本帖最后由 其祥 于 2009-11-17 19:47 编辑
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Figure 2.
Lithium and physical properties of planet-host solar-analogue and comparison stars.
图表2 ”有行星“恒星和”无行星“恒星的锂含量以及物理属性
Chromospheric activity indices R[sub]HK[/sub] were taken from the literature [sup]17, 27, 28 [/sup]while rotational velocities of the comparison sample stars and many planet hosts were measured from CORALIE and HARPS spectra using a cross correlation function [sup]29[/sup]. Typical 1σ uncertainties for log R[sub]HK[/sub] and vsini (panels (a) and (b), bottom right corner) are 0.1 dex and 0.3 km sec[sup]-1[/sup] , respectively [sup]17,29[/sup]. Rotational velocities of several planet-hosts were taken from the literature [sup]29,30[/sup]. The metallicities were measured [sup]12[/sup] with a 1σ precision of 0.05 dex (bottom right corner in panel (c)). In the panel (c )we plot Li abundances versus effective temperature in planet-hosts (red filled circles), and stars of the open clusters M67 (blue triangles) and NGC 6253 (open squares). The data for M67 were taken from the literature [sup]15[/sup]. Li abundances in NGC 6253 have been derived from VLT/Giraffe spectra using standard methods (Randich et al., in preparation). Typical 1σerror bars (panel (c), bottom right corner) are 0.15 dex and 100 K for log N(Li) and T[sub]eff[/sub], respectively.
通过应用互相关函数（参考文献29），在CORALIE 和 HARPS 光谱中被测量的”有行星“恒星及对照组样本的旋转速度，色球层活动指数RHK来自于相关文献（参考文献17，27，28）。典型的log R[sub]HK[/sub] 和vsini（图（a）和图（b）的右下角）的1σ不确定性分别为0.1 底什和0.3 km/s（参考文献17，29）。若干”有行星“恒星自转速率来自于相关文献（参考文献29，30）。在0.05底什（c图的右下角）的1σ精度下测量恒星的金属性（参考文献12）。在c(其祥注：困惑，应该是d图啊，难道发表在nature上的论文经过那么多人审核后存在这样的错误)图中，我们所绘制的是锂丰度和”有行星“恒星（实心红圈）的有效温度之间的关系，恒星为M67 （蓝色三角）和 NGC 6253（空心方框）星系中的恒星。M67的数据来自文献15，NGC 6253中锂丰度的数据应用标准法(Randich 等准备).取自于VLT/Giraffe 的光谱。典型的1σ误差线（图c右下角）对应log N(Li) 和 Teff的分别是0.15dex和100k。 |
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