arXiv 1012.29572010-12-14astro-ph.SRastro-ph.IM

超巨星A[e]星HD62623周围圆盘中旋转的气体和尘埃成像

Imaging the spinning gas and dust in the disc around the supergiant A[e] star HD62623

Florentin Millour, Anthony Meilland, Olivier Chesneau, Philippe Stee, Samer Kanaan, Romain Petrov, Denis Mourard, S. Kraus

备注：: To be published soon in A\&A
发表信息：: A&A (2010) xxx
DOI：: 10.1051/0004-6361/201016193

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摘要：

上下文为了进一步理解大质量恒星的演化，需要限制质量损失，并确定负责物质喷射的现象及其在星周环境中的重组。为了测试各种质量喷射过程，我们探测了A[e]超巨星HD 62623周围尘埃和气体的几何和运动学。方法.我们使用了VLTI/AMBER仪器所涵盖的高光谱和空间分辨率。由于一种新的多波长光学/红外干涉成像技术，我们重建了第一个速度分辨图像在红外域的毫角秒分辨率。结果我们成功地解开了HD 62623环星盘中的尘埃和气体辐射，测量了尘埃盘的内边缘，即6个质量，限制了盘的倾角和长轴的位置角，还测量了内部气体盘的延伸（2个质量），并利用AMBER高光谱分辨率探测了其速度场。我们发现，膨胀速度是可以忽略的，开普勒旋转是一个有利的速度场。如果物质抛射的主要机制仅仅是中心恒星的快速旋转，那么这样的速度场是意想不到的。结论.由于恒星本身的旋转速度似乎低于其分裂速度，旋转不能解释致密赤道盘的形成。此外，由于膨胀速度可以忽略不计，辐射驱动风也不是一个合适的解释来解释盘的形成。因此，最可能的假设是，物质在赤道平面的积累是由于光谱低质量伴星的存在。

英文摘要：

Context. To progress in the understanding of evolution of massive stars one needs to constrain the mass-loss and determine the phenomenon responsible for the ejection of matter an its reorganization in the circumstellar environment Aims. In order to test various mass-ejection processes, we probed the geometry and kinematics of the dust and gas surrounding the A[e] supergiant HD 62623. Methods. We used the combined high spectral and spatial resolution covered by the VLTI/AMBER instrument. Thanks to a new multiwavelength optical/IR interferometry imaging technique, we reconstructed the first velocity-resolved images with a milliarcsecond resolution in the infrared domain. Results. We managed to disentangle the dust and gas emission in the HD 62623 circumstellar disc.We measured the dusty disc inner inner rim, i.e. 6 mas, constrained the inclination angle and the position angle of the major-axis of the disc.We also measured the inner gaseous disc extension (2 mas) and probed its velocity field thanks to AMBER high spectral resolution. We find that the expansion velocity is negligible, and that Keplerian rotation is a favoured velocity field. Such a velocity field is unexpected if fast rotation of the central star alone is the main mechanism of matter ejection. Conclusions. As the star itself seems to rotate below its breakup-up velocity, rotation cannot explain the formation of the dense equatorial disc. Moreover, as the expansion velocity is negligible, radiatively driven wind is also not a suitable explanation to explain the disc formation. Consequently, the most probable hypothesis is that the accumulation of matter in the equatorial plane is due to the presence of the spectroscopic low mass companion.

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