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

使用 3D 非 LTE 蒙特卡罗辐射传递代码模拟灾难性变量中的吸积盘风谱

• 批准号: 24942277
• 负责人: Professor Dr. Klaus Werner
• 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: 2006
• 资助国家: 德国
• 起止时间: 2005-12-31 至 2009-12-31
• 项目状态: 已结题
• 来源: https://gepris.dfg.de/gepris/projekt/24942277?language=en
• 关键词: Simulation; Accretion; Disk; Wind; Spectra

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).

我们的主要目的是完成我们3-D蒙特卡洛（MC）辐射转移代码的开发，以实现从灾难性变量恒星（CVS）中的风的合成光谱计算。 MC代码将在统计平衡（非LTE）和能源保护的约束下解决辐射转移方程。该代码将是第一个不依赖于简化有关电离平衡和原子水平种群的假设的工具。 L.B.最近的开创性发展后，MC代码中的完整非LTE问题的解决方案现在似乎是可行的。露西（所谓的宏观方法）。我们的第二个目标是改善简历风的流出模型。目前，从流体动力学模型获得的质量损失率低1-2个数量级，低于观察结果的预期。我们认为，这种不一致的根源在原子理，辐射场和电离分层的高度简化处理中。我们的MC方法将首次提供有关风血浆中物理状况的精确信息。我们的第三个目标是将合成光谱与观测值进行比较，以估算各种模型参数的影响。 MC代码将完成我们的程序包，该程序包将允许描述整个简历系统的所有光谱组件（白矮人，积聚磁盘，磁盘风）。