论文标题
碰撞引起的卫星在Balmer-Beta系列的蓝翼和Balmer系列的后果
Collision-induced satellite in the blue wing of the Balmer-beta line and consequences on the Balmer series
论文作者
论文摘要
在本文中，我们强调了Balmer系列在氦气为主导的DBA白色矮人恒星中的非Lorentzian行为，为了确定氢丰度以确定数十年历史的问题。在最近的一项工作中，我们已经表明，由于H-HE和H-H碰撞而引起的准分子线卫星负责使用宇宙起源光谱仪（COS）观察到的Lyman-Alpha线的不对称形状，并且对于Balmer-Alpha线概要文件而言，类似的不对称性存在。在最近的工作中，确定了n = 2、3势能和从基态的过渡偶极矩，在这里，我们提出了与H（n = 4）+HE+HE及其与HE（n = 4）的分子状态相关的势能和电子过渡偶极矩与H（n = 4）+与H（N = 2）相关的状态。这些新数据用于对He扰动的H扰动H Balmer-Beta系列的蓝翼进行理论研究。由于表征了Balmer系列中势能的排斥性Sigma状态的总体趋势，因此线核心的幅度随着氦密度的较大，随着该系列的顺序降低非常快，而氦气密度达到10^21 cm^-3。这项研究是通过应用统一的光谱线扩展理论来进行的，该理论在DZA白矮星恒星中发现的非常高的氦密度有效。 该处理包括由于渐近禁止过渡而引起的碰撞引起的（CI）线卫星，并解释了它们在光谱中观察到的不对称性。
In this paper we emphasize the non-Lorentzian behavior of the Balmer series in helium-dominated DBA white dwarf stars for which the decades-old problem exists for the determination of the hydrogen abundance. In a very recent work, we have shown that quasi-molecular line satellites due to H-He and H-H collisions are responsible for the asymmetrical shape of the Lyman-alpha lines observed with the Cosmic Origin Spectrograph (COS) and that a similar asymmetry exists for the Balmer-alpha line profiles. In continuation with very recent work, where the n=2, 3 potential energies and transition dipole moments from the ground state were determined, here, we present accurate H-He potential energies and electronic transition dipole moments concerning the molecular states correlated with H(n=4)+He and their transition dipole moments with the states correlated with H(n=2)+He. Those new data are used to provide a theoretical investigation of the collisional effects in the blue wing of the Balmer-beta line of H perturbed by He. Because of the general trend characterizing the repulsive Sigma states of the potential energies involved in the Balmer series, the amplitude in the core of the line is decreasing very fast with the order of the series when the helium density gets as large as 10^21 cm^-3. This study is undertaken by applying a unified theory of spectral line broadening that is valid at very high helium densities found in DZA white dwarf stars. The treatment includes collision-induced (CI) line satellites due to asymptotically forbidden transitions, and it explains the asymmetry observed in their spectra.
