Radiation driven winds from hot stars: hydrodynamic models with detailed non-LTE radiative transfer

来自热星的辐射驱动风：具有详细非 LTE 辐射传输的流体动力学模型

• 批准号: 185561515
• 负责人: Professor Dr. Wolf-Rainer Hamann
• 金额: --
• 依托单位: Institut für Physik und Astronomie
• 依托单位国家: 德国
• 项目类别: Research Grants
• 财政年份: 2011
• 资助国家: 德国
• 起止时间: 2010-12-31 至 2014-12-31
• 项目状态: 已结题
• 来源: https://gepris.dfg.de/gepris/projekt/185561515?language=en
• 关键词: Radiation; driven; winds; hot; stars

Stars much more massive than the sun play an important role in the cosmic evolution. As their special property, they possess stellar winds that blow lots of matter into their environment. Radiation pressure must be considered in the first place as the driving mechanism. While this is reasonably well understood for part of the stars, the models fail just for the strongest of those stellar winds, which emerge from the so-called Wolf-Rayet stars. After pilot studies we can assume that those strong winds can also be explained by radiation pressure. If so, the corresponding shortfall of previous hydrodynamical models must be due to certain approximations in their treatment of radiative transfer.Such simplifications are avoided by the Potsdam Wolf-Rayet (PoWR) model atmosphere code, which we have developed for the simulation and analysis of spectra. As we have already shown, this code can be combined with the hydrodynamic equations. In the proposed project we will develop these model calculation into a form that they can be routinely applied. Then the comparison with observations will reveal if the dense stellar winds can be generally explained by radiation pressure. The final goal are realistic model predictions, which are needed for understanding the evolution of massive stars and the cosmic circuit of matter.

质量比太阳大得多的恒星在宇宙演化中起着重要作用。作为它们的特殊属性，它们拥有将大量物质吹到环境中的恒星风。首先必须考虑辐射压力作为驱动机制。虽然这对于部分恒星来说是相当好理解的，但模型只适用于最强的恒星风，这些恒星风来自所谓的沃尔夫-拉叶星。在初步研究之后，我们可以假设这些强风也可以用辐射压力来解释。如果是这样的话，以前的流体动力学模式的相应不足，必须是由于某些近似处理的辐射transformation.Such简化是避免了波茨坦Wolf-Rayet（PoWR）模式大气代码，我们已经开发的模拟和分析的光谱。正如我们已经指出的，这个代码可以与流体动力学方程结合起来.在拟议的项目中，我们将把这些模型计算发展成一种可以常规应用的形式。然后与观测结果进行比较，将揭示密集的恒星风是否可以用辐射压来解释。最终目标是现实的模型预测，这是理解大质量恒星的演化和物质的宇宙回路所需要的。

项目成果

The donor star of the X-ray pulsar X1908+075

X射线脉冲星X1908 075的供体星

• DOI: 10.1051/0004-6361/201424823
• 发表时间: 2015
• 期刊: arXiv: Solar and Stellar Astrophysics
• 作者: S. Martínez-Nunez;A. Sander;A. Gímenez-García;A. Gónzalez-Gálan;J. M. Torrejón;C. Gónzalez-Fernández;W.-R. Hamann
• 通讯作者: W.-R. Hamann

Discovery of a new Wolf-Rayet star and a candidate star cluster in the Large Magellanic Cloud with Spitzer

斯皮策在大麦哲伦星云中发现了一颗新的沃尔夫-拉叶星和一个候选星团

• DOI: 10.1093/mnras/stu909
• 发表时间: 2014
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: V. V. Gvaramadze;A.-N. Chené;A. Y. Kniazev;O. Schnurr;T. Shenar;A. Sander;R. Hainich;N. Langer;W.-R. Hamann;Y.-H. Chu;R. A. Gruendl
• 通讯作者: R. A. Gruendl

The Wolf-Rayet stars in M 31. I. Analysis of the late-type WN stars

M 31中的沃尔夫-拉叶星I晚型WN星分析

• DOI: 10.1051/0004-6361/201323240
• 发表时间: 2014
• 期刊: Astronomy and Astrophysics
• 影响因子: 6.5
• 作者: A. Sander;H. Todt;R. Hainich;W.-R. Hamann
• 通讯作者: W.-R. Hamann

One of the most massive stars in the Galaxy may have formed in isolation

银河系中质量最大的恒星之一可能是孤立形成的

• DOI: 10.1093/mnras/stt1817
• 发表时间: 2013
• 期刊: Monthly Notices of the Royal Astronomical Society
• 影响因子: 4.8
• 作者: L. M. Oskinova;M. Steinke;W.-R. Hamann;A. Sander;H. Todt;A. Liermann
• 通讯作者: A. Liermann

Potsdam Wolf-Rayet model atmosphere grids for WN stars

• DOI: 10.1051/0004-6361/201526253
• 发表时间: 2015-07
• 期刊: Astronomy and Astrophysics
• 影响因子: 6.5
• 作者: H. Todt;A. Sander;R. Hainich;W. Hamann;M. Quade;T. Shenar