The O stars in the VLT-FLAMES Tarantula Survey
The O stars in the VLT-FLAMES Tarantula Survey
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DOI：
10.1088/1742-6596/328/1/012022
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发表时间：
2011-12
期刊：
影响因子：
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通讯作者：
A. D. Koter;H. Sana;C. Evans;T. Bagnoli;N. Bastian;J. Bestenlehner;A. Bonanos;E. Bressert;I. Brott;M. Cantiello;G. Carraro;Stephen Clark;P. Crowther;S. D. Mink;E. Doran;P. Dufton;P. Dunstall;M. Garcia;G. Gräfener;V. Hénault-Brunet;A. Herrero;I. Howarth;R. Izzard;K. Kohler;N. Langer;D. Lennon;J. M. Apellániz;N. Markova;Paco Najarro;J. Puls;O. Ramírez;C. Sabín-Sanjulián;S. Simón-Díaz;S. Smartt;V. Stroud;J. V. Loon;W. Taylor;J. Vink
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文献类型：
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作者：
A. D. Koter;H. Sana;C. Evans;T. Bagnoli;N. Bastian;J. Bestenlehner;A. Bonanos;E. Bressert;I. Brott;M. Cantiello;G. Carraro;Stephen Clark;P. Crowther;S. D. Mink;E. Doran;P. Dufton;P. Dunstall;M. Garcia;G. Gräfener;V. Hénault-Brunet;A. Herrero;I. Howarth;R. Izzard;K. Kohler;N. Langer;D. Lennon;J. M. Apellániz;N. Markova;Paco Najarro;J. Puls;O. Ramírez;C. Sabín-Sanjulián;S. Simón-Díaz;S. Smartt;V. Stroud;J. V. Loon;W. Taylor;J. Vink
VLT-FLAMES狼蛛巡天（VFTS）已经获得了大麦哲伦星云剑鱼座30区域300多颗o型恒星的中分辨率光谱。对如此大的样本进行同质分析需要自动化技术，这种方法也将用于即将进行的对北半球和南半球的盖亚调查的分析，以补充盖亚的测量。指出了Gaia对O星研究的重要性，总结了VFTS的O星科学案例，并对综合生成数据的自动建模技术进行了测试。该方法采用基于遗传算法的优化技术，结合快速风模型大气。结果表明，该方法具有较好的鲁棒性，能够准确地恢复光球的主要参数。精确的风参数也可以得到，然而，正如预期的那样，对于矮星来说，风的加速速度很难得到约束。
The VLT-FLAMES Tarantula Survey (VFTS) has secured mid-resolution spectra of over 300 O-type stars in the 30 Doradus region of the Large Magellanic Cloud. A homogeneous analysis of such a large sample requires automated techniques, an approach that will also be needed for the upcoming analysis of the Gaia surveys of the Northern and Southern Hemisphere supplementing the Gaia measurements. We point out the importance of Gaia for the study of O stars, summarize the O star science case of VFTS and present a test of the automated modeling technique using synthetically generated data. This method employs a genetic algorithm based optimization technique in combination with fastwind model atmospheres. The method is found to be robust and able to recover the main photospheric parameters accurately. Precise wind parameters can be obtained as well, however, as expected, for dwarf stars the rate of acceleration of the ow is poorly constrained.