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arXiv 1603.06604astro-ph.HEastro-ph.SR
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辐射驱动的光学厚风的动力学

The dynamics of radiation driven, optically thick winds

Rong-Feng Shen, Ehud Nakar, Tsvi Piran

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9 pages, 3 figures, MNRAS accepted, corrected proof
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摘要：

最近对一些具有低色温的发光瞬态源的观测表明，发射主要是由超爱丁顿吸积驱动的光学厚风。我们提出了一个一般的辐射压力驱动的动力学分析理论，光学厚风。与经典绝热恒星风解不同，其动力学仅由音速半径决定，这里由于光子扩散导致的辐射压力损失也起着重要作用。我们确定了两个高质量损失率制度（$\dot{M} > L_{\rm Edd\,}/c^2$）。在大的总光度区域，解类似于绝热风解。辐射光度$L$和动力学光度$L_k$都是超爱丁顿的，有$L < L_k$和$L \propto L_k^{1/3}$。在较低的总光度范围内，大部分能量由具有$L_k < L \approx L_{\rm Edd\,}$的辐射携带。在第三种低质量损失状态（$\dot{M} < L_{\rm Edd\,}/c^2$）中，风在早期变得光学薄，除非在这个阶段气体压力很重要，否则解与绝热解非常不同。这些结果与风脚下的能量产生机制无关，因此它们适用于广泛的质量喷射系统，从黑洞吸积到行星状星云和经典新星。

英文摘要：

Recent observation of some luminous transient sources with low color temperatures suggests that the emission is dominated by optically thick winds driven by super-Eddington accretion. We present a general analytical theory of the dynamics of radiation pressure-driven, optically thick winds. Unlike the classical adiabatic stellar wind solution whose dynamics are solely determined by the sonic radius, here the loss of the radiation pressure due to photon diffusion also plays an important role. We identify two high mass loss rate regimes ($\dot{M} > L_{\rm Edd\,}/c^2$). In the large total luminosity regime the solution resembles an adiabatic wind solution. Both the radiative luminosity, $L$, and the kinetic luminosity, $L_k$, are super-Eddington with $L < L_k$ and $L \propto L_k^{1/3}$. In the lower total luminosity regime most of the energy is carried out by the radiation with $L_k < L \approx L_{\rm Edd\,}$. In a third, low mass loss regime ($\dot{M} < L_{\rm Edd\,}/c^2$), the wind becomes optically thin early on and, unless gas pressure is important at this stage, the solution is very different from the adiabatic one. The results are independent from the energy generation mechanism at the foot of the wind, therefore they are applicable to a wide range of mass ejection systems, from black hole accretion, to planetary nebulae, and to classical novae.

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