5x1020 kg, with a significant fraction of the material remaining close to Mars. [10][3] This figure lies within the estimated mass range necessary to form the two moons, as other data suggests that only 1% of the mass of an accretion disk successfully forms moons.[10] There are several other large impact basins on Mars that could have ejected enough debris to form the moons.[10]
Ancient tsunamis
[edit]Analysis of Mars Global Surveyor data found mineral deposits similar to terminal moraines on Earth along the southern rim of the northern lowlands. Scientists have developed several theories to explain their presence, including: volcanic activity, glacial activity, and a series of Martian tsunamis.[11] The arrangement of the deposits resembles deposits observed in recent tsunami events here on Earth, and other features of the deposits are inconsistent with the volcanic and glacial hypotheses.[11] One recent investigation identified three impact craters in Acidalia Planitia as being the likely source of the hypothetical tsunamis, with the Lomonosov crater (pictured right) being the most likely candidate.[11] Here, the tsunami generated by the impactor would have reached heights of 75 m (250 ft), and traveled 150 km (90 mi) past the southern rim.[11] Dating techniques put the origin of the deposits sometime between the Late Hesperian and Early Amazonian periods, some 3 billion years ago, providing evidence to the presence of an ocean during this period.[11]
Start Vastitas Borealis Material
[edit]*Notes: The only changes I am proposing to this article are removing or changing the section that says "The North Polar Basin lies within Vastitas Borealis" as this isn't entirely accurate. If anything, the opposite is true, as The Borealis basin is almost the entire Northern Hemisphere. The image of Vastitas Borealis will not be transfered, it is just a placeholder. I will most likely update the caption of the image of the article to include coordinates.*
Vastitas Borealis is centered at 87°44′N 32°32′E / 87.73°N 32.53°E.[12]
All though it is not an officially recognized feature, the North Polar Basin makes up most of the lowlands in the Northern Hemisphere of Mars.[2][1] As a result, Vastitas Borealis lies within the North Polar Basin.
Vastitas Borealis is the large low elevation area surrounding 70°N | |
| Location | Northern Hemisphere, Mars |
|---|---|
| Length | 0-360 E |
| Width | 48.25-82.08 N |
| Diameter | 2002.91 km |
| Depth | 4-5 km |
| Naming | Latin |
References
[edit]- Martel, L.M.V. (June, 2001), "Outflow Channels May Make a Case for a Bygone Ocean on Mars", Planetary Science Research Discoveries. (retrieved 17 August 2005)
- ^ a b c d "NASA - NASA Spacecraft Reveal Largest Crater in Solar System". www.nasa.gov. Retrieved 2017-04-06.
- ^ a b c d e f Andrews-Hanna; et al. (2008). "The Borealis basin and the origin of the Martian crustal dichotomy". Nature. 453 (7199): 1212–1215. Bibcode:2008Natur.453.1212A. doi:10.1038/nature07011. PMID 18580944. S2CID 1981671.
- ^ a b c Marinova; et al. (2008). "Mega-impact formation of the Mars hemispheric dichotomy". Nature. 453 (7199): 1216–1219. Bibcode:2008Natur.453.1216M. doi:10.1038/nature07070. PMID 18580945. S2CID 4328610.
- ^ "Vastitas Borealis". Wikipedia. 2016-11-30.
- ^ Nimmo; et al. (2008). "Implications of an impact origin for the Martian hemispheric dichotomy". Nature. 453 (7199): 1220–1223. Bibcode:2008Natur.453.1220N. doi:10.1038/nature07025. PMID 18580946. S2CID 4402065.
- ^ "Huge Impact Created Mars' Split Personality". Space.com. Retrieved 2008-07-01.
- ^ Chandler, David (2008-06-25). "Solar system's biggest impact scar discovered: MIT scientists solve riddle of Mars' two-faced nature". MIT News. Retrieved 2015-01-01.
{{cite web}}: CS1 maint: url-status (link) - ^ a b c d Ghods, Abdolreza; Arkani-Hamed, Jafar (2011-09-01). "Effects of the Borealis impact on the mantle dynamics of Mars". Physics of the Earth and Planetary Interiors. 188 (1–2): 37–46. doi:10.1016/j.pepi.2011.06.010.
- ^ "Phobos (moon)". Wikipedia. 2017-03-29.
- ^ a b c d e Citron, Robert I.; Genda, Hidenori; Ida, Shigeru (2015-05-15). "Formation of Phobos and Deimos via a giant impact". Icarus. 252: 334–338. arXiv:1503.05623. doi:10.1016/j.icarus.2015.02.011. S2CID 17089080.
- ^ a b c d e Costard, Francois; Séjourné, Antoine; Kelfoun, Karim; Clifford, Stephen; Lavigne, Franck; Di Pietro, Ilaria; Bouley, Sylvain (2017-01-01). "Modeling tsunami propagation and the emplacement of thumbprint terrain in an early Mars ocean". Journal of Geophysical Research: Planets. 122 (3): 633–649. doi:10.1002/2016JE005230. ISSN 2169-9100. S2CID 132378050.
- ^ "Planetary Names: Vastitas, vastitates: Vastitas Borealis on Mars". planetarynames.wr.usgs.gov. Retrieved 2017-04-17.