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The first Doppler imaging of the active binary prototype RS Canum Venaticorum
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dc.contributor.author | Xiang, Yue | |
dc.contributor.author | Gu, Shenghong | |
dc.contributor.author | Wolter, U. | |
dc.contributor.author | Schmitt, J. H. M. M. | |
dc.contributor.author | Cameron, A. Collier | |
dc.contributor.author | Barnes, J. R. | |
dc.contributor.author | Mittag, M. | |
dc.contributor.author | Perdelwitz, V. | |
dc.contributor.author | Kohl, S. | |
dc.date.accessioned | 2020-02-20T10:30:02Z | |
dc.date.available | 2020-02-20T10:30:02Z | |
dc.date.issued | 2020-03 | |
dc.identifier | 266449512 | |
dc.identifier | f4beb025-033b-45ee-8427-fd56e9c4cce4 | |
dc.identifier | 85084546694 | |
dc.identifier | 000518143200041 | |
dc.identifier.citation | Xiang , Y , Gu , S , Wolter , U , Schmitt , J H M M , Cameron , A C , Barnes , J R , Mittag , M , Perdelwitz , V & Kohl , S 2020 , ' The first Doppler imaging of the active binary prototype RS Canum Venaticorum ' , Monthly Notices of the Royal Astronomical Society , vol. 492 , no. 3 , pp. 3647-3656 . https://doi.org/10.1093/mnras/staa063 | en |
dc.identifier.issn | 0035-8711 | |
dc.identifier.other | BibCode: 2020MNRAS.492.3647X | |
dc.identifier.other | ORCID: /0000-0002-8863-7828/work/69463202 | |
dc.identifier.uri | https://hdl.handle.net/10023/19501 | |
dc.description.abstract | We present the first Doppler images of the prototypical active binarystar RS Canum Venaticorum, derived from high-resolution spectra observedin 2004, 2016 and 2017, using three different telescopes and observingsites. We apply the least-squares deconvolution technique to allobserved spectra to obtain high signal-to-noise line profiles, which areused to derive the surface images of the active K-type component. Ourimages show a complex spot pattern on the K star, distributed widely inlongitude. All star-spots revealed by our Doppler images are locatedbelow a latitude of about 70°. In accordance with previouslight-curve modelling studies, we find no indication of a polar spot onthe K star. Using Doppler images derived from two consecutive rotationalcycles, we estimate a surface differential rotation rate ofΔΩ = -0.039 ± 0.003 rad d-1 and α =ΔΩ/Ωeq = -0.030 ± 0.002 for the Kstar. Given the limited phase coverage during those two rotations, theuncertainty of our differential rotation estimate is presumably higher. | |
dc.format.extent | 10 | |
dc.format.extent | 1568763 | |
dc.language.iso | eng | |
dc.relation.ispartof | Monthly Notices of the Royal Astronomical Society | en |
dc.subject | Stars: activity | en |
dc.subject | Stars: binaries: eclipsing | en |
dc.subject | Stars: imaging | en |
dc.subject | Stars: star-spots | en |
dc.subject | Stars: individual: RS CVn | en |
dc.subject | QB Astronomy | en |
dc.subject | QC Physics | en |
dc.subject | DAS | en |
dc.subject.lcc | QB | en |
dc.subject.lcc | QC | en |
dc.title | The first Doppler imaging of the active binary prototype RS Canum Venaticorum | en |
dc.type | Journal article | en |
dc.contributor.institution | University of St Andrews. St Andrews Centre for Exoplanet Science | en |
dc.contributor.institution | University of St Andrews. School of Physics and Astronomy | en |
dc.identifier.doi | https://doi.org/10.1093/mnras/staa063 | |
dc.description.status | Peer reviewed | en |
dc.identifier.url | http://adsabs.harvard.edu/abs/2020MNRAS.492.3647X | en |
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