Stormarnas ocean
| Månkrater | ||
|---|---|---|
| Stormarnas ocean latin: Oceanus Procellarum | ||
 Stormarnas oceans läge är här markerat med en röd ring. | ||
| Egenskaper | ||
| Latitud Longitud | [1] | |
| Medeldiameter | 2568 km [1] | |
| Kartposition | ||
| Månen - Selenografi - ( ) | ||
 Hitta fler artiklar om Astronomi med Astronomiportalen | ||
Stormarnas ocean (latin: Oceanus Procellarum) är det största av månhaven[2] och utgör en basaltisk lavaslätt på månens framsida. Slätten bildades för mellan 3,1 miljarder[3] och 3,5 miljarder år sedan.[4] Stormarnas ocean sträcker sig 2 500 km i nord-sydlig riktning,[5] och täcker en yta av 1 692 000 km²,[6] och ligger i anslutning till de mindre månhaven Molnens hav (Mare Nubium), Vätskornas hav (Mare Humorum) och Regnens hav (Mare Imbrium).[7]
Slätten är gigantisk och oregelbundet formad och innehåller en mycket stor mängd kratrar, bergskedjor och andra formationer, såsom exempelvis kratern Aristarchus, och den stora kratern Copernicus.[8]
Namngivning
Det latinska namnet omnämns för första gången i Jan Hevelius verk Selenographia från 1647.[9] Namnet blev officiell internationell standard efter en omröstning i generalförsamlingen för den Internationella astronomiska unionen (IAU) 1935.[1]
Geologi
Vulkanutbrott på Aristarchusplatån är troligtvis källan till en stor del av materialet i Stormarnas ocean. I oceanen beräknas den totala volymen basalt vara 8,7 × 105 km3, vilket är cirka 10 procent av den totala volymen på månen.[4] Detta innebär att slätten innehar den största oavbrutna förekomsten av basalt på månen.[10]
En teori gör gällande att Stormarnas ocean bildades där det ligger på grund av ett gigantisk nedslag som skedde då månens yta ännu var flytande, eller delvis flytande. Stormarnas ocean är enligt den teorin endast en del av den nordvästra delen av nedslagskratern. På grund av att det finns en koncentration av radioaktiva grundämnen där under har stora mängder basalt smält och blivit lava som därefter kunnat tränga upp och nå ytan. Något som underlättats av att nedslaget ledde till att ytan i området blev tunnare. Det anses då vara förklaringen till varför vulkanismen har varit extra omfattande där.[11]
Analyser av albedon och den spektrisk reflektionsförmågan av basaltet i Stormarnas ocean pekar på att det troligtvis har tillkommit vid fyra olika tillfällen då lava strömmat upp från månens inre och bildat lager som vardera tros vara några hundra meter tjocka.[10]
Månlandningar på Stormarnas ocean
Den sovjetiska sonden Luna 9 mjuklandade på Stormarnas ocean den 31 januari 1966.[12] Den 24 december samma år landade sonden Luna 13 där.[13]
Den första amerikanska mjuklandningen på en annan himlakropp gjordes i Stormarnas ocean av sonden Surveyor 1, den 2 juni 1966. Sonden tog 11 240 fotografier av landningsplatsen och mätte även temperatur och radarreflektiviteten i området. Den 20 april året därpå landade den amerikanska sonden Surveyor 3 i området. Surveyor 3 hade instrument för att kontrollera hållfastheten av månmaterialet och kunde gräva små diken. Detta övervakades och analyserades genom de 6 326 bilder som skickades tillbaka till jorden.[14] I november 1969 landade Apollo 12 på den östra delen av Stormarnas ocean där astronauterna undersökte Surveyor 3 och samlade ihop 34 kg material vilket togs med tillbaka till jorden.[3][15]
Galleri
Namnen på de större månhaven och några kratrar på månens framsida. Oceanus Procellarum befinner sig till vänster på bilden.
Stormarnas ocean är det stora månhavet i mitten och i det övre vänstra hörnet av bilden.
Astronauten Alan Bean blev den fjärde personen att gå på månen då han klev ut ur landaren i den östra delen av Stormarnas ocean.
Uråldriga sprickdalar på fotografi från den 1 oktober 2014.
En konstnärs tolkning av sprickdalarna.
Referenser
Noter
- ^ [a b c] Gazetteer of Planetary Nomenclature (2009). ”Moon: Oceanus Procellarum” (på engelska). USGS och IAU. Arkiverad från originalet den 15 mars 2012. https://www.webcitation.org/66AzyRPTo?url=http://planetarynames.wr.usgs.gov/?feature=64564. Läst 13 juli 2009.
- ^ Hans Rickman (1999). ”Meteorstorm i Stormarnas Ocean”. Uppsala Astronomiska Observatorium. Arkiverad från originalet den 15 mars 2012. https://www.webcitation.org/66AztnuRk?url=http://www.astro.uu.se/astnews/1999/December/99Dec1.html. Läst 13 juli 2009.
- ^ [a b] Lunar and Planetary Institute. ”20. Surface of the Moon — Astronaut Oceanus Procellarum, Moon” (på engelska). Arkiverad från originalet den 15 mars 2012. https://www.webcitation.org/66AzsDHmk?url=http://www.lpi.usra.edu/publications/slidesets/3dsolarsystem/slide_20.html. Läst 10 juli 2009.
- ^ [a b] James L. Whitford-Stark; James W. Head III (1980). ”Stratigraphy of Oceanus Procellarum Basalts: Sources and Styles of Emplacement” (på engelska). American Geophysical Union. Arkiverad från originalet den 15 mars 2012. https://www.webcitation.org/66Azt1cPw?url=http://www.agu.org/pubs/crossref/1980/JB085iB11p06579.shtml. Läst 10 juli 2009.
- ^ ESA Multimedia Gallery
- ^ Chuck Wood. ”Lunar Mare Areas” (på engelska). Lunar Photo Of the Day. Arkiverad från originalet den 15 mars 2012. https://www.webcitation.org/66Azwo9Xz?url=http://www.lpod.org/cwm/DataStuff/MareAreas.htm. Läst 13 juli 2009.
- ^ Siew Meng Chong; Albert Chee Hoon Lim, Poon Seng Ang (2002) (på engelska). Photographic Atlas of the Moon. Cambridge University Press. sid. 73. ISBN 0521813921. http://www.google.be/books?hl=sv&lr=&id=vIcFxgAs-C8C&oi=fnd&pg=PA72&dq=%22Montes+Carpatus%22+%2B+%22Oceanus+Procellarum%22&ots=SdcckROcNx&sig=Ir7RY9c_gpQbDbqiC_46gt4deUw&redir_esc=y#v=onepage&q=%22Montes%20Carpatus%22%20%2B%20%22Oceanus%20Procellarum%22&f=false. Läst 13 april 2012
- ^ Fred Schaaf (på engelska). The 50 best sights in astronomy and how to see them. sid. 188-189
- ^ Th. Westrin (red.) (1917). ”Nordisk familjebok / Uggleupplagan. 25 bandet: Sekt – Slöjskifling - Selene-Selensyra”. Nordisk familjebok, digitalt inscannat av Projekt Runeberg. Arkiverad från originalet den 15 mars 2012. https://www.webcitation.org/66AzxZrx9?url=https://runeberg.org/nfce/0027.html. Läst 13 juli 2009.
- ^ [a b] William A. Ambrose (2009). ”Timing, Emplacement, and Distribution of Mare-Fill Units in Oceanus Procellarum, a Large Nearside Lunar Basin” (på engelska) (PDF). Search and Discovery Article #70063. Arkiverad från originalet den 15 mars 2012. https://www.webcitation.org/66B000k3r?url=http://www.searchanddiscovery.com/documents/2009/70063ambrose/ndx_ambrose.pdf. Läst 13 juli 2009.
- ^ Charles J. Byrne (2007). ”Interior of the Near Side Megabasin of the Moon” (på engelska) (PDF). Lunar and Planetary Science XXXVIII. Arkiverad från originalet den 15 mars 2012. https://www.webcitation.org/66B00xaTh?url=http://www.lpi.usra.edu/meetings/lpsc2007/pdf/1248.pdf. Läst 10 juli 2009.
- ^ Larry Kellog (2001). ”Luna 9” (på engelska). NASA. Arkiverad från originalet den 15 mars 2012. https://www.webcitation.org/66B01j6On?url=http://lunar.arc.nasa.gov/history/timeline/info/luna901.htm.
- ^ Robert Christy. ”The Mission of Luna 13” (på engelska). Zarya, Soviet, Russian and International Spaceflight. Arkiverad från originalet den 15 mars 2012. https://www.webcitation.org/66B02dCW9?url=http://www.zarya.info/Diaries/Luna/Luna13.php. Läst 13 juli 2009.
- ^ Lunar and Planetary Programs Division Office of Space Science and Applications (1969) (på engelska). Surveyor - Program Results. NASA. sid. 7. http://ntrs.nasa.gov/archive/nasa/casi.ntrs.nasa.gov/19690027073_1969027073.pdf
- ^ Ronald Greeley (1992) (på engelska). Planetary landscapes (2). Springer. sid. 76. http://books.google.se/books?id=bcrA9rpZ_JEC&printsec=frontcover&dq=Oceanus+Procellarum&source=gbs_similarbooks_r&cad=2
Media som används på denna webbplats
Författare/Upphovsman:
- Moon_names.jpg: Original uploader was Tauʻolunga at en.wikipedia
- derivative work: Inteloutside2 (talk)
Lunar nearside with major maria and craters labeled
cylindrical map projection of the Moon. The Moon's whole surface was mapped by the Clementine spacecraft in 1994, here North is at the top. The dark floor of crater Plato is at the middle top above Mare Imbrium, while the bright floor and rays of crater Tycho is near the middle bottom below Mare Imbrium. Mare Procellarum is at the near left, and Mare Tranquillitatis is just right of centre and Mare Crisium is at the near right. The far left and far right show the contrast of the mostly cratered farside with small isolated mare.
Red dot, based on the image on en:.
Författare/Upphovsman: Rursus, Licens: CC BY-SA 3.0
Replacement for faulty
(note the ring "around" Saturn!) 
(c) Gregory H. Revera, CC BY-SA 3.0
Full Moon photograph taken 10-22-2010 from Madison, Alabama, USA. Photographed with a Celestron 9.25 Schmidt-Cassegrain telescope. Acquired with a Canon EOS Rebel T1i (EOS 500D), 20 images stacked to reduce noise. 200 ISO 1/640 sec.
Författare/Upphovsman: User:Silvercat, Licens: CC BY-SA 3.0
The Location of Oceanus Procellarum, One of the Lunar Geographical Features.
This is a cropped version of NASA image PIA00077. This picture of the Moon was taken by the Galileo spacecraft at 6:47 p.m. PST Dec.8, 1990 from a distance of almost 220,000 miles. It shows the dark Oceanus Procellarum in the upper center, with Mare Imbrium above it and the smaller circular Mare Humorum below. The Orientale Basin, with a small mare in its center, is on the lower left near the limb or edge. Between stretches the cratered highland terrain, with scattered bright young craters on highlands and maria alike.
October 1, 2014
RELEASE 14-236 NASA Mission Points to Origin of “Ocean of Storms” on Earth’s Moon
http://www.nasa.gov/jpl/grail/pia18821
Earth's moon as observed in visible light (left), topography (center, where red is high and blue is low), and the GRAIL gravity gradients (right). The Procellarum region is a broad region of low topography covered in dark mare basalt. The gravity gradients reveal a giant rectangular pattern of structures surrounding the region.
TEXT Using data from NASA’s Gravity Recovery and Interior Laboratory (GRAIL), mission scientists have solved a lunar mystery almost as old as the moon itself.
Early theories suggested the craggy outline of a region of the moon’s surface known as Oceanus Procellarum, or the Ocean of Storms, was caused by an asteroid impact. If this theory had been correct, the basin it formed would be the largest asteroid impact basin on the moon. However, mission scientists studying GRAIL data believe they have found evidence the craggy outline of this rectangular region -- roughly 1,600 miles (2,600 kilometers) across -- is actually the result of the formation of ancient rift valleys.
"The nearside of the moon has been studied for centuries, and yet continues to offer up surprises for scientists with the right tools," said Maria Zuber, principal investigator of NASA's GRAIL mission, from the Massachusetts Institute of Technology, Cambridge. "We interpret the gravity anomalies discovered by GRAIL as part of the lunar magma plumbing system -- the conduits that fed lava to the surface during ancient volcanic eruptions."
The surface of the moon’s nearside is dominated by a unique area called the Procellarum region, characterized by low elevations, unique composition, and numerous ancient volcanic plains.
The rifts are buried beneath dark volcanic plains on the nearside of the moon and have been detected only in the gravity data provided by GRAIL. The lava-flooded rift valleys are unlike anything found anywhere else on the moon and may at one time have resembled rift zones on Earth, Mars and Venus. The findings are published online in the journal Nature.
Another theory arising from recent data analysis suggests this region formed as a result of churning deep in the interior of the moon that led to a high concentration of heat-producing radioactive elements in the crust and mantle of this region. Scientists studied the gradients in gravity data from GRAIL, which revealed a rectangular shape in resulting gravitational anomalies.
"The rectangular pattern of gravity anomalies was completely unexpected," said Jeff Andrews-Hanna, a GRAIL co-investigator at the Colorado School of Mines in Golden, Colorado, and lead author of the paper. "Using the gradients in the gravity data to reveal the rectangular pattern of anomalies, we can now clearly and completely see structures that were only hinted at by surface observations."
The rectangular pattern, with its angular corners and straight sides, contradicts the theory that Procellarum is an ancient impact basin, since such an impact would create a circular basin. Instead, the new research suggests processes beneath the moon’s surface dominated the evolution of this region.
Over time, the region would cool and contract, pulling away from its surroundings and creating fractures similar to the cracks that form in mud as it dries out, but on a much larger scale.
The study also noted a surprising similarity between the rectangular pattern of structures on the moon, and those surrounding the south polar region of Saturn’s icy moon Enceladus. Both patterns appear to be related to volcanic and tectonic processes operating on their respective worlds.
"Our gravity data are opening up a new chapter of lunar history, during which the moon was a more dynamic place than suggested by the cratered landscape that is visible to the naked eye," said Andrews-Hanna. "More work is needed to understand the cause of this newfound pattern of gravity anomalies, and the implications for the history of the moon."
Launched as GRAIL A and GRAIL B in September 2011, the probes, renamed Ebb and Flow, operated in a nearly circular orbit near the poles of the moon at an altitude of about 34 miles (55 kilometers) until their mission ended in December 2012. The distance between the twin probes changed slightly as they flew over areas of greater and lesser gravity caused by visible features, such as mountains and craters, and by masses hidden beneath the lunar surface.
The twin spacecraft flew in a nearly circular orbit until the end of the mission on Dec. 17, 2012, when the probes intentionally were sent into the moon’s surface. NASA later named the impact site in honor of late astronaut Sally K. Ride, who was America's first woman in space and a member of the GRAIL mission team.
GRAIL’s prime and extended science missions generated the highest resolution gravity field map of any celestial body. The map will provide a better understanding of how Earth and other rocky planets in the solar system formed and evolved.
The GRAIL mission was managed by NASA’s Jet Propulsion Laboratory (JPL) in Pasadena, California, for NASA's Science Mission Directorate in Washington. The mission was part of the Discovery Program managed at NASA's Marshall Space Flight Center in Huntsville, Alabama. GRAIL was built by Lockheed Martin Space Systems in Denver.
For more information about GRAIL, visit:
http://www.nasa.gov/grail
Transparent red circle
October 1, 2014
On the West Coast of the Ocean of Storms (Artist's Concept)
http://www.nasa.gov/jpl/grail/pia18821
A view of Earth's moon looking south across Oceanus Procellarum, representing how the western border structures may have looked while active. The gravity anomalies along the border structures are interpreted as ancient, solidified, lava-flooded rifts that are now buried beneath the surface of the dark volcanic plains, or maria, on the near side of the moon.
This artist's concept combines gravity gradients from NASA's Gravity Recovery and Interior Laboratory (GRAIL) mission, an image mosaic from the Lunar Reconnaissance Orbiter's (LRO) Wide Angle Camera, and topography data from LRO's Lunar Orbiter Laser Altimeter.
Launched as GRAIL A and GRAIL B in September 2011, the probes, renamed Ebb and Flow, operated in a nearly circular orbit near the poles of the moon at an altitude of about 34 miles (55 kilometers) until their mission ended in December 2012. The distance between the twin probes changed slightly as they flew over areas of greater and lesser gravity caused by visible features, such as mountains and craters, and by masses hidden beneath the lunar surface.
The twin spacecraft flew in a nearly circular orbit until the end of the mission on Dec. 17, 2012, when the probes intentionally were sent into the moon's surface. NASA later named the impact site in honor of late astronaut Sally K. Ride, who was America's first woman in space and a member of the GRAIL mission team.
GRAIL's prime and extended science missions generated the highest-resolution gravity field map of any celestial body. The map will provide a better understanding of how Earth and other rocky planets in the solar system formed and evolved.
The GRAIL mission was managed by NASA's Jet Propulsion Laboratory (JPL) in Pasadena, California, for NASA's Science Mission Directorate in Washington. The mission was part of the Discovery Program managed at NASA's Marshall Space Flight Center in Huntsville, Alabama. GRAIL was built by Lockheed Martin Space Systems in Denver.
For more information about GRAIL, please visit http://grail.nasa.gov.