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dc.contributor.authorRab, Ch
dc.contributor.authorPadovani, M.
dc.contributor.authorGüdel, M.
dc.contributor.authorKamp, I.
dc.contributor.authorThi, W. -F.
dc.contributor.authorWoitke, P.
dc.contributor.editorElmegreen, Bruce G.
dc.contributor.editorTóth, L. Viktor
dc.contributor.editorGüdel, Manuel
dc.date.accessioned2020-07-12T23:35:48Z
dc.date.available2020-07-12T23:35:48Z
dc.date.issued2020-01-13
dc.identifier.citationRab , C , Padovani , M , Güdel , M , Kamp , I , Thi , W -F & Woitke , P 2020 , Constraining the stellar energetic particle flux in young solar-like stars . in B G Elmegreen , L V Tóth & M Güdel (eds) , Origins : From the Protosun to the First Steps of Life . Proceedings of the International Astronomical Union , no. S345 , vol. 14 , International Astronomical Union (IAU) , pp. 310-311 , IAU Symposium 345 , Vienna , Austria , 20/08/18 . https://doi.org/10.1017/S174392131900156Xen
dc.identifier.citationconferenceen
dc.identifier.issn1743-9213
dc.identifier.otherPURE: 258237548
dc.identifier.otherPURE UUID: 3d4a2d0a-0b46-45e7-91ee-9f72327642ba
dc.identifier.otherArXiv: http://arxiv.org/abs/1902.00914v1
dc.identifier.otherScopus: 85078013440
dc.identifier.urihttp://hdl.handle.net/10023/20235
dc.description.abstractAnomalies in the abundance measurements of short lived radionuclides in meteorites indicate that the protosolar nebulae was irradiated by a large number of energetic particles (E >∼10 MeV), often called solar cosmic rays. The particle flux of the contemporary Sun cannot explain these anomalies, but, similar to T Tauri stars, the young Sun was more active and probably produced enough high energy particles. However, the stellar particle (SP) flux of young stars is essentially unknown. We model the impact of high-energy ionization sources on the chemistry of the circumstellar environment (disks and envelopes). The model includes X-ray radiative transfer and makes use of particle transport models to calculate the individual molecular hydrogen ionization rates. We study the impact on the chemistry via the ionization tracers HCO+ and N2H+. We argue that spatially resolved observations of those molecules combined with detailed models allow for disentangling the contribution of the individual high-energy ionization sources and to put constraints on the SP flux in young stars.
dc.language.isoeng
dc.publisherInternational Astronomical Union (IAU)
dc.relation.ispartofOriginsen
dc.relation.ispartofseriesProceedings of the International Astronomical Unionen
dc.rightsCopyright © 2020 International Astronomical Union. This work has been made available online in accordance with publisher policies or with permission. Permission for further reuse of this content should be sought from the publisher or the rights holder. This is the author created accepted manuscript following peer review and may differ slightly from the final published version. The final published version of this work is available at https://doi.org/10.1017/S174392131900156Xen
dc.subjectStars: pre-main-sequenceen
dc.subject(Stars:) circumstellar matteren
dc.subjectStars: activityen
dc.subjectAstrochemistryen
dc.subjectRadiative transferen
dc.subjectMethods: numericalen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subjectQD Chemistryen
dc.subjectT-NDASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.subject.lccQDen
dc.titleConstraining the stellar energetic particle flux in young solar-like starsen
dc.typeConference itemen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.contributor.institutionUniversity of St Andrews.St Andrews Centre for Exoplanet Scienceen
dc.identifier.doihttps://doi.org/10.1017/S174392131900156X
dc.date.embargoedUntil2020-07-13


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