论文标题
在天狼星A的旋转速度上
On the rotational velocity of Sirius A
论文作者
论文摘要
为了获取与倾斜效应（SIN I）分离的Sirius A赤道旋转速度（V_E）的信息，对大量的光谱线进行了基于傅立叶变换技术的详细概况分析，同时明确地考虑了在centre-bimb beverity和Gravity dertive there there trot contive conteriontion coldiontion conteries conteriontion coldiestions conteriontion coldive conter的属性（均基于依赖于效应的效应），该效应依赖于该效果（该线路）。模拟表明，傅立叶变换幅度的1st零频率（Q_1）如何取决于V_E，从本质上取决于线之间的温度敏感性参数（k），而线之间的温度敏感性参数（k），而Fe I线（尤其是非常弱的线）对V_E比Fe II更敏感。通过比较许多Fe I和Fe II线的理论和观察到的Q_1值来得出以下结论：（1）Sirius A的投影旋转速度（VSINI）在16.3（+/- 0.1）km/s的确定相当良好地确定，要求Fe I和Fe I和Fe I和Fe I II线产生一致的结果。 （2）尽管V_E和I的精确分离很困难，但V_E得出的范围在16 <v_e <30-40 km/s的范围内，对应于25 <i（deg）<90。因此，Sirius A是本质上缓慢的旋转器，用于A-type星形，与其表面化学化学性质一致。
With an aim of getting information on the equatorial rotation velocity (v_e) of Sirius A separated from the inclination effect (sin i), a detailed profile analysis based on the Fourier transform technique was carried out for a large number of spectral lines, while explicitly taking into account the line-by-line differences in the centre-limb behaviours and the gravity darkening effect (which depend on the physical properties of each line) based on model calculations. The simulations showed that how the 1st-zero frequencies (q_1) of Fourier transform amplitudes depends on v_e is essentially determined by the temperature-sensitivity parameter (K) differing from line to line, and that Fe I lines (especially those of very weak ones) are more sensitive to v_e than Fe II lines. The following conclusions were drawn by comparing the theoretical and observed q_1 values for many Fe I and Fe II lines: (1) The projected rotational velocity (vsini) for Sirius A is fairly well established at 16.3 (+/-0.1) km/s by requiring that both Fe I and Fe II lines yield consistent results. (2) Although precise separation of v_e and i is difficult, v_e is concluded to be in the range of 16 < v_e < 30-40 km/s, which corresponds to 25 < i(deg) < 90. Accordingly, Sirius A is an intrinsically slow rotator for an A-type star, being consistent with its surface chemical peculiarity.
