NLTE models of line-driven stellar winds – III. Influence of X-ray radiation on wind structure of O stars

We study the influence of X-rays on the wind structure of selected O stars. For this purpose we use our non-local thermodynamic equilibrium (NLTE) wind code with inclusion of additional artificial source of X-rays, assumed to originate in the wind shocks.
We show that the influence of shock X-ray emission on wind mass-loss rate is relatively small. Wind terminal velocity may be slightly influenced by the presence of strong X-ray sources, especially for stars cooler than   T _eff≲ 35 000 K  .
We discuss the origin of the   L _X/ L ∼ 10⁻⁷  relation. For stars with thick wind this relation can be explained assuming that the cooling time depends on wind density. Stars with optically thin winds exhibiting the 'weak wind problem' display enhanced X-ray emission which may be connected with large shock cooling length. We propose that this effect can explain the 'weak wind problem'.
Inclusion of X-rays leads to a better agreement of the model ionization structure with observations. However, we do not find any significant influence of X-rays on P  v ionization fraction implying that the presence of X-rays cannot explain the P  v problem.
We study the implications of modified ionization equilibrium due to shock emission on the line transfer in the X-ray region. We conclude that the X-ray line profiles of helium-like ions may be affected by the line absorption within the cool wind.     

Precession and nutation in the η Carinae binary system: evidence from the X-ray light curve

It is believed that η Carinae is actually a massive binary system, with the wind–wind interaction responsible for the strong X-ray emission. Although the overall shape of the X-ray light curve can be explained by the high eccentricity of the binary orbit, other features like the asymmetry near periastron passage and the short quasi-periodic oscillations seen at those epochs have not yet been accounted for. In this paper we explain these features assuming that the rotation axis of η Carinae is not perpendicular to the orbital plane of the binary system. As a consequence, the companion star will face η Carinae on the orbital plane at different latitudes for different orbital phases and, since both the mass-loss rate and the wind velocity are latitude dependent, they would produce the observed asymmetries in the X-ray flux. We were able to reproduce the main features of the X-ray light curve assuming that the rotation axis of η Carinae forms an angle of  29°± 4°  with the axis of the binary orbit. We also explained the short quasi-periodic oscillations by assuming nutation of the rotation axis, with an amplitude of about  5°  and a period of about 22 days. The nutation parameters, as well as the precession of the apsis, with a period of about 274 years, are consistent with what is expected from the torques induced by the companion star.     

THE ANALYSIS ON THE STATISTICAL CHARACTER OF QUIKSCAT SCATTEROMETER WINDS AND STRONG WIND FREQUENCY USING REMOTE SENSOR DATA FROM QUIKSCAT

1 INTRODUCTION Most of the conventional sea surface wind data are measurements from ships, buoys and islands, with coverage and spatial resolution far below the requirements of research and application. At present, due to limited understanding of physical processes and efficient exploitation of data, numerical prediction models have not been used as they should be, although routine procedures are able to give sea surface wind fields at the intervals of 6 hours. With the development of sp…     

Symbiotic stars with spectral indication of bipolar ejection and stellar wind

Four out of a total of five symbiotic systems whose optical spectral lines contain satellite components indicating collimated ejection have an additional absorption of P Cyg type with different velocity. These systems are Z And, Hen 3‐1341, StHα 190, and BF Cyg. It is shown that the line profiles of every of these systems can be interpreted in the framework of a model of a collimated stellar wind from the hot compact component proposed initially to interpret the line profiles of Z And, observed during its last active phase after 2000. (© 2014 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

中国春季沙尘天气频数的时空变化及其与地面风压场的关系

文中利用EOF和SVD方法分析了近半个世纪中国春季沙尘天气频数的时空分布特征及其与近地面风速和海平面气压的关系。中国北方大部分地区春季沙尘天气发生频数近半个世纪呈减少趋势 ,2 0世纪 70年代末以前沙尘天气发生频数较多 ,70年代末开始逐渐减少 ,1997年降到最低值 ,同期中国近地面风速也呈减小趋势 ,两者之间存在显著相关。春季海平面气压场与中国沙尘天气的发生频数有十分密切的联系 ,海平面气压在中高纬度地区降低 ,中低纬度地区升高 ,气压梯度发生改变 ,从而引起地面风速减小 ,进一步影响到沙尘天气发生频数减少     

9608号台风登陆北上总能量变化及渤海高压维持

首先分析了属于台风与西风槽的相互作用型的９６０８号台风在其登陆泊台风核心区总能量及其组成部分的变化。结果指出,决定总能量再度增长的主要是潜热能,而此时潜热能的增长是同台风东侧低层偏南急流有密度关系。台风的东北象限内潜热能增长最盛,特大暴雨区恰也在这个象限。其次利用对流层高层散度风场与旋转风场的配置,从散度风动勇与旋转风动能之间的转换关系,半定量地估计台风东侧黄海、渤海、日本海高压上空反气旋环流的增     

黄渤海大风的客观相似预报

以MICAPS资料为基础，海平面气压资料为指标，设计了一种通过计算相似系数查找相似形势，制作黄、渤海地区24h大风的客观预报方法，并建立了包括109个大风历史个例资料库。试验结果表明，风速预报的平均误差在20％以下，满足大风预报业务的要求。相似法具有不需依赖国外资料及计算简单迅速的特点，它不仅是现在日常业务的一个补充，更重要的是，它是一种可以在战争等非常情况下使用的预报方法。