THE H-BAND EMITTING REGION OF THE LUMINOUS BLUE VARIABLE P CYGNI: SPECTROPHOTOMETRY AND INTERFEROMETRY OF THE WIND
THE H-BAND EMITTING REGION OF THE LUMINOUS BLUE VARIABLE P CYGNI: SPECTROPHOTOMETRY AND INTERFEROMETRY OF THE WIND
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发光蓝变星天鹅座 P 的 H 波段发射区：风的分光光度测量和干涉测量
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发表时间：
2013
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通讯作者：
P. J. Goldfinger
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作者：
Noel D Richardson;Noel D Richardson;Noel D Richardson;G. Schaefer;D. Gies;D. Gies;O. Chesneau;J. D. Monnier;F. Baron;F. Baron;Xiao Che;J. Parks;R. Matson;R. Matson;Y. Touhami;D. Clemens;E. Aldoretta;E. Aldoretta;Nancy D. Morrison;T. Brummelaar;H. Mcalister;S. Kraus;S. Ridgway;J. Sturmann;L. Sturmann;B. Taylor;N. Turner;C. Farrington;P. J. Goldfinger
我们首次在近红外H波段（1.6 μm）对天鹅座星星P进行了高角分辨率观测。利用CHARA阵列和MIRC合束器进行了6台望远镜的干涉观测。这表明空间通量分布比预期的恒星光球大。星星（均匀盘）加晕（二维高斯）的两个组件模型产生一个很好的适合的观测，我们建议，晕对应于从恒星风的基地发出的通量。这个风分量贡献了大约45%的H波段通量，并且具有角半高宽= 0.96质量，而预测的恒星直径为0.41质量。我们展示了几个图像重建的干涉vibrium和关闭阶段，他们表示一个一般的球形几何风。我们还获得了天鹅座P的近红外分光光度法，从中我们推导出的流量过剩相比，一个纯粹的光球光谱能量分布。H-波段通量过剩匹配，从风通量部分来自两个组件适合干涉。我们发现了2006年至2010年期间近红外通量显著变化的证据，这些变化与风中Hα排放通量的变化相似。
We present the first high angular resolution observations in the near-infrared H band (1.6 μm) of the luminous blue variable star P Cygni. We obtained six-telescope interferometric observations with the CHARA Array and the MIRC beam combiner. These show that the spatial flux distribution is larger than expected for the stellar photosphere. A two-component model for the star (uniform disk) plus a halo (two-dimensional Gaussian) yields an excellent fit of the observations, and we suggest that the halo corresponds to flux emitted from the base of the stellar wind. This wind component contributes about 45% of the H-band flux and has an angular FWHM = 0.96 mas, compared to the predicted stellar diameter of 0.41 mas. We show several images reconstructed from the interferometric visibilities and closure phases, and they indicate a generally spherical geometry for the wind. We also obtained near-infrared spectrophotometry of P Cygni from which we derive the flux excess compared to a purely photospheric spectral energy distribution. The H-band flux excess matches that from the wind flux fraction derived from the two-component fits to the interferometry. We find evidence of significant near-infrared flux variability over the period from 2006 to 2010 that appears similar to the variations in the Hα emission flux from the wind.