Informace o publikaci

HD 34736: an intensely magnetised double-lined spectroscopic binary with rapidly rotating chemically peculiar B-type components

Autoři	SEMENKO E. KOCHUKHOV O. MIKULÁŠEK Zdeněk WADE G. A. ALECIAN E. BOHLENDER D. DAS B. FELIZ D. L. JANÍK Jan KOLÁŘ Jakub KRTIČKA Jiří KUDRYAVTSEV D. O. LABADIE-BARTZ J. M. MKRTICHIAN D. MONIN D. PETIT V. ROMANYUK I. I. SHULTZ M. E. SHULYAK D. SIVERD R. J. TKACHENKO A. YAKUNIN I. A. ZEJDA Miloslav
Rok publikování	2024
Druh	Článek v odborném periodiku
Časopis / Zdroj	Monthly Notices of the Royal Astronomical Society
Fakulta / Pracoviště MU	Přírodovědecká fakulta
Citace
www	https://academic.oup.com/mnras/article/535/3/2812/7881589
Doi	http://dx.doi.org/10.1093/mnras/stae2503
Klíčová slova	techniques: polarimetric; binaries: spectroscopic; stars: chemically peculiar; stars: magnetic fields
Popis	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 P-orb=83.(d)219(3) and e=0.8103(3). The primary component is a CP He-wk star with T-effA=13000 +/- 500 K and upsilon(e) sin i=75 +/- 3 km s(-1), while the secondary exhibits variability of Mg and Si lines, and has T-effB=11500 +/- 1000 K and upsilon(e)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 P-rotA=1.d2799885(11), which is lengthening at a rate of 1.26(6) s yr(-1). For the secondary, P-rotB=0.d5226938(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.