Simulating stellar coronal rain and slingshot prominences
Simon Daley-Yates, Moira Jardine

TL;DR
This study uses numerical simulations to explore how stellar rotation influences the formation of coronal rain and slingshot prominences, revealing distinct behaviors and mass-loss components in different rotational regimes.
Contribution
It introduces a detailed simulation framework that distinguishes between slow and fast stellar rotation effects on coronal condensations and prominence formation.
Findings
Condensations form below the co-rotation radius in slow rotators.
Fast rotators develop slingshot prominences and periodic ejections.
Cold gas constitutes about 51% of the coronal mass in fast rotators.
Abstract
We have numerically demonstrated that simulated cool star coronae naturally form condensations. If the star rotates slowly, with a co-rotation radius greater than the Alfv\'{e}n radius (i.e. ), these condensations will form below the co-rotation radius and simply fall back to the stellar surface as coronal rain. If, however, the star is more rapidly rotating, (), not only rain will form but also ``slingshot prominences''. In this case, condensations collect into a large mass reservoir around the co-rotation radius, from which periodic centrifugal ejections occur. In this case, some of the coronal mass is cold gas, either in rain or prominences. We find that 21\% of the mass lost by our simulated fast rotating star is cold gas. Studies of stellar mass-loss from the hot wind do not consider this…
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