Trajectories of coronal mass ejection from solar-type stars

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dc.contributor.authorMenezes F.
dc.contributor.authorValio A.
dc.contributor.authorNetto Y.
dc.contributor.authorAraujo A.
dc.contributor.authorKay C.
dc.contributor.authorOpher M.
dc.date.accessioned2024-03-12T19:09:14Z
dc.date.available2024-03-12T19:09:14Z
dc.date.issued2023
dc.description.abstract© 2023 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.The Sun and other solar-type stars have magnetic fields that permeate their interior and surface, extend through the interplanetary medium, and are the main drivers of stellar activity. Stellar magnetic activity affects the physical processes and conditions of the interplanetary medium and orbiting planets. Coronal mass ejections (CMEs) are the most impactful of these phenomena in near-Earth space weather and consist of plasma clouds with a magnetic field, ejected from the solar corona. Precisely predicting the trajectory of CMEs is crucial in determining whether a CME will hit a planet and impact its magnetosphere and atmosphere. Despite the rapid developments in the search for stellar CMEs, their detection is still very incipient. In this work, we aim to better understand the propagation of CMEs by analysing the influence of initial parameters on CME trajectories, such as position, velocities, and the stellar magnetic field's configuration. We reconstruct magnetograms for Kepler-63 (KIC 11554435) and Kepler-411 (KIC 11551692) from spot transit mapping, and use a CME deflection model, ForeCAT, to simulate trajectories of hypothetical CMEs launched into the interplanetary medium from Kepler-63 and Kepler-411. We apply the same methodology to the Sun, for comparison. Our results show that in general deflections and rotations of CMEs decrease with their radial velocity and increase with ejection latitude. Moreover, magnetic fields stronger than the Sun's, such as Kepler-63's, tend to cause greater CME deflections.
dc.description.firstpage4392
dc.description.issuenumber3
dc.description.lastpage4403
dc.description.volume522
dc.identifier.doi10.1093/mnras/stad1078
dc.identifier.issn1365-2966
dc.identifier.urihttps://dspace.mackenzie.br/handle/10899/34058
dc.relation.ispartofMonthly Notices of the Royal Astronomical Society
dc.rightsAcesso Restrito
dc.subject.otherlanguageplanet-star interactions
dc.subject.otherlanguagestars: activity
dc.subject.otherlanguagestars: magnetic fields
dc.subject.otherlanguagestars: solar-type
dc.subject.otherlanguagestarspots
dc.subject.otherlanguageSun: coronal mass ejections (CMEs)
dc.titleTrajectories of coronal mass ejection from solar-type stars
dc.typeArtigo
local.scopus.citations3
local.scopus.eid2-s2.0-85159859552
local.scopus.subjectCoronal mass ejection
local.scopus.subjectInterplanetary medium
local.scopus.subjectMagnetic-field
local.scopus.subjectPlanet-star interactions
local.scopus.subjectStar: activity
local.scopus.subjectStars: magnetic field
local.scopus.subjectStars: solar types
local.scopus.subjectStarspots
local.scopus.subjectSun: coronal mass ejection
local.scopus.updated2025-04-01
local.scopus.urlhttps://www.scopus.com/inward/record.uri?partnerID=HzOxMe3b&scp=85159859552&origin=inward
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