Surface feature1

Surface feature1 - Surface features Titania's surface is...

Info iconThis preview shows pages 1–2. Sign up to view the full content.

View Full Document Right Arrow Icon
Surface features Titania's surface is intersected by a system of enormous faults , or scarps. In some places, two parallel scarps mark depressions in the satellite's crust, [6] forming grabens , which are sometimes called canyons. [29] The most prominent among Titania's canyons is Messina Chasma , which runs for about 1500 km from the equator almost to the south pole. [27] The grabens on Titania are 20– 50 km wide and have a relief of about 2–5 km. [6] The scarps that are not related to canyons are called rupes, such as Rousillon Rupes near Ursula crater. [27] The regions along some scarps and near Ursula appear smooth at Voyager 's image resolution. These smooth plains were probably resurfaced later in Titania's geological history, after the majority of craters formed. The resurfacing may have been either endogenic in nature, involving the eruption of fluid material from the interior ( cryovolcanism ), or, alternatively it may be due to blanking by the impact ejecta from nearby large craters. [25]
Background image of page 1

Info iconThis preview has intentionally blurred sections. Sign up to view the full version.

View Full DocumentRight Arrow Icon
Image of page 2
This is the end of the preview. Sign up to access the rest of the document.

Page1 / 3

Surface feature1 - Surface features Titania's surface is...

This preview shows document pages 1 - 2. Sign up to view the full document.

View Full Document Right Arrow Icon
Ask a homework question - tutors are online