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Short-term variations of surface magnetism and prominences of the young sun-like star V530 Per

Published online by Cambridge University Press:  16 August 2023

Cang Tianqi Open the ORCID record for Cang Tianqi [Opens in a new window] ,
Pascal Petit ,
Jean-François Donati  and
Colin Folsom
Cang Tianqi
Affiliation:
Department of Astronomy, Beijing Normal University, Xinjiekouwaidajie 19, 100875, Beijing, China Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, CNES, 31400 Toulouse, France
Pascal Petit
Affiliation:
Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, CNES, 31400 Toulouse, France
Jean-François Donati
Affiliation:
Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, CNES, 31400 Toulouse, France
Colin Folsom
Affiliation:
Institut de Recherche en Astrophysique et Planétologie, Université de Toulouse, CNRS, CNES, 31400 Toulouse, France Tartu Observatory, University of Tartu, Observatooriumi 1, Tõravere, 61602 Tartumaa, Estonia
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Abstract

V530 Per is a solar-like member of the young open cluster α Persei, with an ultra-short rotation period (P∼0.32d). We report on two spectropolarimetric campaigns using ESPaDOnS, aimed at characterizing the short-term variability of its magnetic activity and large-scale magnetic field. We used time-resolved spectropolarimetric observations obtained in 2006 and 2018 and reconstructed the brightness distribution and large-scale magnetic field geometry of V530 Per through Zeeman-Doppler imaging. Using the same data sets, we also mapped the spatial distribution of prominences through tomography of Hα emission. We reconstruct, at both epochs, a large, dark spot occupying the polar region of V530 Per while smaller (dark and bright) spots were reconstructed at lower latitudes. The maximal field strength reached ∼1 kG. The prominence pattern displayed a stable component that was confined close to the corotation radius. In 2018, we also observed rapidly evolving Hα emitting structures, over timescales ranging from minutes to days. The fast Hα evolution was not linked to any detected photospheric changes in the spot or magnetic coverage.

Keywords

stars: magnetic fieldsstars: chromospheresstars: individual (V530 Per)
Type
Poster Paper
Information
Proceedings of the International Astronomical Union , Volume 17 , Symposium S370: Winds of Stars and Exoplanets , August 2021 , pp. 89 - 90
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Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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