Properties of the Be-type stars in 30 Doradus

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY(2022)

引用 5|浏览12
暂无评分
摘要
The evolutionary status of Be-type stars remains unclear, with both single-star and binary pathways having been proposed. Here, VFI'S spectroscopy of 73 Be-type stars, in the spectral-type range, B0-B3, is analysed to estimate projected rotational velocities, radial velocities, and stellar parameters. They are found to be rotating faster than the corresponding VETS B-type sample but simulations imply that their projected rotational velocities are inconsistent with them all rotating at near critical velocities. The de-convolution of the projected rotational velocities estimates leads to a mean rotational velocity estimate of 320-350 km s(-1), approximately 100 km s(-1) larger than that for the corresponding B-type sample. There is a dearth of targets with rotational velocities less than 0.4 of the critical velocity, with a broad distribution reaching up to critical rotation. Our best estimate for the mean or median of the rotational velocity is 0.68 of the critical velocity. Rapidly rotating B-type stars are more numerous than their Be-type counterparts, whilst the observed frequency of Be-type stars identified as binary systems is significantly lower than that for normal B-type stars, consistent with their respective radial-velocity dispersions. The semi-amplitudes for the Be-type binaries are also smaller. Similar results are found for a Small Magellanic Cloud Be-type sample centred on NGC 346 with no significant differences being found between the two samples. These results are compared with the predictions of single and binary stellar evolutionary models for Be-type stars. Assuming that a single mechanism dominated the production of classical Be-type stars, our comparison would favour a binary evolutionary history.
更多
查看译文
关键词
stars: emission-line, Be, stars: rotation, Magellanic Clouds, galaxies: star clusters: individual: Tarantula Nebula
AI 理解论文
溯源树
样例
生成溯源树,研究论文发展脉络
Chat Paper
正在生成论文摘要