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Although the present-day Sun rotates too slowly to exhibitcentrifugally-supported 'slingshot prominences', at some time during its pastit may have formed these clouds of cool gas and ejected them into theinterplanetary medium. We determine the time period for this behaviour by usinga rotation evolution code to derive the properties of the formation andejection of slingshot prominences during the lifetime of a star similar to ourSun. The mass, mass loss rate and rate of ejection of these prominences arecalculated using the analytical expression derived in our previous work. Wefind that for stars with an initial rotation rate larger than $4.6\,\Omega_\odot$, about half of all solar mass stars, slingshot prominences willbe present even after the star reaches the main sequence phase. In a fastrotator, this means that prominences can form until the star reaches $\sim 800$Myr old. Our results also indicate that the mass and lifetime of this type ofprominence have maximum values when the star reaches the ZAMS at an age of$\sim 40$ Myr for a solar mass star.

Slingshot prominence evolution for a solar-like star