Simulation of Accretion Disk Wind Spectra in Cataclysmic Variables with a 3D non-LTE Monte-Carlo Radiation Transfer Code

我们的主要目标是完成我们的3-D蒙特卡罗（MC）辐射传输代码的发展，使从激变变星（CV）的风合成光谱的计算。MC代码将在统计平衡（非LTE）和能量守恒的约束下求解辐射传输方程。该代码将是第一个不依赖于简化电离平衡和原子水平人口假设的工具。在MC码中的完全非LTE问题的解决方案现在在L.B. Lucy（所谓的macroatom approach）。我们的第二个目标是改进CV风的外流模型。目前从流体动力学模型得到的质量损失率比从观测得到的要低1-2个数量级。我们认为，这种不一致性根源于对原子物理、辐射场和电离分层的高度简化处理。我们的MC方法将首次给出风等离子体物理条件的精确信息。我们的第三个目标是比较合成光谱的观测，以估计各种模型参数的影响。MC代码将完成我们的程序包，将允许整个CV系统（白色矮星，吸积盘，盘风）的所有光谱成分的描述。

Our primary aim is to complete the development of our 3-D Monte Carlo (MC) radiation transfer code to enable the computation of synthetic spectra of winds from cataclysmic variable stars (CVs). The MC code will solve the radiation transfer equation under the constraints of statistical equilibrium (non-LTE) and energy conservation. This code will be the first tool that does not rely on simplifying assumptions on ionisation balance and atomic level populations. The solution of the full non-LTE problem in a MC code appears feasible now after recent pioneering developments achieved by L.B. Lucy (so-called macroatom approach). Our second aim is to improve the outflow models for CV winds. At present the mass-loss rates obtained from hydrodynamical models are 1-2 orders of magnitude below those expected from observations. We think that this inconsistency roots in the highly simplified treatment of atomic physics, radiation field, and ionisation stratification. Our MC approach will for the first time give precise information on the physical conditions in the wind plasma. Our third aim is the comparison of synthetic spectra to observations in order to estimate the influence of various model parameters. The MC code will complete our program package that will allow the description of all spectral components of the entire CV system (white dwarf, accretion disk, disk wind).