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dc.contributor.authorDaley-Yates, Simon
dc.contributor.authorJardine, Moira M
dc.contributor.authorJohnston, Craig D
dc.identifier.citationDaley-Yates , S , Jardine , M M & Johnston , C D 2023 , ' Heating and cooling in stellar coronae: coronal rain on a young Sun ' , Monthly Notices of the Royal Astronomical Society , vol. 526 , no. 2 , pp. 1646-1656 .
dc.identifier.otherRIS: urn:AA084449044E2DE59B4C2D6BA945E029
dc.identifier.otherORCID: /0000-0002-1466-5236/work/143917983
dc.descriptionFunding: SD-Y and MJ acknowledge support from STFC consolidated grant number ST/R000824/1. This work was performed using the DiRAC Data Intensive service at Leicester, operated by the University of Leicester IT Services, which forms part of the STFC DiRAC HPC Facility ( The equipment was funded by BEIS capital funding via STFC capital grants ST/K000373/1 and ST/R002363/1 and STFC DiRAC Operations grant ST/R001014/1. DiRAC is part of the National e-Infrastructure. CDJ acknowledges support from the NASA GSFC Internal Scientist Funding Model (competitive work package) programme.en
dc.description.abstractRecent observations of rapidly rotating cool dwarfs have revealed H α line asymmetries indicative of clumps of cool, dense plasma in the stars’ coronae. These clumps may be either long-lived (persisting for more than one stellar rotation) or dynamic. The fastest dynamic features show velocities greater than the escape speed, suggesting that they may be centrifugally ejected from the star, contributing to the stellar angular momentum loss. Many, however, show lower velocities, similar to coronal rain observed on the Sun. We present 2.5D magnetohydrodynamic simulations of the formation and dynamics of these condensations in a rapidly rotating (Prot = 1 d) young Sun. Formation is triggered by excess surface heating. This pushes the system out of thermal equilibrium and triggers a thermal instability. The resulting condensations fall back towards the surface. They exhibit quasi-periodic behaviour, with periods longer than typical periods for solar coronal rain. We find line-of-sight velocities for these clumps in the range of 50 km s−1 (blueshifted) to 250 km s−1 (redshifted). These are typical of those inferred from stellar H α line asymmetries, but the inferred clump masses of 3.6 × 1014 g are significantly smaller. We find that a maximum of ${\simeq}3~{{ \rm per\ cent}}$ of the coronal mass is cool clumps. We conclude that coronal rain may be common in solar-like stars, but may appear on much larger scales in rapid rotators.
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.subjectSun: filamentsen
dc.subjectStars: activityen
dc.subjectStars: coronaeen
dc.subjectStars: magnetic fieldsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.titleHeating and cooling in stellar coronae: coronal rain on a young Sunen
dc.typeJournal articleen
dc.contributor.sponsorScience & Technology Facilities Councilen
dc.contributor.institutionUniversity of St Andrews. School of Physics and Astronomyen
dc.description.statusPeer revieweden

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