Editing Oceanus Procellarum (section)

==Characteristics==
Like all lunar maria, Oceanus Procellarum was formed by ancient [[volcano|volcanic]] eruptions resulting in [[basalt]]ic floods that covered the region in a thick, nearly flat layer of solidified [[magma]]. Basalts in Oceanus Procellarum have been estimated to be as young as one billion years old.<ref>{{Cite web|last=Andrea Thompson 06 November 2008|title=Signs of Late Volcanism Seen on Moon|url=https://www.space.com/6071-signs-late-volcanism-moon.html|access-date=2021-05-07|website=Space.com|date=6 November 2008 |language=en}}</ref> Unlike the other lunar maria, however, Oceanus Procellarum may or may not be contained within a single, well-defined impact basin.

Around its edges lie many minor bays and seas, including [[Sinus Roris]] to the north, and [[Mare Nubium]], [[Mare Humorum]] and {{ill|Sinus Viscositatis|it}}<ref>{{cite web |title=Sinus Viscositatis |url=https://planetarynames.wr.usgs.gov/Feature/16118 |website=Planetary Names |publisher=[[US Geological Survey]] |access-date=January 6, 2024}}</ref> to the south. To the northeast, Oceanus Procellarum is separated from [[Mare Imbrium]] by the [[Montes Carpatus|Carpathian Mountains]]. On its north-west edge lies the 32&nbsp;km wide [[Aristarchus (crater)|Aristarchus ray crater]], the brightest feature on the Near side of the Moon.<ref>DK Space Encyclopedia: The Near Side of the Moon</ref> Also, the more-prominent ray-crater [[Copernicus (lunar crater)|Copernicus]] lies within the eastern edge of the mare, distinct with its bright ray materials sprawling over the darker material.<ref>{{Cite web|title=NASA – Copernicus|url=https://www.nasa.gov/mission_pages/LRO/multimedia/lroimages/lola-20100430-copernicus.html|access-date=2021-05-07|website=www.nasa.gov|language=en|archive-date=2021-12-14|archive-url=https://web.archive.org/web/20211214010757/https://www.nasa.gov/mission_pages/LRO/multimedia/lroimages/lola-20100430-copernicus.html|url-status=dead}}</ref>