| Download | - View final version: HD 34736: an intensely magnetised double-lined spectroscopic binary with rapidly rotating chemically peculiar B-type components (PDF, 5.2 MiB)
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| DOI | Resolve DOI: https://doi.org/10.1093/mnras/stae2503 |
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| Author | Search for: Semenko, EORCID identifier: https://orcid.org/0000-0002-1912-1342; Search for: Kochukhov, OORCID identifier: https://orcid.org/0000-0003-3061-4591; Search for: Mikulášek, Z; Search for: Wade, G A; Search for: Alecian, E; Search for: Bohlender, D1; Search for: Das, BORCID identifier: https://orcid.org/0000-0001-8704-1822; Search for: Feliz, D L; Search for: Janík, J; Search for: Kolář, J; Search for: Krtička, J; Search for: Kudryavtsev, D O; Search for: Labadie-Bartz, J MORCID identifier: https://orcid.org/0000-0002-2919-6786; Search for: Mkrtichian, DORCID identifier: https://orcid.org/0000-0001-5094-3910; Search for: Monin, D1; Search for: Petit, VORCID identifier: https://orcid.org/0000-0002-5633-7548; Search for: Romanyuk, I I; Search for: Shultz, M E; Search for: Shulyak, D; Search for: Siverd, R J; Search for: Tkachenko, A; Search for: Yakunin, I A; Search for: Zejda, M |
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| Affiliation | - National Research Council Canada. Herzberg Astronomy and Astrophysics
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| Format | Text, Article |
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| Subject | techniques: polarimetric; binaries: spectroscopic; stars: chemically peculiar; stars: magnetic fields |
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| Abstract | We report the results of a comprehensive study of the spectroscopic binary (SB2) system HD 34736 hosting two chemically peculiar (CP) late B-type stars. Using new and archival observational data, we characterize the system and its components, including their rotation and magnetic fields. Fitting of the radial velocities yields Porb = 83.ᵈ219(3) and e = 0.8103(3). The primary component is a CP He-wk star with TeffA = 13000 ± 500 K and υₑ sin i = 75 ± 3 km s⁻¹ , while the secondary exhibits variability of Mg and Si lines, and has TeffB = 11500 ± 1000 K and υₑ sin i = 110–180 km s⁻¹ . Transiting Exoplanet Survey Satellite and Kilodegree Extremely Little Telescope photometry reveal clear variability of the primary component with a rotational period ProtA = 1.ᵈ279 988 5(11), which is lengthening at a rate of 1.26(6) s yr⁻¹. For the secondary, ProtB = 0.ᵈ522 693 8(5), reducing at a rate of −0.14(3) s yr⁻¹. The longitudinal component <Bz> of the primary’s strongly asymmetric global magnetic field varies from −6 to +5 kG. Weak spectropolarimetric evidence of a magnetic field is found for the secondary star. The observed X-ray and radio emission of HD 34736 may equally be linked to a suspected T Tau-like companion or magnetospheric emission from the principal components. Given the presence of a possible third magnetically active body, one can propose that the magnetic characteristics of the protostellar environment may be connected to the formation of such systems. |
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| Publication date | 2024-11-06 |
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| Publisher | Oxford University Press |
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| Licence | |
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| In | |
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| Language | English |
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| Peer reviewed | Yes |
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| Export citation | Export as RIS |
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| Report a correction | Report a correction (opens in a new tab) |
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| Record identifier | 931c9015-ddd6-4592-ba0c-8f8f4abb6814 |
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| Record created | 2025-03-19 |
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| Record modified | 2025-03-19 |
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