On the observability of bow shocks of Galactic runaway OB stars
On the observability of bow shocks of Galactic runaway OB stars
复制标题
银河系失控OB星弓形激波的可观测性
DOI：
10.1093/mnras/stw651
复制
发表时间：
2016
影响因子：
4.8
通讯作者：
W. Kley
中科院分区：
文献类型：
--
作者：
D. Meyer;A. J. Marle;A. J. Marle;R. Kuiper;W. Kley
从母星团中被抛射出来并以超音速航行通过星际介质（ISM）的大质量恒星被归类为流亡星。它们产生可以观测到的拱星弓形激波星云。我们提出了二维，轴对称流体动力学模拟的代表性样本的恒星风弓冲击银河OB星在周围介质的密度范围从n_ISM=0.01到10.0/cm 3。独立于它们在银河系中的位置，我们确认红外线是最合适的波段，以寻找弓冲击从大质量恒星。它们的谱能量分布是分析它们的方便工具，因为它们的发射不依赖于可能影响不稳定薄壳弓形激波的暂时效应。我们的数值模型产生的高质量（~40 Mo）失控恒星的银河系弓激波产生H$\alpha$通量，可以观察到的设施，如超级宇宙H-阿尔法调查。最明亮的弓形激波星云产生于ISM的密度较高的区域。我们预测，在哈通过瑞利敏感设施观察到的领域中的弓激波周围形成的初始质量大于约20钼的恒星。我们的OB星弓形激波模型在3 <= lambda <= 50 μ m波长范围内具有最大发射，这可以比逃逸星本身亮几个数量级，特别是对于初始质量大于20 Mo的恒星。
Massive stars that have been ejected from their parent cluster and supersonically sailing away through the interstellar medium (ISM) are classified as exiled. They generate circumstellar bow shock nebulae that can be observed. We present two-dimensional, axisymmetric hydrodynamical simulations of a representative sample of stellar wind bow shocks from Galactic OB stars in an ambient medium of densities ranging from n_ISM=0.01 up to 10.0/cm3. Independently of their location in the Galaxy, we confirm that the infrared is the most appropriated waveband to search for bow shocks from massive stars. Their spectral energy distribution is the convenient tool to analyze them since their emission does not depend on the temporary effects which could affect unstable, thin-shelled bow shocks. Our numerical models of Galactic bow shocks generated by high-mass (~40 Mo) runaway stars yield H$\alpha$ fluxes which could be observed by facilities such as the SuperCOSMOS H-Alpha Survey. The brightest bow shock nebulae are produced in the denser regions of the ISM. We predict that bow shocks in the field observed at Ha by means of Rayleigh-sensitive facilities are formed around stars of initial mass larger than about 20 Mo. Our models of bow shocks from OB stars have the emission maximum in the wavelength range 3 <= lambda <= 50 micrometer which can be up to several orders of magnitude brighter than the runaway stars themselves, particularly for stars of initial mass larger than 20 Mo.
影响因子：
6.5
作者：
Brott, I.;Evans, C. J.;Anders, P.
通讯作者：
Anders, P.
DOI：
10.1088/0004-6256/140/6/1868
发表时间：
2010-07
期刊：
The Astronomical Journal
影响因子：
--
作者：
E. Wright;P. Eisenhardt;A. Mainzer;M. Ressler;R. Cutri;T. Jarrett;J. Kirkpatrick;D. Padgett;
通讯作者：
E. Wright;P. Eisenhardt;A. Mainzer;M. Ressler;R. Cutri;T. Jarrett;J. Kirkpatrick;D. Padgett;