Editing Mira (section)

====Mass loss====
Ultraviolet studies of Mira by [[NASA]]'s Galaxy Evolution Explorer ([[GALEX]]) space telescope have revealed that it sheds a trail of material from the outer envelope, leaving a tail 13 light-years in length, formed over tens of thousands of years.<ref name=martin/><ref name=minkel/> It is thought that a hot [[Bow shock|bow wave]] of compressed plasma/gas is the cause of the tail; the bow wave is a result of the interaction of the stellar wind from Mira A with gas in interstellar space, through which Mira is moving at an extremely high speed of {{Convert|130|km/s|mph|abbr=off}}.<ref name=wareing2007/> The tail consists of material stripped from the head of the bow wave, which is also visible in ultraviolet observations. Mira's bow shock will eventually evolve into a [[planetary nebula]], the form of which will be considerably affected by the motion through the [[interstellar medium]] (ISM).<ref name=wareing/> Mira’s tail offers a unique opportunity to study how stars like our sun die and ultimately seed new solar systems. As Mira hurls along, its tail drops off carbon, oxygen and other important elements needed for new stars, planets, and possibly even life to form. This tail material, visible now for the first time, has been shed over the past 30,000 years.

[[File:Mira the star-by Nasa alt crop.jpg|thumb|699px|center|Ultraviolet mosaic of Mira's bow shock and tail obtained using NASA's Galaxy Evolution Explorer ([[GALEX]])]]