VLTI/AMBER spectro-interferometry of the Herbig Be star MWC 297 with spectral resolution 12 000
VLTI/AMBER spectro-interferometry of the Herbig Be star MWC 297 with spectral resolution 12 000
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Herbig Be 星 MWC 297 的 VLTI/AMBER 光谱干涉测量，光谱分辨率 12 000
DOI：
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发表时间：
2011
期刊：
影响因子：
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通讯作者：
E. Tatulli
中科院分区：
文献类型：
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作者：
G. Weigelt;V. Grinin;J. Groh;K. Hofmann;S. Kraus;A. S. Miroshnichenko;D. Schertl;L. Tambovtseva;M. Benisty;T. Driebe;S. Lagarde;F. Malbet;A. Meilland;A. Meilland;R. Petrov;E. Tatulli
上下文星周盘和外流在星星的形成中起着重要作用。红外光谱干涉法可以解决内部吸积-喷射区域。目标。我们研究的磁盘和Br发射区的MWC 297高空间和光谱分辨率，并比较我们的观测与磁盘风模型。方法.我们测量的干涉vibrations，波长差分相位，并关闭阶段的MWC 297与光谱分辨率为12000。为了解释我们的MWC 297观测，我们采用了盘风模型。结果测量的连续光谱证实了先前的结果，MWC 297的连续发射区是非常紧凑的。我们得到了一个连续环拟合半径为2.2质量（在250 pc的距离上为0.56 Au），这比硅酸盐颗粒预期的3 Au尘埃升华半径小5.4倍（在没有辐射屏蔽材料的情况下）。强波长依赖和不对称的Br-发射区比连续发射区扩展了约2.7倍。在Br线的中心，我们推导出高斯拟合半径为6.3 mas HWHM（1.6 Au）。为了解释这些观测结果，我们采用了一个磁离心驱动的盘风模型，该模型由一个吸积盘和一个盘风组成，吸积盘发出观测到的连续辐射，盘风发出Br线。将计算的波长相关模型强度分布和Br线轮廓与观测结果进行比较（即，K-波段光谱、振动频率、微分相位和闭合相位）。最接近的拟合模型预测了一个内半径为-0.3 Au的连续发射盘和一个内半径为-0.5 Au（-17.5恒星半径）的盘风喷射区。我们获得的盘风半张角（旋转轴与盘风最内侧流线之间的角度）为80 °，大于T Tau模型，盘倾角为20 °（即，几乎极点上）。结论.我们的观测光谱分辨率为12000，使我们能够在Br发射线的10个不同光谱通道中研究MWC 297的AU尺度环境。我们发现，K-波段的通量，village，和非常强的相位可以解释所采用的磁离心驱动盘风模型。
Context. Circumstellar disks and outflows play a fundamental role in star formation. Infrared spectro-interferometry allows the inner accretion-ejection region to be resolved. Aims. We study the disk and Br-emitting region of MWC 297 with high spatial and spectral resolution and compare our observations with disk-wind models. Methods. We measured interferometric visibilities, wavelength-differential phases, and closure phases of MWC 297 with a spectral resolution of 12000. To interpret our MWC 297 observations, we employed disk-wind models. Results. The measured continuum visibilities confirm previous results that the continuum-emitting region of MWC 297 is remarkably compact. We derive a continuum ring-fit radius of �2.2 mas (�0.56 AU at a distance of 250 pc), which is �5.4 times smaller than the 3 AU dust sublimation radius expected for silicate grains (in the absence of radiation-shielding material). The strongly wavelength-dependent and asymmetric Br-emitting region is more extended (�2.7times) than the continuum-emitting region. At the center of the Br line, we derive a Gaussian fit radius of �6.3 mas HWHM (�1.6 AU). To interpret the observations, we employ a magneto-centrifugally driven disk-wind model consisting of an accretion disk, which emits the observed continuum radiation, and a disk wind, which emits the Br line. The calculated wavelength-dependent model intensity distributions and Br line profiles are compared with the observations (i.e., K-band spectrum, visibilities, differential phases, and closure phases). The closest fitting model predicts a continuumemitting disk with an inner radius of �0.3 AU and a disk wind ejection region with an inner radius of �0.5 AU (�17.5 stellar radii). We obtain a disk-wind half-opening angle (the angle between the rotation axis and the innermost streamline of the disk wind) of �80 � , which is larger than in T Tau models, and a disk inclination angle of �20 � (i.e., almost pole-on). Conclusions. Our observations with a spectral resolution of 12000 allow us to study the AU-scale environment of MWC 297 in �10 different spectral channels across the Br emission line. We show that the K-band flux, visibilities, and remarkably strong phases can be explained by the employed magneto-centrifugally driven disk wind model.
影响因子：
3.2
作者：
V. Mannings;A. Boss;S. Russell
通讯作者：
V. Mannings;A. Boss;S. Russell