| 词条 | North Polar Basin (Mars) |
| 释义 |
|name = Borealis Basin |image = |caption = The Borealis Basin is the large blue and green region lying north of the equator. Volcanic eruptions on the Tharsis bulge, the higher elevation region on the left of the image, covered over parts of the basin after its formation. |location = Northern Hemisphere, Mars |coordinates = {{coord|67|N|208|E|globe:mars_type:landmark|display=inline,title}} }} The North Polar Basin, more commonly known 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][4] 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. Large regions within the Borealis Basin [2]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 ImpactFormation of the Borealis BasinOne 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—{{convert|6|to|10|km|mi|abbr=on}} per second—oblique angle and a diameter of {{convert|1600|-|2700|km|mi|abbr=on}}.[2][3] Topographical data from Mars Global Surveyor are consistent with the models and also suggest that the elliptical crater has axes of length {{convert|10600|km|mi|abbr=on}} and {{convert|8500|km|mi|abbr=on}}, centered on {{Coord|67|N|208|E|globe:Mars}}, 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.[4][5] 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 imbedded inside the North Polar Basin, the South Pole–Aitken basin on the Moon, and Hellas Planitia on Mars's southern hemisphere.[6] 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.[7] 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.[7] Overall, such an event would actually increase the rate of cooling of the Martian interior.[7] The lack of magnetic anomalies observed in the northern hemisphere could be explained by such an impact, as the shock waves produced might have demagnetized the crust.[7] Potential formation of Phobos and Deimos via Borealis impactThe origin of Mars' moons, Phobos and Deimos (pictured right), is unknown and remains controversial. One theory is that the moons are captured asteroids. However, the moons' near circular orbits and low inclination relative to the Martian equator are not in agreement with the capture hypothesis.[18] 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 accretion in Martian orbit, similar to how Earth's Moon formed.[18] 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.[8][2] 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.[8] There are several other large impact basins on Mars that could have ejected enough debris to form the moons.[8] Ancient tsunamisAnalysis 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.[9] 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.[9] 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.[9] 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.[9] 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.[9] See also
References
1. ^1 2 {{Cite web|url=https://www.nasa.gov/home/hqnews/2008/jun/HQ_08159_Mars_crater.html|title=NASA - NASA Spacecraft Reveal Largest Crater in Solar System|website=www.nasa.gov|language=en|access-date=2017-04-06}} {{Geography of Mars}}{{portal bar|Mars}}2. ^1 2 {{cite journal |title=Mega-impact formation of the Mars hemispheric dichotomy |author=Marinova |journal=Nature |volume=453 |pages=1216–1219 |doi=10.1038/nature07070 |year=2008 |pmid=18580945 |last2=Aharonson |first2=O |last3=Asphaug |first3=E |issue=7199 |bibcode=2008Natur.453.1216M |display-authors=1 }} 3. ^{{cite journal |title=Implications of an impact origin for the Martian hemispheric dichotomy |author=Nimmo |journal=Nature |volume=453 |pages=1220–1223 |doi=10.1038/nature07025 |year=2008 |pmid=18580946 |last2=Hart |first2=SD |last3=Korycansky |first3=DG |last4=Agnor |first4=CB |issue=7199 |bibcode=2008Natur.453.1220N |display-authors=1 }} 4. ^1 2 3 4 {{cite journal|title=The Borealis basin and the origin of the Martian crustal dichotomy|author=Andrews-Hanna|journal=Nature|volume=453|pages=1212–1215|doi=10.1038/nature07011|year=2008|pmid=18580944|last2=Zuber|first2=MT|last3=Banerdt|first3=WB|issue=7199|bibcode = 2008Natur.453.1212A|display-authors=1 }} 5. ^{{cite web|url=http://www.space.com/scienceastronomy/080625-mars-impact.html|title=Huge Impact Created Mars' Split Personality|accessdate=2008-07-01|publisher=Space.com}} 6. ^{{cite web|url=http://newsoffice.mit.edu/2008/solar-systems-biggest-impact-scar-discovered|title=Solar system's biggest impact scar discovered: MIT scientists solve riddle of Mars' two-faced nature|author=Chandler, David|date=2008-06-25|accessdate=2015-01-01|publisher=MIT News|deadurl=no}} 7. ^1 2 3 {{Cite journal|last=Ghods|first=Abdolreza|last2=Arkani-Hamed|first2=Jafar|date=2011-09-01|title=Effects of the Borealis impact on the mantle dynamics of Mars|url=http://www.sciencedirect.com/science/article/pii/S0031920111001324|journal=Physics of the Earth and Planetary Interiors|volume=188|issue=1–2|pages=37–46|doi=10.1016/j.pepi.2011.06.010|bibcode=2011PEPI..188...37G}} 8. ^1 2 3 4 {{Cite journal|last=Citron|first=Robert I.|last2=Genda|first2=Hidenori|last3=Ida|first3=Shigeru|date=2015-05-15|title=Formation of Phobos and Deimos via a giant impact|url=http://www.sciencedirect.com/science/article/pii/S0019103515000639|journal=Icarus|volume=252|pages=334–338|doi=10.1016/j.icarus.2015.02.011|arxiv=1503.05623|bibcode=2015Icar..252..334C}} 9. ^1 2 3 4 {{Cite journal|last=Costard|first=Francois|last2=Séjourné|first2=Antoine|last3=Kelfoun|first3=Karim|last4=Clifford|first4=Stephen|last5=Lavigne|first5=Franck|last6=Di Pietro|first6=Ilaria|last7=Bouley|first7=Sylvain|date=2017-01-01|title=Modeling tsunami propagation and the emplacement of thumbprint terrain in an early Mars ocean|journal=Journal of Geophysical Research: Planets|volume=122|issue=3|language=en|pages=2016JE005230|doi=10.1002/2016JE005230|issn=2169-9100|bibcode=2017JGRE..122..633C}} 1 : Surface features of Mars |
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