TY - JOUR

T1 - Magnetic field and radial velocities of the star Chi Draconis A

AU - Lee, Byeong Cheol

AU - Gadelshin, D.

AU - Han, Inwoo

AU - Kang, Dong Il

AU - Kim, Kang Min

AU - Valyavin, G.

AU - Galazutdinov, G.

AU - Jeong, Gwanghui

AU - Beskrovnaya, N.

AU - Burlakova, T.

AU - Grauzhanina, A.

AU - Ikhsanov, N. R.

AU - Kholtygin, A. F.

AU - Valeev, A.

AU - Bychkov, V.

AU - Park, Myeong Gu

PY - 2018/1/1

Y1 - 2018/1/1

N2 - We present high-resolution spectropolarimetric observations of the spectroscopic binary χ Dra. Spectral lines in the spectrum of the main component χ DraA show variable Zeeman displacement, which confirms earlier suggestions about the presence of a weak magnetic field on the surface of this star. Within about 2 yr of time base of our observations, the longitudinal component BL of the magnetic field exhibits variation from -11.5 ± 2.5 to +11.1 ± 2.1G with a period of about 23 d. Considering the rotational velocity of χ Dra A in the literature and that newly measured in this work, this variability may be explained by the stellar rotation under the assumption that the magnetic field is globally stable. Our new measurements of the radial velocities (RV) in high-resolution I-spectra of χ DraA refined the orbital parameters and reveal persistent deviations of RVs from the orbital curve.We suspect that these deviations may be due to the influence of local magnetically generated spots, pulsations, or a Jupiter-size planet orbiting the system.

AB - We present high-resolution spectropolarimetric observations of the spectroscopic binary χ Dra. Spectral lines in the spectrum of the main component χ DraA show variable Zeeman displacement, which confirms earlier suggestions about the presence of a weak magnetic field on the surface of this star. Within about 2 yr of time base of our observations, the longitudinal component BL of the magnetic field exhibits variation from -11.5 ± 2.5 to +11.1 ± 2.1G with a period of about 23 d. Considering the rotational velocity of χ Dra A in the literature and that newly measured in this work, this variability may be explained by the stellar rotation under the assumption that the magnetic field is globally stable. Our new measurements of the radial velocities (RV) in high-resolution I-spectra of χ DraA refined the orbital parameters and reveal persistent deviations of RVs from the orbital curve.We suspect that these deviations may be due to the influence of local magnetically generated spots, pulsations, or a Jupiter-size planet orbiting the system.

KW - Binaries

KW - Individual

KW - Magnetic field

KW - Stars

KW - χ Dra

UR - http://www.scopus.com/inward/record.url?scp=85044414393&partnerID=8YFLogxK

M3 - Article

AN - SCOPUS:85044414393

VL - 473

SP - L41-L45

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 1

ER -