来自SDSS和SPY的亚矮星O
Subdwarf O Stars from SDSS and SPY
摘要：
我们提出的SDSS数据库中的sdOs的定量光谱分析的结果。拟合的Balmer，HeI和HeII线的非LTE模型的光谱，我们推导出它们的有效温度，表面重力和氦丰度。我们发现富氦的sdO星在Teff = 40，000K到50，000K和log（g）= 5.5到6.0的小区间内聚集。我们的结论是，sdB星与缺氦sdO星联系在一起，即sdB星是缺氦sdO星的前身。为了完整地解释氦富集的sdO星，我们认为两种情况最有希望：两颗氦核白矮星的合并和后期的热闪光。
英文摘要：
We present the results of quantitative spectral analysis of sdOs from the SDSS database. Fitting the Balmer, HeI and HeII lines to non-LTE model spectra, we derived their effective temperatures, surface gravities and helium abundances. We find the helium-enriched sdO stars to rally in a small intervall of Teff = 40,000K to 50,000K and log(g) = 5.5 to 6.0. We conclude, that the sdB stars are linked with the helium-deficient sdO stars, i.e. the sdBs are predecessors for the helium-deficient sdOs. To explain the helium-enriched sdO stars in their entirety, we regard two scenarios as most promising: The merging of two helium-core white dwarfs and the late hot flashers.
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