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dc.contributor.authorBemporad, Alessandro
dc.contributor.authorPagano, Paolo
dc.contributor.authorGiordano, Silvio
dc.contributor.authorFineschi, Silvano
dc.identifier.citationBemporad , A , Pagano , P , Giordano , S & Fineschi , S 2017 , ' Constraining the pass-band of future space-based coronagraphs for observations of solar eruptions in the FeXIV 530.3 nm “green line” ' , Experimental Astronomy , vol. 44 , no. 1 , pp. 83-96 .
dc.identifier.otherPURE: 250365204
dc.identifier.otherPURE UUID: 91aae5df-2826-4d69-bfea-335a5eac5f7c
dc.identifier.otherScopus: 85020554226
dc.identifier.otherWOS: 000412076500004
dc.descriptionThis research has received funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No 647214) and from the UK Science and Technology Facilities Council.en
dc.description.abstractObservations of the solar corona in the FeXIV 530.3 nm “green line” have been very important in the past, and are planned for future coronagraphs on-board forthcoming space missions such as PROBA-3 and Aditya. For these instruments, a very important parameter to be optimized is the spectral width of the band-pass filter to be centred over the “green line”. Focusing on solar eruptions, motions occurring along the line of sight will Doppler shift the line profiles producing an emission that will partially fall out of the narrower pass-band, while broader pass-band will provide observations with reduced spectral purity. To address these issues, we performed numerical (MHD) simulation of CME emission in the “green line” and produced synthetic images assuming 4 different widths of the pass-band (Δλ = 20 Å, 10 Å, 5 Å, and 2 Å). It turns out that, as expected, during solar eruptions a significant fraction of “green line” emission will be lost using narrower filters; on the other hand these images will have a higher spectral purity and will contain emission coming from parcels of plasma expanding only along the plane of the sky. This will provide a better definition of single filamentary features and will help isolating single slices of plasma through the eruption, thus reducing the problem of superposition of different features along the line of sight and helping physical interpretation of limb events. For these reasons, we suggest to use narrower band passes (Δλ ≤ 2 Å) for the observations of solar eruptions with future coronagraphs.
dc.relation.ispartofExperimental Astronomyen
dc.rights© Springer Science+Business Media Dordrecht 2017. This work has been made available online in accordance with the publisher’s policies. This is the author created accepted version manuscript following peer review and as such may differ slightly from the final published version. The final published version of this work is available at:
dc.subjectInstrumentation: coronagraphsen
dc.subjectMethods: numericalen
dc.subjectSun: coronaen
dc.subjectSun: coronal mass ejectionsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectSpace and Planetary Scienceen
dc.subjectAstronomy and Astrophysicsen
dc.titleConstraining the pass-band of future space-based coronagraphs for observations of solar eruptions in the FeXIV 530.3 nm “green line”en
dc.typeJournal articleen
dc.contributor.institutionUniversity of St Andrews.School of Mathematics and Statisticsen
dc.contributor.institutionUniversity of St Andrews.Applied Mathematicsen
dc.description.statusPeer revieweden

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