论文标题
快速旋转磁性早期B星HD的光度特性和恒星参数345439
Photometric properties and stellar parameters of the rapidly rotating magnetic early-B star HD 345439
论文作者
论文摘要
我们首先使用Nanshan一米宽场望远镜介绍快速旋转磁星HD 345439的多色光度法结果。从光度观测值中，我们得出0.7699 \ pm0.0014天的旋转周期。 HD 345439的光曲线由磁云引起的双重不对称S波特征主导。在过渡系外行星调查卫星的第41区未观察到脉动行为。尚未发现在残留通量中的离心突破事件发生，也没有发现光曲线极值的系统变化。基于刚性旋转磁层模型的假设，我们限制了磁性倾斜角{$β$}和旋转倾斜角$ i $ $ $，以便它们满足近似关系{$β+ i \ i \ of 105^{\ cource} $}。确定颜色过剩，灭绝和发光度为$ e _ {（b-v）} = 0.745 \ pm0.016 \，$ mag，$ a_ {v} = 2.31 \ pm0.05 \，$ mag，$，$ \ rm log \ rm log \，（l/l/l/l/l/l/l/l/l/l/此外，我们将有效温度得出为$ t $ \ rm _ {eff} = 22 \ pm1 $ kk，而表面重力为log $ g = 4.00 \ pm0.22 $。质量$ m = 7.24 _ { - 1.24}^{+1.75} \ rm m _ {\ odot} $，半径$ r = 4.44 _ { - 1.93}^{+2.68} {+2.68} \ rm rm rm r _ { τ_{age} = 23.62 \，_ { - 21.97}^{+4.24} $ myr是从Hertzsprung-Russell图中估算的
We first present the multicolor photometry results of the rapidly rotating magnetic star HD 345439 using the Nanshan One-meter Wide-field Telescope. From the photometric observations, we derive a rotational period of 0.7699\pm0.0014 day. The light curves of HD 345439 are dominated by the double asymmetric S-wave feature that arises from the magnetic clouds. Pulsating behaviors are not observed in Sector 41 of the Transiting Exoplanet Survey Satellite. No evidence is found of the occurrence of centrifugal breakout events neither in the residual flux nor in the systematic variations at the extremum of the light curve. Based on the hypothesis of the Rigidly Rotating Magnetosphere model, we restrict the magnetic obliquity angle {$β$} and the rotational inclination angle $i$ so that they satisfy the approximate relation {$β+ i \approx 105^{\circ}$}. The colour excess, extinction, and luminosity are determined to be $E_{(B-V)}=0.745\pm0.016\,$mag, $A_{V}=2.31\pm0.05\,$mag, and $\rm log\,(L/L_{\odot})=3.82\pm0.1 $dex, respectively. Furthermore, we derive the effective temperature as $T$$\rm _{eff}=22\pm1 $kK and the surface gravity as log$g=4.00\pm0.22$. The mass$ M=7.24_{-1.24}^{+1.75}\rm M_{\odot}$, radius$ R=4.44_{-1.93}^{+2.68}\rm R_{\odot}$, and age$\rm τ_{age}=23.62\,_{-21.97}^{+4.24} $Myr are estimated from the Hertzsprung--Russell Diagram
