再探A型金属线恒星飞马座ο的表面磁场
Surface magnetic field of the A-type metallic-line star omicron Pegasi revisited
AI总结：
本研究针对早期A型金属线恒星飞马座ο表面磁场研究的经验性与数据不足问题，通过严谨的谱线流量模拟结合高质量光谱的Fe谱线参数分析，证实其平均磁场约为1-2kG，与既往结果基本一致。
摘要：
20世纪90年代初，研究人员通过分析谱线的宽度和强度，报道了明亮的A型金属线恒星飞马座ο（o Peg）具有约2kG的表面磁场。鉴于这些早期研究具有相当强的经验性或近似性，且观测数据质量不足，本研究基于物理上更严谨的谱线流量轮廓模拟，结合从高质量光谱中测量得到的198条Fe I和182条Fe II谱线的观测等值宽度（W）和半峰全宽（h），对该问题进行了重新研究。在通过常规分析得到铁丰度的前提下，将针对多组参数计算的理论W和h值与观测值进行了比较，从而得出关于<H>（平均磁场强度）的以下结论：（1）对W的分析显示，在微湍流速度vt~1.5km/s的条件下，Fe II谱线给出的<H>约为1-1.5kG。（2）对h的比较结果表明，<H>约为1.5-2kG，同时得到投影自转速度vsini约为5km/s。（3）据此，本研究证实了飞马座ο中存在量级为<H>~1-2kG的平均磁场，这与之前工作的结果几乎一致。
英文摘要：
The bright A-type metallic-line star o Peg was reported in the early 1990s to have a surface magnetic field of ~2kG by analyzing the widths and strengths of spectral lines. In respect that those old studies were of rather empirical or approximate nature and the quality of observational data was not sufficient, this problem has been newly reinvestigated based on physically more rigorous simulations of line flux profiles, along with the observed equivalent widths (W) and full-widths at half-maximum (h) of 198 Fe I and 182 Fe II lines measured from the high-quality spectra. Given the Fe abundance derived from the conventional analysis, theoretical W and h values calculated for various sets of parameters were compared with the observed ones, which lead to the following conclusion regarding <H> (mean field strength). (1) An analysis of W yielded <H>~1-1.5kG from Fe II lines with the microturbulence of vt~1.5km/s. (2) A comparison of h resulted in <H>~1.5-2kG as well as the projected rotational velocity of vsini~5km/s. (3) Accordingly, the existence of mean magnetic field on the order of <H>~1-2kG in o Peg was confirmed, which is almost consistent with the consequence of the previous work.
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