论文标题
太阳光谱和太阳型星的线条不对称
Asymmetry of Lines in the Spectra of the Sun and Solar-Type Stars
论文作者
论文摘要
我们使用竖琴光谱仪上的观察数据，使用三个FTS地图集和竖琴图地图集和13颗恒星的光谱中分析了太阳通量光谱中Fe I和Fe II的不对称性。为了减少观察噪声，每个恒星的单个双线都有平均。恒星光谱中获得的平均双分式与太阳众所周知的形状C或多或少相似。在旋转速度大于5 km /s的恒星中，双层的形状更像是 /。双压的曲率和跨度随恒星的温度而增加。我们的结果证实了有关旋转速度对双压跨度和形状的强大影响的已知事实。平均对流速度是基于平均分配器的跨度确定的，这表明冷落的速度与对流的热量流动的速度之间的差异最大。作为恒星，太阳等于-420 m/s。在太阳能型星中，它的有效温度分别为4800至6200 K，从-150增至-700 m/s。对于表面重力较大且金属性更大的恒星，平均对流速度降低。它还随着星年的年龄而降低，并且与微燃烧运动的速度相关。太阳通量分析的结果表明，FTS地图集中的绝对波长尺度使用的精度约为-10 m/s，除了Hinkle的地图集等，其尺度的变化并取决于波长。在450 nm到650 nm的范围内，该地图集的比例位移分别从-100到-330 m/s，平均等于-240 m/s。由此产生的平均恒星等分组包含有关对流速度场的信息，并且可能对恒星大气的流体动力建模有用，以研究表面对流的特征。
We have analysed the asymmetry of lines Fe I and Fe II in spectra of a solar flux using three FTS atlases and the HARPS atlas and also in spectra of 13 stars using observation data on the HARPS spectrograph. To reduce observation noise individual line bisectors of each star have been averaged. The obtained average bisectors in the stellar spectra are more or less similar to the shape C well known to the Sun. In stars with rotation speeds greater than 5 km/s the shape of the bisectors is more like /. The curvature and span of the bisectors increase with the temperature of the star. Our results confirm the known facts about strong influence of rotation velocity on the span and shape of bisectors. The average convective speed was determined based on the span of the average bisector, which shows the largest difference between the velocity of cold falling and hot rising convective flows of the matter. It's equal to -420 m/s for the Sun as a star. In solar-type stars, it grows from -150 to -700 m/s with an effective temperature of 4800 to 6200 K, respectively. For stars with greater surface gravity and greater metallicity, the average convective velocity decreases. It also decreases with star age and correlates with the speed of micro and macroturbulent movements. The results of solar flux analysis showed that absolute wavelength scales in the FTS atlases used coincide with an accuracy of about -10 m/s, except for the atlas of Hinkle, etc., whose scale is shifted and depends on the wavelength. In the range from 450 to 650 nm, the scale shift of this atlas varies from -100 to -330 m/s, respectively, and it equals on average of -240 m/s. The resulting average star bisectors contain information about the fields of convective velocities and may be useful for hydrodynamic modeling of stellar atmospheres in order to study the characteristic features of surface convection.
