# Slingshot prominence evolution for a solar-like star

## TL;DR

This study models the evolution of slingshot prominences in solar-like stars, showing they can form and eject cool gas clouds for hundreds of millions of years, especially in faster rotators, influencing stellar and planetary environments.

## Contribution

It provides a detailed analysis of the formation, ejection, and lifespan of slingshot prominences in stars similar to the Sun, based on rotation evolution modeling.

## Key findings

- Prominences form in stars with initial rotation rates >4.6 Ω⊙.
- Prominences can persist until stars are about 800 Myr old.
- Maximum prominence mass and lifetime occur at ~40 Myr age.

## Abstract

Although the present-day Sun rotates too slowly to exhibit centrifugally-supported 'slingshot prominences', at some time during its past it may have formed these clouds of cool gas and ejected them into the interplanetary medium. We determine the time period for this behaviour by using a rotation evolution code to derive the properties of the formation and ejection of slingshot prominences during the lifetime of a star similar to our Sun. The mass, mass loss rate and rate of ejection of these prominences are calculated using the analytical expression derived in our previous work. We find that for stars with an initial rotation rate larger than $4.6\, \Omega_\odot$, about half of all solar mass stars, slingshot prominences will be present even after the star reaches the main sequence phase. In a fast rotator, 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 of prominence have maximum values when the star reaches the ZAMS at an age of $\sim 40$ Myr for a solar mass star.