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首页> 外文期刊>The Astrophysical journal >TESTING THE REALITY OF STRONG MAGNETIC FIELDS ON T TAURI STARS: THE NAKED T TAURI STAR HUBBLE 4
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TESTING THE REALITY OF STRONG MAGNETIC FIELDS ON T TAURI STARS: THE NAKED T TAURI STAR HUBBLE 4

机译：测试T陶里星上强磁场的真实性：裸T陶里星恒星4

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摘要

High-resolution optical and infrared (IR) echelle spectra of the naked (diskless) T Tauri star Hubble 4 are presented. The K-band IR spectra include four Zeeman-sensitive Ti I lines along with several magnetically insensitive CO lines. Detailed spectrum synthesis combined with modern atmospheric models is used to fit the optical spectra of Hubble 4 in order to determine its key stellar parameters: T_(eff) = 4158 ± 56 K; log g = 3.61 ± 0.50; [M/H] = -0.08 ± 0.05; v sin i = 14.6 ±1.7 km s~(-1). These stellar parameters are used to synthesize K-band spectra to compare with the observations. The magnetically sensitive Ti I lines are all significantly broadened relative to the lines produced in the nonmagnetic model, while the magnetically insensitive CO lines are well matched by the basic nonmagnetic model. Models with magnetic fields are synthesized and fitted to the Ti I lines. The best-fit models indicate a distribution of magnetic field strengths on the stellar surface characterized by a mean magnetic field strength of 2.51 ± 0.18 kG. The mean field is a factor of 2.0 greater than the maximum field strength predicted by pressure equipartition arguments. To confirm the reality of such strong fields, we attempt to refit the observed profiles using a two-component magnetic model in which the field strength is confined to the equipartition value representing plagelike regions in one component and the field is allowed to vary in a cooler component representing spots. It is shown that such a model is inconsistent with the optical spectrum of the TiO bandhead at 7055 A.
机译：提出了裸露的（无盘的）T Tauri星哈勃4号的高分辨率光学和红外（IR）阶梯光谱。 K波段红外光谱包括4条对塞曼敏感的Ti I谱线以及几条对磁不敏感的CO谱线。详细的光谱合成与现代大气模型相结合以拟合哈勃4的光谱，以确定其关键的恒星参数：T_（eff）= 4158±56 K； log g = 3.61±0.50; [M / H] = -0.08±0.05； v sin i = 14.6±1.7 km s〜（-1）。这些恒星参数用于合成K波段光谱以与观测值进行比较。相对于非磁性模型中产生的线，对磁敏感的Ti I线都显着加宽，而对磁性不敏感的CO线与基本的非磁性模型很好地匹配。合成具有磁场的模型并将其拟合到Ti I线。最佳拟合模型表明，恒星表面的磁场强度分布为2.51±0.18 kG的平均磁场强度。平均场比压力均分参数预测的最大场强大2.0倍。为了确认这种强磁场的真实性，我们尝试使用两分量磁性模型对观测到的剖面进行拟合，其中磁场强度被限制为代表一个分量中像斑一样的区域的等分值，并且允许在较冷的区域中改变磁场代表斑点的组件。结果表明，这种模型与7055 A时TiO带头的光谱不一致。

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