发表机构
University of Warwick; University of Kiel; Center for Astrophysics, Harvard & Smithsonian; The Space Telescope Science Institute; University College London; Boston University; Forschungszentrum Jülich GmbH（华威大学; 基尔大学; 哈佛-史密森尼天体物理中心; 太空望远镜科学研究所; 伦敦大学学院; 波士顿大学; 于利希研究中心有限公司）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
对太阳13秒差距内44颗白矮星进行多波长分析，用混合拟合方法计算大气参数，发现氢大气白矮星温度差异，重新分类富氦白矮星，识别出紫外金属星，揭示白矮星行星系统证据及不同类型白矮星氢碳含量差异和多重性分数。
AI 中文摘要
我们对太阳13秒差距内44颗已确认的白矮星进行了全面的多波长光谱和光度分析。结合哈勃太空望远镜（STIS和COS）的通量校准紫外光谱、地面光学光谱以及盖亚、2MASS和WISE的光度测量，采用混合拟合方法计算大气参数。除两颗强磁星外，为每颗白矮星定制模型。发现Teff<10,000K的氢大气白矮星存在系统差异，紫外光谱拟合的有效温度比仅光学和红外光度测量得出的高2%-6%。重新分类三颗富氦白矮星。共识别出6颗仅在紫外中检测到金属的恒星。发现30%的13秒差距白矮星有行星系统演化的光谱证据。分析显示DQ和DC白矮星氢含量无显著差异，DC碳上限低于DQ。13秒差距白矮星的多重性分数为32%。
英文摘要
We present a comprehensive multi-wavelength spectroscopic and photometric analysis of the 44 confirmed white dwarfs within 13 pc of the Sun. Combining flux-calibrated ultraviolet spectroscopy from the Hubble Space Telescope (STIS and COS) with ground-based optical spectroscopy, as well as photometry from Gaia, 2MASS, and WISE, we employ a combined fitting method to calculate atmospheric parameters. Each white dwarf is fitted with a bespoke model depending on its detailed atmospheric composition. Two strongly magnetic stars could not be fitted due to the complex splitting of their spectral lines. We find a systematic discrepancy in hydrogen-atmosphere white dwarfs with effective temperatures below 10,000K, where fits incorporating ultraviolet spectra result in effective temperatures that are 1 - 5 per cent higher than those derived from optical and infrared photometry alone. We re-classify three helium-atmosphere white dwarfs as metal enriched following a magnesium detection in their near-ultraviolet spectra: WD 0435-088, WD 1132-325 and WD 1917+386. In total, we identify five stars in the sample for which metals are only detected in the ultraviolet. Overall, we find that 30 per cent of the 13 pc white dwarfs show spectroscopic evidence of evolved planetary systems. Our analysis reveals no measurable difference between the hydrogen content of DQ and DC white dwarfs, although the upper limits of carbon in DCs are significantly below that of the DQ population. We find a multiplicity fraction of 33 per cent for the 13 pc white dwarfs.
CommentsAccepted for publication in MNRAS. 27 pages, 17 figures
Journal refMon Not R Astron Soc (2026)
