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The X-ray spectrum of BF Eri contains a puzzling contradiction. BF Eri is the optical counterpart of an Einstein slew survey source 1ES0437-046 comma and was identified as a cataclysmic variable with a massive openPar>1.23 MsunclosePar white dwarf. As such comma we expect a hot comma optically-thin comma thermal plasma with prominent emission lines of He-like and-or H-like iron. No such lines are seen in the Suzaku observation comma showing instead a continuum-dominated spectrum. While this could be due to a low abundance of iron comma the equivalent width of the 6.4 keV line suggests a near-solar abundance. Here we propose an XMM-Newton observation of BF Eri to confirm and refine comma or refute comma these Suzaku results comma with the aim of constructing a model for the X-ray emission from BF Eri with a single abundance of iron.

BF Eri的X射线光谱（X-ray spectrum）存在一处令人困惑的矛盾。BF Eri是爱因斯坦漫游巡天（Einstein slew survey）源1ES0437-046的光学对应体，此前被鉴定为拥有质量大于1.23倍太阳质量的白矮星（white dwarf）的激变变星（cataclysmic variable）。因此，我们预期该天体应存在炽热的光学薄热等离子体，伴随类氦（He-like）和/或类氢（H-like）铁的显著发射线。但朱雀号（Suzaku）的观测并未探测到此类谱线，其光谱反而呈现连续谱主导的特征。尽管这一现象可归因于铁丰度偏低，但6.4千电子伏（keV）谱线的等效宽度显示其铁丰度接近太阳丰度。本文提出将对BF Eri开展XMM-牛顿卫星（XMM-Newton）观测，以验证、细化或推翻朱雀号的观测结果，目标是构建基于单一铁丰度的BF Eri X射线辐射模型。