Stellar mass ejections

Moira Jardine, Jean-Francois Donati, Scott G. Gregory

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Abstract

It has been known for some time now that rapidly-rotating solar-like stars possess the stellar equivalent of solar prominences. These may be three orders of magnitude more massive than their solar counterparts, and their ejection from the star may form a significant contribution to the loss of angular momentum and mass in the stellar wind. In addition, their number and distribution provide valuable clues as to the structure of the stellar corona and hence to the nature of magnetic activity in other stars.Until recently, these “slingshot prominences” had only been observed in mature stars, but their recent detection in an extremely young star suggests that they may be more widespread than previously thought. In this review we will summarise our current understanding of these stellar prominences, their ejection from their stars and their role in elucidating the (sometimes very non-solar) behaviour of stellar magnetic fields.
Original languageEnglish
Title of host publicationUniversal Heliophysical Processes
Subtitle of host publicationProceedings of the International Astronomical Union
EditorsN Gopalswamy, D Webb
PublisherCambridge University Press
Pages201-210
Number of pages10
Volume257
ISBN (Print)9780521889889
DOIs
Publication statusPublished - Mar 2009

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    Jardine, M., Donati, J-F., & Gregory, S. G. (2009). Stellar mass ejections. In N. Gopalswamy, & D. Webb (Eds.), Universal Heliophysical Processes: Proceedings of the International Astronomical Union (Vol. 257, pp. 201-210). Cambridge University Press. https://doi.org/10.1017/S1743921309029317