New Fe I level energies and line identifications from stellar spectra
Ruth C. Peterson, Robert L. Kurucz
备注：
v3 is the version submitted to the Astrophysical Journal Oct. 24, 2014, 10 pages, 3 tables, 5 figures, in response to the referee's report; minor corrections to that submission appear in italics. The number of newly-identified levels has nearly doubled to 66 (23 even, 43 odd), with a corresponding increase in the number of newly-identified lines. The full listing of these lines is included
Fe I原子的光谱对天体物理学的许多领域和其他领域都至关重要。然而，尽管对紫外实验室铁吸收光谱、光学实验室铁发射光谱和太阳红外光谱进行了广泛的分析，但对其高能级能量的测量仍然非常不完整。在这项工作中，我们使用的高分辨率档案吸收线的紫外线和恒星的光谱，其温暖的温度有利于温和的Fe I激发源。我们得出的能量为一个特定的上水平在库鲁茨的半经验计算采用一个试验值，产生相同的波长为一个给定的线预测是一样强的一个强的不明谱线观察到的恒星光谱，然后检查新的波长的其他强预测的过渡，共享相同的上水平与其他强观察到的不明线。到目前为止，这种分析提供了66 Fe I能级的上限能量。许多新能级的能量高于实验室实验所能获得的能量，有几个超过了Fe I的电离能。这些水平提供了超过2000个潜在可检测线的新鉴定。几乎所有的新水平的奇宇称包括紫外线检测到，但未分类在实验室的Fe I吸收光谱，提供了一个外部检查的能量值。我们激励和目前的程序，提供由此产生的新的水平的能量和它们的不确定性，列出所有潜在的可检测的紫外线和光学新的Fe I线的识别和它们的GF值，指出新的天体物理学感兴趣的线路，并讨论在不久的将来的前景，额外的Fe I能级测定。
英文摘要：
The spectrum of the Fe I atom is critical to many areas of astrophysics and beyond. Measurements of the energies of its high-lying levels remain woefully incomplete, however, despite extensive analysis of ultraviolet laboratory iron absorption spectra, optical laboratory iron emission spectra, and the solar infrared spectrum. In this work we use as sources the high-resolution archival absorption-line ultraviolet and optical spectra of stars, whose warm temperatures favor moderate Fe I excitation. We derive the energy for a particular upper level in Kurucz's semiempirical calculations by adopting a trial value that yields the same wavelength for a given line predicted to be about as strong as that of a strong unidentified spectral line observed in the stellar spectra, then checking the new wavelengths of other strong predicted transitions that share the same upper level for coincidence with other strong observed unidentified lines. To date this analysis has provided the upper energies of 66 Fe I levels. Many new level energies are higher than those accessible to laboratory experiments; several exceed the Fe I ionization energy. These levels provide new identifications for over two thousand potentially detectable lines. Almost all of the new levels of odd parity include UV lines that were detected but unclassified in laboratory Fe I absorption spectra, providing an external check on the energy values. We motivate and present the procedure, provide the resulting new level energies and their uncertainties, list all the potentially detectable UV and optical new Fe I line identifications and their gf-values, point out new lines of astrophysical interest, and discuss the prospects for additional Fe I energy-level determinations in the near future.
The impact of envelope binding energies on the merger rate density of binary compact objects
Universität Heidelberg, Zentrum für Astronomie (ZAH), Institut für Theoretische Astrophysik（海德堡大学天文学中心理论天体物理研究所）；SISSA（的里雅斯特国际高等研究学院）；National Institute for Nuclear Physics – INFN, Sezione di Trieste（意大利国家核物理研究所的里雅斯特分部）；Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Roma（意大利国家天体物理研究所罗马天文台）；Physics and Astronomy Department Galileo Galilei, University of Padova（帕多瓦大学伽利略·伽利莱物理学与天文学系）；INAF-Osservatorio Astronomico di Padova（意大利国家天体物理研究所帕多瓦天文台）；Departament de Física Quàntica i Astrofísica, Institut de Ciències del Cosmos, Universitat de Barcelona（巴塞罗那大学宇宙科学研究所量子物理与天体物理学系）；Niels Bohr International Academy, Niels Bohr Institute（尼尔斯·玻尔研究所尼尔斯·玻尔国际学院）；Departamento de Astronomía, Facultad Ciencias Físicas y Matemáticas, Universidad de Concepción（康塞普西翁大学理学院天文学系）
Scalable, Advanced Machine Learning-based Approaches for Stellar Flare Identification: Application to TESS short-cadence Data and Analysis of a New Flare Catalogue
A New Approach to Determine Radiative Capture Reaction Rates at Astrophysical Energies
辐射俘获反应在恒星核合成中起着至关重要的作用，但已被证明具有挑战性的实验确定。特别是，在任何恒星演化模型中，测量的$^{12}$ C $(α,γ)^{16}$ O反应速率的大不确定性（$\sim$ 100%）是最大的不确定性来源。随着新的高电流能量回收直线加速器（ERLs）和高密度气体靶的发展，使用细致平衡测量接近阈值的$^{16}$ O $(e,e^\prime α)^{12}$ C反应开辟了一种新的方法来确定$^{12}$ C $(α,γ)^{16}$ O反应速率，其精度显著提高（$<$ 20%）。我们提出的形式主义与光和电衰变反应，并考虑设计一个最佳的实验，以提供更高的精度。一旦新的ERLs上线，应该进行实验来验证我们提出的新方法。这种新方法对天体物理中的辐射俘获反应具有广泛的适用性。
