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Revealing the Binarity of HD 36030-One of the Hottest Flare Stars
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SYSNO ASEP 0572123 Document Type J - Journal Article R&D Document Type Journal Article Subsidiary J Článek ve WOS Title Revealing the Binarity of HD 36030-One of the Hottest Flare Stars Author(s) Maryeva, Olga (ASU-R) ORCID
Németh, Péter (ASU-R) ORCID
Karpov, Sergey (FZU-D) ORCID, RIDNumber of authors 3 Article number 55 Source Title Galaxies. - : MDPI
Roč. 11, č. 2 (2023)Number of pages 15 s. Publication form Online - E Language eng - English Country CH - Switzerland Keywords stars flares ; stars activity ; stars binaries spectroscopic Subject RIV BN - Astronomy, Celestial Mechanics, Astrophysics OECD category Astronomy (including astrophysics,space science) Subject RIV - cooperation Institute of Physics - Astronomy, Celestial Mechanics, Astrophysics R&D Projects EF15_003/0000437 GA MŠMT - Ministry of Education, Youth and Sports (MEYS) LM2018102 GA MŠMT - Ministry of Education, Youth and Sports (MEYS) GA22-34467S GA ČR - Czech Science Foundation (CSF) Research Infrastructure AUGER-CZ II - 90102 - Fyzikální ústav AV ČR, v. v. i. Method of publishing Open access Institutional support ASU-R - RVO:67985815 ; FZU-D - RVO:68378271 UT WOS 000976440400001 EID SCOPUS 85153706736 DOI 10.3390/galaxies11020055 Annotation The Kepler and TESS space missions significantly expanded our knowledge of what types of stars display flaring activity by recording a vast amount of super-flares from solar-like stars, as well as detecting flares from hotter stars of A-F spectral types. Currently, we know that flaring occurs in the stars as hot as B-type ones. However, the structures of atmospheres of hot B-A stars crucially differ from the ones of late types, and thus the occurrence of flaring in B-A type stars requires some extension of our theoretical views of flare formation and therefore a detailed study of individual objects. Here we present the results of our spectral and photometric study of HD 36030, which is a B9 V star with flares detected by the TESS satellite. The spectra we acquired suggest that the star is in a binary system with a low-mass secondary component, but the light curve lacks any signs of periodic variability related to orbital motion or surface magnetic fields. Because of that, we argue that the flares originate due to magnetic interaction between the components of the system. Workplace Astronomical Institute Contact Radka Svašková, bibl@asu.cas.cz, Tel.: 323 620 326 Year of Publishing 2024 Electronic address https://hdl.handle.net/11104/0342980
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