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dc.contributor.authorMoschou, Sofia-Paraskevi
dc.contributor.authorDrake, Jeremy J.
dc.contributor.authorCohen, Ofer
dc.contributor.authorAlvarado-Gómez, Julián D.
dc.contributor.authorGarraffo, Cecilia
dc.contributor.authorFraschetti, Federico
dc.date.accessioned2019-10-02T17:43:42Z
dc.date.available2019-10-02T17:43:42Z
dc.date.issued2019-05-31
dc.identifier.citationSofia-Paraskevi Moschou et al 2019 ApJ 877 105en_US
dc.identifier.issn0004-637X
dc.identifier.doi10.3847/1538-4357/ab1b37
dc.identifier.urihttp://hdl.handle.net/10150/634642
dc.description.abstractSolar coronal mass ejections (CMEs) and flares have a statistically well-defined relationship, with more energetic X-ray flares corresponding to faster and more massive CMEs. How this relationship extends to more magnetically active stars is a subject of open research. Here we study the most probable stellar CME candidates associated with flares captured in the literature to date, all of which were observed on magnetically active stars. We use a simple CME model to derive masses and kinetic energies from observed quantities and transform associated flare data to the Geostationary Operational Environmental Satellite 1-8 angstrom band. Derived CME masses range from similar to 10(15) to 10(22) g. Associated flare X-ray energies range from 10(31) to 10(37) erg. Stellar CME masses as a function of associated flare energy generally lie along or below the extrapolated mean for solar events. In contrast, CME kinetic energies lie below the analogous solar extrapolation by roughly 2 orders of magnitude, indicating approximate parity between flare X-ray and CME kinetic energies. These results suggest that the CMEs associated with very energetic flares on active stars are more limited in terms of the ejecta velocity than the ejecta mass, possibly because of the restraining influence of strong overlying magnetic fields and stellar wind drag. Lower CME kinetic energies and velocities present a more optimistic scenario for the effects of CME impacts on exoplanets in close proximity to active stellar hosts.en_US
dc.description.sponsorshipNASA Living [NNX16AC11G]; NASA [NAS8-03060]; NASA Astrobiology Institute [NNX15AE05G]; Chandra [AR4-15000X, GO5-16021X]; SI Grand Challenges grant "Lessons from Mars: Are Habitable Atmospheres on Planets around M Dwarfs Viable?"en_US
dc.language.isoenen_US
dc.publisherIOP PUBLISHING LTDen_US
dc.rightsCopyright © 2019. The American Astronomical Society. All rights reserved.en_US
dc.subjectplanet-star interactionsen_US
dc.subjectstars: activityen_US
dc.subjectstars: flareen_US
dc.subjectstars: late-typeen_US
dc.subjectSun: coronal mass ejections (CMEs)en_US
dc.subjectX-rays: starsen_US
dc.titleThe Stellar CME–Flare Relation: What Do Historic Observations Reveal?en_US
dc.typeArticleen_US
dc.contributor.departmentUniv Arizona, Dept Planetary Sci, Lunar & Planetary Laben_US
dc.identifier.journalASTROPHYSICAL JOURNALen_US
dc.description.collectioninformationThis item from the UA Faculty Publications collection is made available by the University of Arizona with support from the University of Arizona Libraries. If you have questions, please contact us at repository@u.library.arizona.edu.en_US
dc.eprint.versionFinal published versionen_US
dc.source.volume877
dc.source.issue2
dc.source.beginpage105
refterms.dateFOA2019-10-02T17:43:42Z


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