AI 中文总结
研究通过比较宽双星和单颗恒星中白矮星钙污染发生率，分析宽恒星伴星对行星系统的影响，采用校正可探测性累积分数方法，得出单颗恒星和有宽伴星恒星在外行星系统发生率上无显著差异的结论，该方法为比较不同样本提供框架。
AI 中文摘要
白矮星（WD）大气金属污染为残余行星物质的存在提供了有力证据，可作为外行星系统的间接示踪剂。我们通过比较宽双星和明显单颗恒星中氢大气白矮星钙（Ca）污染的发生率，分析宽恒星伴星的存在是否会影响外行星系统的出现。构建了两个样本对，测量Ca丰度或上限并计算校正可探测性后的累积污染分数。结果表明，在当前不确定性范围内，单颗恒星和有宽（约200天文单位）伴星的恒星在外行星系统发生率上无显著差异。校正可探测性累积分数方法为比较不同探测灵敏度样本提供了框架，可扩展到更大光谱数据集。
英文摘要
White dwarf (WD) atmospheric metal pollution provides strong evidence for the presence of remnant planetary material and it can be used as an indirect tracer of outer planetary systems. We analyze whether the presence of a wide stellar companion affects the occurrence of outer planetary systems by comparing the incidence of calcium (Ca) pollution in hydrogen-atmosphere WDs in wide binaries and in apparently single stars. We construct two sample pairs: a large homogeneous SDSS low-resolution spectroscopic set and a smaller high-resolution sample. For each WD, we measure Ca abundances or upper limits and compute detectability-corrected cumulative pollution fractions that account for variations in effective temperature, signal-to-noise ratio, and spectral resolution. In the SDSS-based samples, we find pollution fractions <1%, defined as the fraction of WDs with detected Ca, for both single WDs and WDs in wide binaries. After correcting for detectability, the cumulative abundance distributions of the two populations are statistically consistent. The same conclusion is obtained for the higher-resolution samples, despite their different raw detection fractions. Our results indicate no statistically significant difference in the occurrence rate of remnant outer planetary systems between single stars and stars with wide (~200 au) companions, within the current uncertainties. These uncertainties are significant because the samples contain only a small number of polluted WDs. The corrected detectability cumulative fraction approach used here provides a framework for comparing samples with different detection sensitivities and can be extended to larger spectroscopic datasets. Such samples will be required to determine whether wide stellar companions affect the survival and delivery of planetary material and to search for more subtle trends, for example, as a function of companion separation.
Comments14 pages, 7 figures, accepted in A&A
Journal refA&A, 714, A64 (2026)
DOI：10.1051/0004-6361/202659856
