HIGH-RESOLUTION IUE SPECTROSCOPY OF FAST WINDS FROM CATACLYSMIC VARIABLES
HIGH-RESOLUTION IUE SPECTROSCOPY OF FAST WINDS FROM CATACLYSMIC VARIABLES
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来自灾难性变量的快风的高分辨率 IUE 光谱
DOI：
10.1093/mnras/273.2.461
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发表时间：
1995
影响因子：
4.8
通讯作者：
R. Rosen
中科院分区：
文献类型：
--
作者：
R. Prinja;R. Rosen
使用 31 个高分辨率 IUE 光谱研究了来自 6 个矮新星和 4 个类新星灾难变星的风。这些数据提供了有关圆盘驱动流出的时间和相位平均性质的详细信息，这些特征是通过由于 C IV、N V 和 Si IV 共振线双峰以及 He II lambda 1640 导致的类 P Cygni 和扩展吸收分布的存在来诊断的。这些分布通过吸收和发射速度、宽度和强度的测量进行参数化。最大风速可超过 -4000 km s(-1)，但吸收最大值（最小通量）通常出现在大约 20% 的短剖面边缘处。在吸收槽中识别出光学深度和速度结构，这可能表明流出的不均匀性。讨论了相对离子行为以及对内盘和风的发射剖面的各自贡献。综合模型轮廓用于估计质量损失率和 C3+ 离子分数的乘积。
The winds from six dwarf novae and four nova-like cataclysmic variables are studied using 31 high-resolution IUE spectra. The data provide details on the time- and phase-averaged nature of disc-driven outflows, which are diagnosed via the presence of P Cygni-like and extended absorption profiles due to the C IV, N V and Si IV resonance line doublets, and He II lambda 1640. The profiles are parametrized using measures of the absorption and emission velocities, widths and strengths. The maximum wind velocity can exceed -4000 km s(-1), although the absorption maximum (minimum flux) typically occurs at similar to 20 per cent of the shortward profile edge. Optical depth and velocity structure is identified in the absorption troughs which may indicate inhomogeneities in the outflows. The relative ion behaviour and the respective contributions to the emission profiles of the inner disc and wind are discussed. Synthesized model profiles are used to estimate the products of mass-loss rate and C3+ ion fractions.